Current date: 2026-11-10
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Scoring abstracts
Number of records retrieved: 1300
Keyword score statistics
score 12 -- 1 abstracts
score 11 -- 1 abstracts
score 8 -- 1 abstracts
score 6 -- 2 abstracts
score 5 -- 3 abstracts
score 4 -- 2 abstracts
score 3 -- 16 abstracts
score 2 -- 39 abstracts
in total -- 65 abstracts
Articles that appeared on 2026-11-10
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[abstract 1 / 65] Wow! (score: 12)
- Title: SMMAN studies of AGN variability. II. Radio and optical quasi-periodic oscillations and changing variability states in the RELATIVISTIC JET of the BLAZAR PKS 0754+100Authors: Ashutosh Tripathi, Xin Wang, Xi Yan, Paul J. Wiita, Lang Cui,Comments: 15 pages, 7 figures, 1 table. Submitted to ApJSubjects: astro-ph.HECreated: 2026-11-07; Updated: 2026-11-10; Datestamp: 2026-11-10
We report the detection of $\sim$280-day quasi-periodic oscillations (QPOs) in the SMMAN observations of PKS 0754+100 at 4.8 and 23.6 GHz, which may also be present in VLBI observations made at 15 GHz. The onset of a transition of the amplitude of variability in the radio flux density, observed more clearly in the 15 GHz and 23.6 GHz observations, coincides with the detection of a likely QPO of $\sim$1.4 days in optical observations made by the Transiting Exoplanet Survey Satellite. This transition in radio variability also occurs close in time to the disappearance of the secondary knot in the VLBI radio map during the lower variability state. An X-ray flare was observed 100 days before this transition, suggesting that the mechanisms causing these quasi-periodicities are related. After the transition to a higher variability state, both the 15 and 23.6 GHz light curves exhibit indications of QPOs at $\sim$400 days. For the first time, a QPO detected in the radio band from a BL Lac has been seen to appear to shift to a QPO of lower frequency, with that transition occurring near the appearance of a QPO in optical emission at a much shorter period. This multi-waveband behavior could be related to the internal helical structure of the JET, where an instability or kink develops due to MAGNETic RECONNECTion and propagates outward.
[abstract 2 / 65] Wow! (score: 11) - Title: Current Closure and Gamma-Ray Signatures of Spark-Gap and Current-Sheet Activities in Radiative Black Hole MagnetospheresAuthors: Koki Kin, Shota Kisaka, Kenji Toma, John M. Mehlhaff, Benoît Cerutti,Comments: 25 pages, 15 figures, submitted to APSSubjects: astro-ph.HECreated: 2026-11-07; Updated: 2026-11-10; Datestamp: 2026-11-10
We investigate the evolution of an axisymmetric BLACK HOLE MAGNETosphere using general RELATIVISTIC particle-in-cell simulations, focusing on its global current structure, variability, and radiative effects. We include inverse-Compton (IC) scattering of ambient photons and subsequent two-photon pair production, and compare simulations with and without SYNCHROTRON-curvature (SC) radiation reaction. Starting from an axisymmetric vertical MAGNETic field, the system develops a polar spark gap and a variable equatorial current sheet that together sustain the global poloidal current. For the parameters explored in this study, we observe that the spark gap oscillates upon the onset of SC cooling, whereas the current sheet is less sensitive to radiative cooling. Time-dependent electric fields in the return-current layer trigger MAGNETic-field rearrangement followed by MAGNETic RECONNECTion. Cross-correlation analysis finds no significant correlation between the two regions' variability, suggesting dynamical independence. We further perform post-processing ray-tracing calculations to evaluate the radiative efficiencies of the IC and SC processes. High-energy particles dominate the bolometric luminosity, which reaches up to 1 percent of the Blandford-Znajek luminosity for SC emission and 0.1 percent for IC emission. The relative IC luminosity to SC is higher at lower viewing angles because particle momenta are more anisotropic near the pole than near the equator, due to efficient acceleration along the local MAGNETic field lines. Together with energetic estimates, these results suggest that both regions can contribute to high-energy emission in ACTIVE GALACTIC NUCLEi, with spark-gap photons reaching the sub-TeV regime.
[abstract 3 / 65] Wow! (score: 8) - Title: Polarization Signatures of Magnetic Reconnection Bubbles near Black HolesAuthors: Yu-Xiang Huang, En-Wei Liang,Comments:Subjects: astro-ph.HE gr-qcCreated: 2026-11-07; Updated: 2026-11-10; Datestamp: 2026-11-10
Motivated by the observed horizon-scale POLARIZATION variability in multi-epoch Event Horizon Telescope (EHT) data, we develop a time-dependent general RELATIVISTIC polarized ray-tracing framework to study how localized MAGNETic RECONNECTion near a BLACK HOLE imprints itself on SYNCHROTRON POLARIZATION. We model the RECONNECTion phenomenologically as a transient MAGNETic bubble. While keeping the underlying spacetime, emission prescription, and POLARIZATION transport scheme unchanged, the bubble weakens the local ordered field, reorganizes its geometry, induces a conservative local kinematic response, and relaxes through a finite MAGNETic-memory prescription. We explore how the key bubble parameters control the recovery of the MAGNETic-field strength, the spatial spreading of the disturbed region, the persistence of the post-RECONNECTion imprint, and the resulting POLARIZATION signatures. Perturbations dominated by different MAGNETic-field components produce distinct polarized morphologies, EVPA evolution, and Stokes-(Q, U) trajectories: azimuthal perturbations favor outward EVPA shifts, radial perturbations favor inward shifts, and vertical perturbations mainly suppress the polarized intensity. For the illustrative M87^*-like cases, the phase evolution of the β_2 POLARIZATION coefficient further traces how localized MAGNETic reconfiguration contributes to the global EVPA twist of the ring. These results show that horizon-scale POLARIZATION variability can provide a sensitive diagnostic of localized MAGNETic restructuring and that the present framework offers a physically transparent way to interpret time-dependent polarimetric signatures in future EHT observations.
[abstract 4 / 65] Yes (score: 6) - Title: Constraining the white-dwarf mass in the intermediate polar IGR J17014-4306 using X-ray and optical spectroscopyAuthors: D. C. Souza, M. P. Diaz, A. S. Oliveira, G. J. M. Luna, C. V. Rodrigues, M. Reynolds, N. Palivanas, I. J. Lima, J. Mikołajewska, M. Orio,Comments:Subjects: astro-ph.HE astro-ph.SRCreated: 2026-11-04; Updated: 2026-11-10; Datestamp: 2026-11-10
Intermediate polars (IPs), a subclass of MAGNETic cataclysmic variables, often show discrepancies between white-dwarf (WD) mass measurements from X-ray spectral modeling and optical dynamical studies. We investigate the IP IGR J17014-4306. We performed a joint spectral analysis of NUSTAR observations combined with archival XMM-Newton and SWIFT data, modeling the broad-band X-ray spectrum with a multi-temperature cooling-flow model. Additionally, we obtained time-resolved optical spectroscopy with the SOAR telescope to measure the radial velocity of the donor star and constrain the system's orbital parameters. The X-ray spectral analysis reveals a very high post-shock plasma temperature of $kT_{\max}=50_{-8}^{+11}\,\mathrm{keV}$, corresponding to a WD mass of $M_{\mathrm{WD}}=0.94_{-0.07}^{+0.09}\,M_\odot$. We also fitted the NUSTAR spectrum above 10 keV with the ipolar30KK model, obtaining $M_{\mathrm{WD}}=0.88_{-0.12}^{+0.14}\,M_\odot$. Our optical spectroscopy yields a radial-velocity semi-amplitude for the companion star of $K_2=165\pm4\,\mathrm{km\,s^{-1}}$ and an optical mass function of $f(M)=0.249\pm0.018\,M_\odot$. Combined with the eclipse geometry and the WD mass estimate from the X-ray models, these results favor a high mass ratio, $0.76\lesssim q\lesssim0.95$, and a donor-star mass of approximately $0.67\lesssim M_2/M_\odot\lesssim0.89$. In the limiting case of $q=1$, the WD mass has an upper limit of $1.14\,M_\odot$. Together with the X-ray measurements, this indicates a relatively massive WD. The lack of an independent measurement of the WD dynamical mass leaves it unclear whether the dynamical mass is consistent with the X-ray measurements or whether the X-ray mass is underestimated, as has been found for other IPs. Thus, our constraints make IGR J17014-4306 an important system for improving our understanding of IPs.
[abstract 5 / 65] Yes (score: 6) - Title: Quasi-spherical fallback in binary neutron-star mergers: fuel and obstacle for extended emissionAuthors: Zhiwei Chen, Marie Cassing, Paramvir Singh, Luciano Rezzolla,Comments: To be submitted. 13 pages, 7 figuresSubjects: astro-ph.HE gr-qcCreated: 2026-11-06; Updated: 2026-11-10; Datestamp: 2026-11-10
Extended emission (EE) lasting hundreds of seconds has been observed in a fraction of short GAMMA-RAY BURSTs (sGRB) containing both nonthermal and thermal components, and representing a significant puzzle for models involving binary neutron stars (BNSs). Recent GRMHD simulations of BNS mergers found that the late-time fallback is approximately quasi-spherical and motivated an r-process powered thermal model for EE. However, the available radioactive-heating power may be insufficient to sustain the luminosity inferred by such a model. We therefore propose a fallback-fed secondary-JET scenario in which a fraction of the fallback material circularizes on the black-hole equatorial plane and powers the JET, while polar fallback impedes its propagation. Using a semi-analytic toy model, we follow the propagation of the JET-head through the fallback envelope and identify JET-dominated, cocoon-dominated, and choked scenarios. The boundaries of these regimes depend primarily on the circularization fraction $f_{\rm circ}$, on the JET half-opening angle $θ_j$, and on the polar refilling factor $ξ_{\rm pol}$, with the approximate scaling $\widetilde{L}\propto f_{\rm circ}/(ξ_{\rm pol}θ_j^2)$. By post-processing data from BNS-merger simulations we find that the fraction of bound fallback material that avoids prompt capture is $f_{\rm npc}\simeq0.52$, thus providing an upper bound on the circularizable fallback supply. Under suitable prescriptions for nonthermal JET emission and thermal emission from the JET head, the estimated isotropic-equivalent $0.3$--$10$ keV energies reproduce well both the observed EE distribution for the JET-dominated branch and its low-energy end for the cocoon-dominated branch. Overall, these results suggest that fallback-fed secondary JETs represent a dynamically feasible and energetically consistent explanation of the EE in sGRBs.
[abstract 6 / 65] Yes (score: 5) - Title: Dark matter deformations of photon-ring echoes in horizon-scale interferometryAuthors: Mohsen Fathi,Comments: 20 pages, 17 figures, 3 tables. Revised version with improved presentation, updated figures, and referencesSubjects: physics.gen-phCreated: 2026-11-08; Updated: 2026-11-10; Datestamp: 2026-11-10
Photon-ring echoes can probe the delayed light paths near rotating BLACK HOLEs, even when their main ring scales agree. We study an effective rotating geometry with a strong DARK MATTER spike and compare it with a separately ring-matched Kerr control. At $a/M_B=0.8$, $i=70^\circ$, and $M_H/M_B=10$, the remaining angular critical-parameter fingerprint is $1.49\%$. The first two higher image orders have median delays of $13.33M$ and $33.06M$, with spike--Kerr shifts of $1.192M$ and $0.378M$. Finite-order ray transport, slow-light SYNCHROTRON images, and complex very long baseline interferometry (VLBI) visibilities show distinct delay and interference patterns. Direct and higher-order images contribute differently to the complex visibility signal. With the same emitting source, the model difference survives controlled station noise. Independent synthetic-source tests show that the signal depends strongly on source variability: EHT-like held-out closures give an area under the receiver operating characteristic curve (AUC) of $0.658$ (95\% interval $0.497$--$0.807$), while two source-conditioned tests give AUC values close to $0.5$. Published general RELATIVISTIC MAGNETohydrodynamic (GRMHD) light curves of Sgr A* illustrate how electron physics changes variability on the relevant time scales. Together these results connect environmental photon transport to interferometric observables and quantify the importance of source information for future echo studies.
[abstract 7 / 65] Yes (score: 5) - Title: The shape and velocity of BLACK HOLE coronasAuthors: Henric Krawczynski, Kun Hu, Sohee Chun,Comments: 12 pages, 4 figures, submitted to ApJLSubjects: astro-ph.HE gr-qcCreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
The first highly significant detection of the POLARIZATION of the X-rays from the Black Hole X-ray Binary Cygnus X-1 revealed surprisingly strong POLARIZATION parallel to its radio JET. The observation is now commonly interpreted as resulting from the Comptonization of some lower frequency seed photons in a laterally extended corona. The emitting plasma is likely moving along the JET axis with a sizable fraction beta of the speed of light, amplifying the POLARIZATION degree. In this letter we address the question of how laterally extended the corona actually needs to be to account for the observations, and we calculate the required outflow velocities of velocity-stratified coronas as a function of the stationary-frame aspect ratio h=H/2R of cylindrical coronas of height H and radius R. We find that models with h lesser equal 0.8 and beta=0.5-0.9 at the top of the corona can give both the observed photon index of Gamma=1.6 and the observed 4% POLARIZATION parallel to the symmetry axis. We do not find suitable solutions for larger h. Given the constraints on h, we discuss the likely size of the corona, emphasizing that compact coronas close to the BLACK HOLE are preferred as they can tap more efficiently into the gravitational energy and the rotational energy of the BLACK HOLE, and are less exposed to their own emission reprocessed in the optically thick portion of the accretion flow.
[abstract 8 / 65] Yes (score: 5) - Title: The Edge of the Warm Corona in Active Galactic NucleiAuthors: Parikshit Partha Biswas, Agata Różańska, Debora Lančová, Dominik Gronkiewicz, Rafał Wojaczyński, Andrzej Zdziarski, Stefano Bianchi,Comments: 14 pages, 12 figures, submitted to ApJSubjects: astro-ph.HE astro-ph.GACreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
A model of warm, dissipative corona on top of an accretion disk is investigated, to explain the soft X-ray excess (SXE) emission observed in ACTIVE GALACTIC NUCLEi (AGN). The final ray-traced spectrum, computed through photoionization code with Comptonization, accounts for both: emitted and reflected components. As a result, the strength of the SXE depends on the radial extend of the warm corona, i.e., its outer edge. We show that the radial transition from warm corona to disk atmosphere is governed by line cooling. By moving away from a central BLACK HOLE Compton cooling is gradually replaced by line cooling, and the temperature drops sharply in vertical direction at a narrow iron ionization front, where iron ions Fe \textsc{xxv}--Fe \textsc{xxvi} recombine to Fe \textsc{xvii}. Notably, this transition takes place at a particular value of internal heating $\approx 1.6 \times 10^{-23}$ erg cm$^{3}$ s$^{-1}$, regardless of the Eddington ratio. We show, that at the given metal abundance, the SXE emitting area is larger for a higher accretion rate, in agreement with recent findings in changing look AGN. The overall emission spectrum from a warm corona is featureless, and the only iron K$_α$ line comes from a reflection. The line is stronger and more gravitationally distorted for a lower accretion rate, which is a direct result of the size of the warm corona. Furthermore, by increasing the iron abundance, the iron ionization front moves closer towards BLACK HOLE, and a stronger iron line complex is emitted locally.
[abstract 9 / 65] Yes (score: 4) - Title: Energy Extraction via Magnetic Reconnection from a Rotating Dyonic Black Hole in $N = 2, \ U(1)^2$ Gauged SupergravityAuthors: Raid M Suleiman, Shanshan Rodriguez, Dominic O. Chang, Leo Rodriguez,Comments: 25 pages, 14 figuresSubjects: gr-qc astro-ph.HE hep-thCreated: 2026-11-07; Updated: 2026-11-10; Datestamp: 2026-11-10
We study energy extraction via MAGNETic RECONNECTion from a rotating dyonic BLACK HOLE in four-dimensional $N=2$, $U(1)^2$ gauged supergravity. Using the Comisso-Asenjo mechanism in the ZAMO frame, we derive the asymptotic hydrodynamic energy per unit enthalpy $ε^{\infty}_\pm$ and determine when RECONNECTion outflows attained negative energy at infinity. By varying the spin $a$, electric and MAGNETic charges, NUT parameter $N_g$, and gauge coupling $g$, we compute the cutoff MAGNETization $σ_0^{\rm cutoff}$ and map the region of parameter space that admits $ε^{\infty}_-<0$. We find that $σ_0^{\rm cutoff}$ and the very existence of Comisso-Asenjo extraction are tightly controlled by $g$ and the dyonic charges: increasing $g$ or pushing the charges toward extremality raises $σ_0^{\rm cutoff}$ and shrinks the CA-active part of the ergoregion. Unlike Kerr, the spin enters through the normalization factor $Ξ$, and the quartic horizon function $Δ_g$, so geometric effects from the AdS/NUT deformation dominate the usual frame-dragging enhancement. As a result, the extracted power and efficiency are non-monotonic in $a$ and peak at intermediate spin ($a\sim0.8$); near-extremal rotation is not required for high efficiency, provided $g$ is small and $Q$ is moderate. Efficient extraction further demands extreme MAGNETization and nearly radial outflows, confining the active RECONNECTion layer to a thin shell, just outside the horizon.
[abstract 10 / 65] Yes (score: 4) - Title: The Role of Small-Scale Flux Emergence in Pre-eruptive Magnetic DestabilizationAuthors: Satoshi Inoue, Huu Minh Triet Nguyen,Comments: Accepted for publication in ApJSubjects: astro-ph.SRCreated: 2026-11-08; Updated: 2026-11-10; Datestamp: 2026-11-10
Recent high-resolution observations have reported the emergence of small-scale MAGNETic flux shortly before the onset of solar flares; however, their role in solar eruption processes remains unclear. In this study, we perform three-dimensional MAGNETohydrodynamic (MHD) simulations to examine the effect of small-scale emerging flux on the eruption process. We construct a bipolar active region by extrapolating a potential MAGNETic field from a pair of sunspots and drive the system with sustained rotational motions to build up strong shear along the polarity inversion line. A small-scale emerging flux, amounting to approximately 0.6%-3.0% of the total MAGNETic flux and having a polarity opposite to that of the main sunspot, is then introduced at the center of the bipole. As a result, although no significant differences are found in the pre-existing MAGNETic field during the early phase with or without the emerging flux, the current sheet formed in the sheared field lines collapses more rapidly, and the RECONNECTion-driven eruption is initiated earlier in the case with small-scale emerging flux. This result suggests that small-scale emerging flux accelerates the destabilization of the pre-eruptive MAGNETic configuration through enhanced current-sheet thinning and MAGNETic RECONNECTion, leading to an earlier eruption onset. Furthermore, we find that the involvement of highly twisted field lines during the pre-eruption phase plays a crucial role in determining the eruption onset time.
[abstract 11 / 65] (score: 3) - Title: CANTON-$μ$ Proposal: A Next-Generation Muon $g-2$ Measurement at Sub-0.1 ppm PrecisionAuthors: Ce Zhang, Yu Xu, On Kim, Bingzhi Li, Zejia Lu, Saskia Charity, Guodong Shen, Liangwen Chen, Fedor Ignatov, Liang Li, Qiang Li, Xueheng Zhang, Zhiyu Sun,Comments: Published in Eur. Phys. J. C. DOI: 10.1140/epjc/s10052-026-16588-xSubjects: hep-ex hep-phCreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
We propose a next-generation precision measurement of the muon anomalous MAGNETic moment (muon g-2) at the High Intensity Heavy-Ion Accelerator Facility (HIAF) in Huizhou, China. We refer to this proposed experimental programme as CANTON-$μ$ (Coherent Anomalous magNetic momenT ObservatioN with muon). HIAF's intense, pulsed GeV-scale muon beams, particularly for negative muons, provide a promising basis for this programme. Building on two previously proposed storage-ring concepts, this work develops HIAF-specific experimental schemes that relax the conventional magic-momentum constraint and allow greater flexibility in the choice of beam momentum. We assess the expected muon intensity at HIAF and the corresponding statistical sensitivity. For each scheme, we identify its distinctive systematic effects, examine feasible control strategies, and propose quantitative systematic-uncertainty targets. Together, the statistical projections and systematic-uncertainty targets indicate prospective total precisions of 0.1 ppm in Phase-I, comparable to the current FERMIlab precision, with the potential to reach the 0.05 ppm level in Phase-II following the planned HIAF upgrade. At the ultimate projected precision, the measurement would provide a stringent test of the Standard Model and probe new physics at multi-TeV scales. A focus on negative-muon measurements would enable direct comparison with existing high-precision positive-muon results and strengthen tests of CPT symmetry in the muon sector within the Standard-Model Extension, with a projected sensitivity at the $10^{-24}$ GeV level, an order of magnitude beyond current limits.
[abstract 12 / 65] (score: 3) - Title: Magnetic properties of the Abell 3391-3395 system revealed using wide-field MeerKAT polarimetryAuthors: V. Gustafsson, M. Brüggen, C. Tasse, S. P. O'Sullivan,Comments:Subjects: astro-ph.GA astro-ph.COCreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
Magnetic fields in cluster outskirts and the intercluster medium are poorly constrained because diffuse SYNCHROTRON emission is hard to detect at low surface brightness. Faraday rotation measures (RMs) of polarized background sources can probe foreground large-scale structure. The nearby interacting Abell 3391-3395 system hosts a well-established X-ray bridge, making it an excellent target for studying MAGNETization in the intercluster environment. We characterize the MAGNETized environment of Abell 3391/95 and its surroundings by constructing a dense RM grid from wide-field polarimetry. We observed Abell 3391/95 with MeerKAT in full POLARIZATION using a three-pointing mosaic. The data were calibrated with direction-independent and direction-dependent techniques and imaged using visibility-plane mosaicing for a large field of view at high sensitivity. Using Faraday synthesis, we formed Faraday cubes and measured RMs for polarized background sources. We defined on- and off-target regions using contours from a wavelet-filtered eROSITA image. We identified 434 polarized sources within the field, with a polarized source density ranging from about 30 sources per square degree in the outer regions to about 110 sources per square degree in the central field, and a field-averaged density of 73 sources per square degree. The clusters show a statistically significant enhancement of RM scatter relative to the off-target region. In contrast, the bridge shows comparatively low RM scatter, while an RM structure-function analysis on matched angular scales yields a tentative indication of larger RM differences in the bridge than off-target. Combined with low per-source dePOLARIZATION, this suggests a bridge MAGNETic field relatively ordered on ~10 kpc scales, but less ordered on larger scales. The non-detection of diffuse SYNCHROTRON emission in the bridge yields improved upper limits on the emissivity.
[abstract 13 / 65] (score: 3) - Title: Second stability region for gyrokinetics and the L-H transitionAuthors: R. J. J. Mackenbach, A. Zocco, P. Helander,Comments:Subjects: physics.plasm-phCreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
Using a simple circular tokamak geometry, we show the well-known `second stability region' of MHD-ballooning modes exists for linear gyrokinetics too---whether electrostatic or electroMAGNETic---and we suggest that the plasma enters this region in H-mode as a consequence of the bootstrap current and Shafranov shift altering the MAGNETic field, which may occur if the normalised pressure gradient is $α_{\rm MHD} \simgt 1$ and collisionality is low. By performing simulations in more realistic MAGNETic geometries, we demonstrate a large reduction in collisionless, electrostatic turbulent transport when going from density and temperature profiles typical of L- and H-mode, respectively. This reduction is shown to be a consequence of both the bootstrap current lowering the global MAGNETic shear, and the pressure gradient altering the local MAGNETic shear, pushing the plasma towards the second-stability region. A path connecting the L- and H-mode equilibria is constructed, along which the energy and particle fluxes exhibit non-monotonic behaviour as a function of the pressure gradient.
[abstract 14 / 65] (score: 3) - Title: Loss-Cone-Limited Dark Matter Capture by Early Black Hole SeedsAuthors: Brian Zhang, Grant J. Mathews,Comments:Subjects: astro-ph.CO astro-ph.GA gr-qcCreated: 2026-11-07; Updated: 2026-11-10; Datestamp: 2026-11-10
The rapid appearance of supermassive BLACK HOLEs at high redshift motivates a reassessment of non-baryonic growth channels. We develop a new loss-cone framework for collisionless dark-matter (DM) capture by early black-hole seeds, with particular attention to phase-space depletion and refilling. The calculation combines Eddington-inverted NFW-like halos, a RELATIVISTIC direct-capture boundary, and an orbit-averaged Fokker-Planck treatment of angular-momentum transport. Primordial BLACK HOLEs (PBHs) are treated as massive perturbers whose refilling strength depends on both their abundance and individual mass. Collisionless refilling by triaxial or chaotic centrophilic orbits is included as a phenomenological upper-envelope channel. We show that ordinary stellar relaxation gives negligible DM-driven growth for the fiducial high-redshift seeds. PBH-driven granularity can yield order-of-magnitude growth in sufficiently compact halos, while triaxial or full-loss-cone supply can produce a rapid early burst. In the self-consistent calculations, however, the evolution generally becomes supply-limited. Once the accessible low-angular-momentum phase-space reservoir is depleted, the capture rate collapses and the black-hole mass saturates. Fixed-background NFW calculations therefore overestimate sustained growth, especially in the full-loss-cone limit. A TNG50-calibrated NFW benchmark gives negligible growth even under optimistic refilling assumptions. Collisionless DM capture is therefore unlikely to solve early SMBH growth in generic NFW-like halos, but it can provide a radiatively dark upper envelope in rare compact environments with efficient angular-momentum refilling.
[abstract 15 / 65] (score: 3) - Title: Search for active-sterile neutrino transitions using Pierre Auger Observatory dataAuthors: The Pierre Auger Collaboration, A. Abdul Halim, P. Abreu, M. Aglietta, M. Ahmed, I. Allekotte, K. Almeida Cheminant, R. Aloisio, J. Alvarez-Muñiz, A. Ambrosone, J. Ammerman Yebra, L. Anchordoqui, B. Andrada, L. Andrade Dourado, L. Apollonio, C. Aramo, J. C. Arteaga Velázquez, P. Assis, G. Avila, E. Avocone, A. Bakalova, Y. Balibrea, A. Baluta, F. Barbato, A. Bartz Mocellin, O. Batalla Cruz, J. P. Behler, C. Berat, M. E. Bertaina, M. Bianciotto, P. L. Biermann, V. Binet, K. Bismark, T. Bister, J. Biteau, J. Blazek, J. Blümer, M. Boháčová, D. Boncioli, C. Bonifazi, N. Borodai, J. Brack, P. G. Brichetto Orquera, S. Buitink, A. Bwembya, T. R. Caba Pineda, K. S. Caballero-Mora, S. Cabana-Freire, L. Caccianiga, J. Caraça-Valente, R. Caruso, A. Castellina, F. Catalani, G. Cataldi, L. Cazon, M. Cerda, B. Čermáková, A. Cermenati, K. Cerny, J. A. Chinellato, J. Chudoba, L. Chytka, R. W. Clay, A. C. Cobos Cerutti, R. Colalillo, R. Conceição, A. Condorelli, G. Consolati, M. Conte, F. Convenga, D. Correia dos Santos, P. J. Costa, C. E. Covault, M. Cristinziani, C. S. Cruz Sanchez, S. Dasso, K. Daumiller, B. R. Dawson, R. M. de Almeida, E. -T. de Boone, B. de Errico, J. de Jesús, S. J. de Jong, J. R. T. de Mello Neto, I. De Mitri, D. de Oliveira Franco, F. de Palma, V. de Souza, E. De Vito, A. Del Popolo, O. Deligny, N. Denner, K. Denner Syrokvas, L. Deval, A. di Matteo, C. Dobrigkeit, J. C. D'Olivo, L. M. Domingues Mendes, T. Dominguez, Y. Dominguez Ballesteros, Q. Dorosti, R. C. dos Anjos, J. Ebr, F. Ellwanger, R. Engel, M. Erdmann, A. Etchegoyen, C. Evoli, H. Falcke, G. Farrar, A. C. Fauth, T. Fehler, F. Feldbusch, A. Fernandes, M. Fernández Alonso, B. Fick, J. M. Figueira, P. Filip, A. Filipčič, B. Flaggs, A. Franco, M. Freitas, T. Fujii, A. Fuster, C. Galea, B. García, C. Gaudu, P. L. Ghia, U. Giaccari, M. Giammarco, C. Glaser, F. Gobbi, F. Gollan, G. Golup, P. F. Gómez Vitale, J. P. Gongora, N. González, D. Góra, A. Gorgi, M. Gottowik, F. Guarino, G. P. Guedes, Y. C. Guerra, L. Gülzow, S. Hahn, P. Hamal, M. R. Hampel, P. Hansen, V. M. Harvey, A. Haungs, M. Havelka, T. Hebbeker, C. Hojvat, J. R. Hörandel, P. Horvath, M. Hrabovský, T. Huege, A. Insolia, P. G. Isar, M. Ismaiel, P. Janecek, V. Jilek, K. -H. Kampert, B. Keilhauer, V. V. Kizakke Covilakam, H. O. Klages, M. Kleifges, A. Klingel, J. Köhler, F. Krieger, M. Kubatova, N. Kunka, B. L. Lago, N. Langner, N. Leal, M. A. Leigui de Oliveira, Y. Lema-Capeans, A. Letessier-Selvon, I. Lhenry-Yvon, L. Lopes, M. Mallamaci, S. Mancuso, D. Mandat, P. Mantsch, A. G. Mariazzi, C. Marinelli, I. C. Mariş, G. Marsella, D. Martello, S. Martinelli, O. Martínez Bravo, A. Martínez-Mendez, M. A. Martins, H. -J. Mathes, J. Matthews, G. Matthiae, E. Mayotte, S. Mayotte, P. O. Mazur, G. Medina-Tanco, D. Melo, A. Menshikov, C. Merx, S. Michal, M. I. Micheletti, L. Miramonti, M. Mogarkar, S. Mollerach, F. Montanet, L. Morejon, K. Mulrey, R. Mussa, W. M. Namasaka, S. Negi, L. Nellen, K. Nguyen, G. Nicora, M. Niechciol, D. Nitz, D. Nosek, A. Novikov, V. Novotny, L. Nožka, A. Nucita, L. A. Núñez, S. E. Nuza, J. Ochoa, M. Olegario, C. Oliveira, L. Östman, M. Palatka, J. Pallotta, G. Parente, T. Paulsen, M. Pech, J. Pękala, R. Pelayo, C. Pérez Bertolli, L. Perrone, S. Petrera, T. Pierog, M. Pimenta, M. Platino, P. Privitera, C. Priyadarshi, M. Prouza, K. Pytel, S. Querchfeld, J. Rautenberg, D. Ravignani, J. V. Reginatto Akim, M. Z. Rennó, A. Reuzki, J. Ridky, F. Riehn, M. Risse, V. Rizi, B. Rocha Moldes, E. Rodriguez, G. Rodriguez Fernandez, J. Rodriguez Rojo, S. Rossoni, M. Roth, E. Roulet, A. C. Rovero, A. Saftoiu, M. Saharan, F. Salamida, H. Salazar, G. Salina, P. Sampathkumar, N. San Martin, J. D. Sanabria Gomez, F. Sánchez, F. M. Sánchez Rodriguez, E. Santos, F. Sarazin, R. Sarmento, R. Sato, P. Savina, V. Scherini, H. Schieler, M. Schimp, D. Schmidt, O. Scholten, H. Schoorlemmer, P. Schovánek, F. G. Schröder, J. Schulte, T. Schulz, S. J. Sciutto, M. Scornavacche, A. Sedoski, S. Sehgal, S. U. Shivashankara, G. Sigl, K. Simkova, F. Simon, R. Šmída, S. Soares Sippert, P. Sommers, S. Stanič, J. Stasielak, P. Stassi, S. Strähnz, M. Straub, T. Suomijärvi, A. D. Supanitsky, Z. Svozilikova, Z. Szadkowski, F. Tairli, A. Tapia, C. Taricco, C. Timmermans, O. Tkachenko, P. Tobiska, C. J. Todero Peixoto, B. Tomé, A. Travaini, P. Travnicek, C. Trimarelli, M. Tueros, M. Unger, R. Uzeiroska-Geyik, L. Vaclavek, M. Vacula, I. Vaiman, J. F. Valdés Galicia, L. Valore, P. van Dillen, E. Varela, V. Vašíčková, A. Vásquez-Ramírez, D. Veberič, I. D. Vergara Quispe, S. Verpoest, V. Verzi, J. Vicha, S. Vorobiov, J. B. Vuta, A. A. Watson, A. Weindl, M. Weitz, L. Wiencke, H. Wilczyński, B. Wundheiler, B. Yue, A. Yushkov, E. Zas, D. Zavrtanik, M. Zavrtanik,Comments: 12 pages, 4 figuresSubjects: hep-ph astro-ph.HE hep-exCreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
We investigate the sensitivity of the Pierre Auger Observatory to physics beyond the Standard Model arising from MAGNETic-moment-induced transitions between active and heavy sterile neutrinos. Such dipole portal interactions can enhance neutrino-nucleon cross sections above a kinematic threshold set by the sterile neutrino mass, leading to observable modifications of neutrino detection rates at ultrahigh energies (UHE). We estimate the impact of these interactions on both down-going and Earth-skimming neutrino detection channels, the contrasting responses of which enable discrimination between an enhanced neutrino flux and a modified interaction cross section. Using the non-observation of UHE neutrino candidates, we derive neutrino-flux-dependent constraints with 90% confidence-level on the transition MAGNETic moment for sterile neutrino masses in the range 1 TeV-100 TeV. Under the assumed flux scenarios, the resulting flavor-independent limits extend existing bounds into previously unexplored parameter space.
[abstract 16 / 65] (score: 3) - Title: Evidence for the Moon and Sun shadows with COSMIC RAYs at an average energy of $\text{7}{\times}\text{10}^\text{17}\,$eVAuthors: The Pierre Auger Collaboration, A. Abdul Halim, P. Abreu, M. Aglietta, M. Ahmed, I. Allekotte, K. Almeida Cheminant, R. Aloisio, J. Alvarez-Muñiz, A. Ambrosone, J. Ammerman Yebra, L. Anchordoqui, B. Andrada, L. Andrade Dourado, L. Apollonio, C. Aramo, J. C. Arteaga Velázquez, P. Assis, G. Avila, E. Avocone, A. Bakalova, Y. Balibrea, A. Baluta, F. Barbato, A. Bartz Mocellin, O. Batalla Cruz, J. P. Behler, C. Berat, M. E. Bertaina, M. Bianciotto, P. L. Biermann, V. Binet, K. Bismark, T. Bister, J. Biteau, J. Blazek, J. Blümer, M. Boháčová, D. Boncioli, C. Bonifazi, N. Borodai, J. Brack, P. G. Brichetto Orquera, S. Buitink, A. Bwembya, T. R. Caba Pineda, K. S. Caballero-Mora, S. Cabana-Freire, L. Caccianiga, J. Caraça-Valente, R. Caruso, A. Castellina, F. Catalani, G. Cataldi, L. Cazon, M. Cerda, B. Čermáková, A. Cermenati, K. Cerny, J. A. Chinellato, J. Chudoba, L. Chytka, R. W. Clay, A. C. Cobos Cerutti, R. Colalillo, R. Conceição, G. Consolati, M. Conte, F. Convenga, D. Correia dos Santos, P. J. Costa, C. E. Covault, M. Cristinziani, C. S. Cruz Sanchez, S. Dasso, K. Daumiller, B. R. Dawson, R. M. de Almeida, E. -T. de Boone, B. de Errico, J. de Jesús, S. J. de Jong, J. R. T. de Mello Neto, I. De Mitri, D. de Oliveira Franco, F. de Palma, V. de Souza, E. De Vito, A. Del Popolo, O. Deligny, N. Denner, K. Denner Syrokvas, L. Deval, A. di Matteo, C. Dobrigkeit, J. C. D'Olivo, L. M. Domingues Mendes, T. Dominguez, Y. Dominguez Ballesteros, Q. Dorosti, R. C. dos Anjos, J. Ebr, F. Ellwanger, R. Engel, M. Erdmann, A. Etchegoyen, C. Evoli, H. Falcke, G. Farrar, A. C. Fauth, T. Fehler, F. Feldbusch, A. Fernandes, M. Fernández Alonso, B. Fick, J. M. Figueira, P. Filip, A. Filipčič, B. Flaggs, A. Franco, M. Freitas, T. Fujii, A. Fuster, C. Galea, B. García, C. Gaudu, P. L. Ghia, U. Giaccari, M. Giammarco, C. Glaser, F. Gobbi, F. Gollan, G. Golup, P. F. Gómez Vitale, J. P. Gongora, N. González, D. Góra, A. Gorgi, M. Gottowik, F. Guarino, G. P. Guedes, Y. C. Guerra, L. Gülzow, S. Hahn, P. Hamal, M. R. Hampel, P. Hansen, A. Haungs, M. Havelka, T. Hebbeker, C. Hojvat, J. R. Hörandel, M. Horvat, P. Horvath, M. Hrabovský, T. Huege, A. Insolia, P. G. Isar, M. Ismaiel, P. Janecek, V. Jilek, K. -H. Kampert, B. Keilhauer, V. V. Kizakke Covilakam, H. O. Klages, M. Kleifges, A. Klingel, J. Köhler, F. Krieger, M. Kubatova, N. Kunka, B. L. Lago, N. Langner, N. Leal, M. A. Leigui de Oliveira, Y. Lema-Capeans, A. Letessier-Selvon, I. Lhenry-Yvon, L. Lopes, M. Mallamaci, S. Mancuso, D. Mandat, P. Mantsch, A. G. Mariazzi, C. Marinelli, I. C. Mariş, G. Marsella, D. Martello, S. Martinelli, O. Martínez Bravo, A. Martínez-Mendez, M. A. Martins, H. -J. Mathes, J. Matthews, G. Matthiae, E. Mayotte, S. Mayotte, P. O. Mazur, G. Medina-Tanco, D. Melo, A. Menshikov, C. Merx, S. Michal, M. I. Micheletti, L. Miramonti, M. Mogarkar, S. Mollerach, F. Montanet, L. Morejon, K. Mulrey, R. Mussa, W. M. Namasaka, S. Negi, L. Nellen, K. Nguyen, G. Nicora, M. Niechciol, D. Nitz, D. Nosek, A. Novikov, V. Novotny, L. Nožka, A. Nucita, L. A. Núñez, S. E. Nuza, J. Ochoa, M. Olegario, C. Oliveira, L. Östman, M. Palatka, J. Pallotta, G. Parente, T. Paulsen, M. Pech, J. Pękala, R. Pelayo, C. Pérez Bertolli, L. Perrone, S. Petrera, T. Pierog, M. Pimenta, M. Platino, P. Privitera, C. Priyadarshi, M. Prouza, K. Pytel, S. Querchfeld, J. Rautenberg, D. Ravignani, J. V. Reginatto Akim, M. Z. Rennó, A. Reuzki, J. Ridky, F. Riehn, M. Risse, V. Rizi, B. Rocha Moldes, E. Rodriguez, G. Rodriguez Fernandez, J. Rodriguez Rojo, S. Rossoni, M. Roth, E. Roulet, A. C. Rovero, A. Saftoiu, M. Saharan, F. Salamida, H. Salazar, G. Salina, P. Sampathkumar, N. San Martin, J. D. Sanabria Gomez, F. Sánchez, F. M. Sánchez Rodriguez, E. Santos, F. Sarazin, R. Sarmento, R. Sato, P. Savina, V. Scherini, H. Schieler, M. Schimp, D. Schmidt, O. Scholten, H. Schoorlemmer, P. Schovánek, F. G. Schröder, J. Schulte, T. Schulz, S. J. Sciutto, M. Scornavacche, A. Sedoski, S. Sehgal, S. U. Shivashankara, G. Sigl, K. Simkova, F. Simon, R. Šmída, S. Soares Sippert, P. Sommers, S. Stanič, J. Stasielak, P. Stassi, S. Strähnz, M. Straub, T. Suomijärvi, A. D. Supanitsky, Z. Svozilikova, Z. Szadkowski, F. Tairli, A. Tapia, C. Taricco, C. Timmermans, O. Tkachenko, P. Tobiska, C. J. Todero Peixoto, B. Tomé, A. Travaini, P. Travnicek, C. Trimarelli, M. Tueros, M. Unger, R. Uzeiroska-Geyik, L. Vaclavek, M. Vacula, I. Vaiman, J. F. Valdés Galicia, L. Valore, P. van Dillen, E. Varela, V. Vašíčková, A. Vásquez-Ramírez, D. Veberič, I. D. Vergara Quispe, S. Verpoest, V. Verzi, J. Vicha, S. Vorobiov, J. B. Vuta, A. A. Watson, A. Weindl, M. Weitz, L. Wiencke, H. Wilczyński, B. Wundheiler, B. Yue, A. Yushkov, E. Zas, D. Zavrtanik, M. Zavrtanik,Comments: acceptedSubjects: astro-ph.HECreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
Interactions of COSMIC RAYs with the Moon and the Sun produce deficits in their arrival-direction distributions relative to an isotropic flux. Such shadows have been observed previously at energies between $10^{12}\,$eV and $10^{16}\,$eV. We report the first evidence for the Moon and Sun shadows at cosmic-ray energies larger than about $10^{16}\,$eV (average energy of $7\times10^{17}\,$eV), using data collected by the Pierre Auger Observatory. We employ data from three detector arrays covering $3000\,\text{km}^2$, $27\,\text{km}^2$, and $2\,\text{km}^2$, with spacings of $1500\,\text{m}$, $750\,\text{m}$, and $433\,\text{m}$, respectively. The data amount to over 10.6 million events. The Moon and Sun shadows are detected with a combined significance of approximately $3σ$. These observations confirm the pointing accuracy of the Surface Detector of the Pierre Auger Observatory using celestial bodies. From the combined Sun and Moon shadows, we infer an overall angular resolution of $(0.59^{+0.15}_{-0.11})^\circ$.
[abstract 17 / 65] (score: 3) - Title: Black Hole Seeds and Little Red Dots: Connecting Formation and Growth with a JWST Multi-Cycle Treasury ProgramAuthors: Fabio Pacucci, Raffaella Schneider, Harley Katz, Brant E. Robertson, Rachel S. Somerville, Abdurro'uf, K. Aditya, Jose M. Afonso, Junya Arita, Guillermo Barro, Arghyadeep Basu, Ryan Begley, Sownak Bose, Marusa Bradac, Greg L. Bryan, Christopher Cain, Riccardo Caleno, Alex J. Cameron, Stefano Carniani, Hyunseop Choi, Nicholas Choustikov, Emma Curtis-Lake, Alessia D'Angelo, Romeel Dave, Rebecca L. Davies, Kelcey Davis, Callum T. Donnan, Qiao Duan, Yohan Dubois, Andreas L. Faisst, Marion Farcy, Steven L. Finkelstein, Steven Gillman, Simon C. O. Glover, Luca Graziani, Ansh R. Gupta, Thales A. Gutcke, Martin G. Haehnelt, Nimish P. Hathi, Evanthia Hatziminaoglou, Kasper E. Heintz, Michaela Hirschmann, Luis C. Ho, Lucy R. Ivey, Kartheik Iyer, Junehyoung Jeon, Brenda L. Jones, Ignas Juodzbalis, Anton M. Koekemoer, Christian Kragh Jespersen, Danial Langeroodi, Andrea Lapi, Muhammad A. Latif, Yuankang Liu, Christopher C. Lovell, Filippo Mannucci, Kentaro Nagamine, Priyamvada Natarajan, Zhiwei Pan, Robert Pascalau, Pablo G. Pérez-González, Elia Pizzati, Eniko Regos, Pierluigi Rinaldi, Daniel Roberts, William Roper, Dominik R. G. Schleicher, Francesco Shankar, Xuejian Shen, Thomas M. Stanton, Guochao Sun, Yang Sun, Alessandro Trinca, Jonathan R. Trump, Jack C. Turner, Hannah Übler, Rosa Valiante, Floor van Donkelaar, Giacomo Venturi, Aswin P. Vijayan, Fabio Vito, Tao Wang, Stephen Wilkins, John H. Wise, Joris Witstok, Zihao Wu, L. Y. Aaron Yung, Tommaso Zana, Huanian Zhang, Saiyang Zhang, Ming-Yang Zhuang,Comments: Theory white paper on black hole seeds and Little Red Dots, submitted to the STScI call for JWST Multi-Cycle Treasury concept white papers as part of the Genesis Initiative (www.jwst-genesis.com). 5 pages (plus affiliations and references)Subjects: astro-ph.GA astro-ph.CO astro-ph.HECreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
JWST has revealed an abundant population of faint ACTIVE GALACTIC NUCLEi and a new class of compact, high-redshift sources known as Little Red Dots (LRDs), whose physical nature remains debated, with accreting massive BLACK HOLEs among the leading explanations. The emerging demographics of early BLACK HOLEs, with their high inferred number densities and, in some systems, the apparent excess of BLACK HOLE mass relative to stellar mass, challenge simple scenarios of BLACK HOLE seeding and growth. Despite these observational breakthroughs, the origin of early massive BLACK HOLEs remains uncertain, because "BLACK HOLEs have no memory": current samples cannot separate the imprint of seeding from subsequent growth. This white paper identifies the multi-cycle JWST observations needed to revolutionize our understanding of early BLACK HOLE growth by: (i) distinguishing seeding pathways, (ii) constraining early BLACK HOLE growth mechanisms, (iii) resolving the physical nature of broad-line emitters and LRDs, and (iv) testing BLACK HOLE-galaxy co-evolution. These tasks require uniformly selected samples extending to low BLACK HOLE and host-galaxy masses, allowing self-consistent measurements of BLACK HOLE mass functions, Eddington-ratio distributions, and host properties. Grating spectroscopy, deep MIRI imaging, and variability analysis through repeated observations of the same fields would provide complementary tests of BLACK HOLE formation and growth, their connection to host-galaxy evolution, and the nature of newly discovered populations of LRDs. In this white paper, we argue that these joint tests require a coordinated JWST Multi-Cycle Treasury program; such a program could provide the depth, uniformity, and time baseline needed to place substantially stronger, complementary constraints on early BLACK HOLE formation, growth, and their connection to galaxy evolution.
[abstract 18 / 65] (score: 3) - Title: Time-Delay Recovery in AGN Reverberation Mapping via Mutual InformationAuthors: R. A. A. Souza, E. Hatziminaoglou, D. O. Fontinele, L. B. T. Santos, M. V. D. Souza, T. Stosic,Comments: Accepted for publication in MNRAS. 16 pages, 8 figures, 4 tablesSubjects: astro-ph.GACreated: 2026-11-07; Updated: 2026-11-10; Datestamp: 2026-11-10
Active galactic nuclei exhibit complex, nonlinear multiwavelength variability that standard cross-correlation techniques, sensitive only to linear covariance, may fail to capture fully. We apply time-lagged Mutual Information (MI) lag estimation, via the Kraskov-Stoegbauer-Grassberger $k$-nearest-neighbour estimator ($k = 5$) with a 150-iteration Random Subset Selection bootstrap, to the light curves of four Seyfert galaxies (Mrk 509, NGC 5548, NGC 4151, and NGC 4593) monitored across eight energy bands by SWIFT. In the UV/optical regime the MI estimator successfully reproduces the inter-band disc reprocessing lags established by the interpolated cross-correlation function, with performance degrading toward the optical where low variability amplitude produces poorly defined MI peaks. In the X-ray bands, where the physical X-ray/UV coupling is known to be weak, the estimator fails to recover consistent lags across the sample, with the notable exception of NGC 4593. Contextualising these outcomes within the multifractal characterisation of our previous work, we discuss how MI performance relates to the multifractal spectral width $Δα$ of each band, and we propose $Δα$ as a candidate diagnostic for anticipating where MI-based reverberation mapping is likely to succeed or fail in multiband datasets of ACTIVE GALACTIC NUCLEi.
[abstract 19 / 65] (score: 3) - Title: Probing the origin of the LHAASO Peanut with a hidden central acceleratorAuthors: Agnibha De Sarkar,Comments: 13 pages, 2 figures, 2 tables; accepted for publication in Astronomy & Astrophysics (A&A)Subjects: astro-ph.HECreated: 2026-11-07; Updated: 2026-11-10; Datestamp: 2026-11-10
A highly asymmetric, giant Peanut-shaped structure has been detected by the Large High Altitude Air Shower Observatory (LHAASO) in ultra-high-energy gamma rays at high Galactic latitude, $b\approx-17.5^{\circ}$, suggesting anisotropic particle transport around a Galactic accelerator. We investigate whether its spectrum and morphology can arise from a hidden central accelerator embedded in a projected anisotropic halo. The baseline model accounts for the diffuse strip and central excess, while a phenomenological prescription for a localized MAGNETic field reorientation toward the line of sight (LOS), together with a particle-conserved remapping of the electrons downstream of the far excess into an emitting column of prescribed transverse extent, enhances the emission at the far excess position. We explore various source ages, along with different combinations of ambient MAGNETic field strength and parallel diffusion coefficient, while accounting for radiative cooling when estimating the viewing geometry. The exploration reveals that relatively rapid parallel transport enhances the far component while preserving a dominant diffuse strip. Representative configurations remain compatible with the observed spectral energy distribution, although the fitted far component remains comparatively weaker than the central component above 100 TeV, even in cases where their component fluxes are comparable at 25-100 TeV. These results illustrate the plausibility of a hidden central accelerator as the origin of the LHAASO Peanut, while identifying the remaining difficulty in reproducing the relative brightness of its compact components within the adopted phenomenological framework.
[abstract 20 / 65] (score: 3) - Title: Pushing the accuracy of the quasi-circular baseline for the SEOBNR family of modelsAuthors: Cheng Foo, Alessandra Buonanno, Héctor Estellés, Lorenzo Pompili,Comments: 39 pages, 16 figures and 2 tablesSubjects: gr-qc astro-ph.HECreated: 2026-11-08; Updated: 2026-11-10; Datestamp: 2026-11-10
Gravitational-wave observations have opened a new era of astronomy, with accurate modeling of binary BLACK HOLE signals becoming increasingly important for source characterization and astrophysical inference as detector sensitivities improve. We present SEOBNRv5iHM, an updated quasi-circular, aligned-spin inspiral-merger-ringdown gravitational-waveform model with higher-order modes, constructed within the effective-one-body formalism and building upon SEOBNRv5HM. The improvements mainly concern the late inspiral and the merger-ringdown: we remove the non-quasi-circular corrections used in previous models and instead introduce a phenomenological intermediate region between the inspiral and the ringdown, which allows the ringdown attachment time to be chosen independently for each mode, including at the peak of the mode's amplitude. The model is calibrated and validated against 591 quasi-circular aligned-spin waveforms from the third Simulating eXtreme Spacetimes catalog. For the $(2,2)$ mode, when considering the maximum unfaithfulness against numerical relativity over a total mass range of 10-300$M_\odot$, SEOBNRv5iHM achieves a median of $4.25\times10^{-5}$, a factor of 4.5 below SEOBNRv5HM, and a factor of 3-8 below other semi-analytical models, with $84\%$ of cases below $10^{-4}$. For $M\ge150 M_\odot$, the median drops to $9.7\times10^{-6}$, comparable to the numerical-relativity surrogate NRHybSur3dq8. For POLARIZATION mismatches at inclination $π/3$, with modes up to $\ell_\mathrm{max} = 5$, the median maximum unfaithfulness is $4.2\times10^{-4}$, a factor of 2.6 below SEOBNRv5HM, 1.9 below IMRPhenomTHM, and 6-11 below the other semi-analytical models. Since spin-precessing and eccentric models are built on top of the quasi-circular, aligned-spin baseline, these improvements will make future SEOBNR models more accurate, reducing waveform systematics in upcoming analyses.
[abstract 21 / 65] (score: 3) - Title: Unveiling a Concentration of Hard X-Ray Point Sources in the Nuclear Stellar Disk with XMM-NewtonAuthors: Shifra Mandel, Kaya Mori, Gabriele Ponti, Samaresh Mondal, Charles J. Hailey, Michael M. Shara, Tong Bao, Heshou Zhang, Mark R. Morris, JaeSub Hong, Jonathan Grindlay, Nicola Locatelli, Simone Piscitelli,Comments: Submitted to ApJ; comments welcomeSubjects: astro-ph.HE astro-ph.GACreated: 2026-11-08; Updated: 2026-11-10; Datestamp: 2026-11-10
The Galactic Center is home to the largest known concentration of X-ray sources ever detected in our Galaxy, including a sizable population of accreting compact objects. Utilizing data from the XMM-Newton Galactic Plane Heritage Survey of the central $20^{\circ}\times2^{\circ}$ of the Milky Way, we investigate the varying source populations in the inner regions of the Galaxy. We identify for the first time a concentration of extremely hard X-ray sources within $|l|<1.3^{\circ}$ and $|b|<0.3^{\circ}$, a region that overlaps the nuclear stellar disk (NSD). We determine that this hardness is intrinsic to the sources and not a manifestation of high line-of-sight column density ($N_{\rm H}$). Unlike the "soft" X-ray sources, this population does not trace the stellar mass distribution, indicating an overabundance compared to the underlying stellar population. We simulate spectra for a variety of source types to model their X-ray hardness and compare their distributions to those we observed in our survey data. We find that a significant subset of the Galactic Center X-ray population may comprise intermediate polars (IPs) with massive white dwarfs, possibly formed through dynamical processes. Our study provides novel observational insights into the distribution of stellar remnants and other X-ray sources in the vicinity of our supermassive BLACK HOLE, Sgr A*.
[abstract 22 / 65] (score: 3) - Title: Axion-Photon Conversion in Variable-Domain Magnetic Fields and the Highest-Energy Photons from GRB 221009AAuthors: Rick Sundar Garai, Tanmoy Kumar, Sourov Roy,Comments: 12 pages, 8 figuresSubjects: hep-phCreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
We investigate photon-ALP conversion as a simultaneous explanation of the ultra-high-energy photons observed from GRB 221009A by LHAASO and of the $\sim300$ TeV photon reported by Carpet-3. We model the MAGNETic field of the host galaxy as a set of domains with randomly oriented field directions and variable domain lengths, and propagate the photon-ALP system through the host galaxy, the intergalactic medium and the Milky Way. Fitting the combined LHAASO and Carpet-3 spectra, we find that a broad distribution of domain lengths raises the photon survival probability at the highest energies and accommodates the Carpet-3 point with photon-ALP conversion alone. The best fit, $m_a=3.85\times10^{-7}$~eV and $g_{aγ}=3.07\times10^{-11}\,\mathrm{GeV}^{-1}$, lies below the CAST bound, and parts of the $1σ$ and $2σ$ regions are also compatible with it.
[abstract 23 / 65] (score: 3) - Title: CMB Bounds on Primordial Black Holes via Radiation Capture: Linear PerturbationsAuthors: M. Farhang, S. M. S. Movahed,Comments: 5 pages, 2 figuresSubjects: astro-ph.COCreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
We investigate the gravitational interaction between primordial radiation, consisting of photons and ultra-RELATIVISTIC neutrinos, and primordial BLACK HOLEs (PBHs), and study its imprint on the anisotropies of the cosmic microwave background (CMB). Assuming that PBHs are immersed in the cosmic radiation background, we introduce a covariant energy-momentum transfer four-vector to describe the gravitational capture of radiation by PBHs. We extend the background-level framework of M. Farhang and S. M. S. Movahed [Phys. Rev. D 114, 083533 (2026)] to an inhomogeneous Universe at linear order by consistently modifying the perturbed continuity and Euler equations to account for both energy and momentum transfer. We use the imprint of this interaction on the CMB to place novel constraints on the PBH abundance, $f_{\rm pbh}$. We show that these constraints are up to two orders of magnitude tighter than those obtained from background-only analyses and exhibit a strong dependence on the PBH mass. Using Planck temperature and POLARIZATION data, we constrain the PBH fraction to $f_{\rm pbh} \lesssim 0.05-0.002$ for $M$ in the range $10^{15}-10^{17} M_\odot$. Furthermore, sensitivity forecasts for a cosmic-variance-limited survey with $\ell_{\rm max}=7000$, assuming a fiducial $f_{\rm pbh}=0$, yield projected bounds of $f_{\rm pbh} \lesssim 10^{-2}-2\times 10^{-4}$ over the mass range $10^{13}-10^{17} M_\odot$.
[abstract 24 / 65] (score: 3) - Title: Long before plunge: Uncovering intermediate-mass BLACK HOLEs through their inspiralling compact object companions with LISAAuthors: Jean Maurice Meus, Christian Chapman-Bird, Alberto Vecchio,Comments: 28 pages, 14 figuresSubjects: astro-ph.HE astro-ph.GA gr-qcCreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
The Laser Interferometer Space Antenna (LISA) will provide novel capability to discover and study intermediate-mass (~$10^2-10^5 M_\odot$) BLACK HOLEs at the centres of dwarf galaxies and in dense stellar environments. We systematically map out the LISA-detectable parameter space of binaries consisting of a low-mass compact object spiralling into an intermediate-mass BLACK HOLE (mass ratio ~$10^{-5} - 10^{-2}$) on equatorial orbits with generic eccentricity. The depth of the LISA survey reaches a redshift ~$5$ ($0.1$) for binaries with a primary BLACK HOLE mass $m_1$ ~$10^4 M_\odot$ ($10^3 M_\odot$). If the orbital companion is a white dwarf, which could be disrupted prior to plunge, LISA's survey depth is well matched to (and, in many cases, exceeds) the one of electro-MAGNETic surveys. Although the maximum distance at which a source can be detected depends weakly on the orbital eccentricity, the latter strongly affects the portion of the binary inspiral over which a source is detectable. The instrument's sensitivity time-volume varies by many orders of magnitude depending on the binary's component masses: it reaches ~$1 - 10^3 Gpc^3 yr$ (~$10^{-2} - 10^3 Gpc^3 yr$) for the more massive systems with $m_1 = 10^5 M_\odot$ ($10^4 M_\odot$) and decreases to ~$10^{-4} - 1 Gpc^3 yr$ for lighter primary BLACK HOLEs with $m_1 = 10^3 M_\odot$. Importantly, from tens of percent to the overwhelming majority of the total sensitivity time-volume (and therefore number of potential detections) comes from sources that do not plunge during the yr-long mission lifetime and are observed at an earlier stage of their inspiral. Despite the poorly known merger rates of this class of sources, our results show that LISA could identify from a handful to ~$10^3$ intermediate-mass BLACK HOLEs providing a new observational avenue for studying these elusive objects and the environments in which they reside.
[abstract 25 / 65] (score: 3) - Title: A Many-Shapes framework for Galactic Cosmic RaysAuthors: Paolo Lipari,Comments: 29 pages, 9 figuresSubjects: astro-ph.HECreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
Thanks to recent measurements by space and ground-level detectors, the energy spectra of COSMIC RAY protons and helium nuclei are now known with good precision over a broad energy range extending for more than six orders of magnitude, from a few GeV to approximately 10PeV. These measurements reveal that both spectra do not have a simple power--law form, and exhibit several features. The proton to helium ratio exhibits a very unexpected behavior: it decreases for rigidities $\lesssim 10^5$~GV, and increases for higher rigidities. Several authors have interpreted the observed spectral features as revealing the fact the CR spectra are formed by the contributions of a few components (in some cases as few as two) produced by sources that belong to distinct classes of astrophysical accelerators, with sources in the same class producing spectra with the same characteristic shape. Most of these authors also consider it necessary to include the contribution of one (or perhaps more than one) ``local'' sources, recently active in the vicinity of the solar system. However, this approach has several limitations, and in this work we discuss an alternative scenario in which the COSMIC RAY sources, even belonging to the same class, produce spectra with a broad range of shapes. The power--law form of the total source spectrum emerges as the average of these contributions. In this framework observable spectral features can be produced by statistical fluctuations, and different spectral slopes for protons and helium nuclei can be observed even if one assumes that acceleration is rigidity-dependent.
[abstract 26 / 65] (score: 3) - Title: GRB 241030A: A fallback-accreting MAGNETar description of the early X-ray emissionAuthors: Nissim Fraija, Simone Dichiara, Antonio Galván,Comments: 20 pages, 6 figures, 4 tables. Accepted in MNRASSubjects: astro-ph.HECreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
The bright, variable early X-ray emission of GRB~241030A at $z=1.411$ motivates investigating continued central-engine activity before the smoother afterglow emerges. We model a possible underlying MAGNETar contribution to the unabsorbed 0.3--10~keV XRT flux over 80--430~s, evolving the spin under fallback-disk and electroMAGNETic torques. A descriptive estimate gives $P_0\simeq4.25$~ms, $B\simeq3.04\times10^{15}$~G and source-frame $t_{\rm fb}\simeq143$~s, with exploratory temporal-block uncertainty ranges. The effective efficiency reaches its geometry-dependent ceiling of 81.2. At observer time 200~s, this realization has $P_*\simeq4.82$~ms and MAGNETospheric, corotation and light-cylinder radii $r_{\rm m}\simeq235$~km, $r_{\rm co}\simeq48$~km and $r_{\rm LC}\simeq230$~km. It is on the ejector branch; light-cylinder entry near 255~s initiates negative propeller torque and steepens the decline. The smooth component declines throughout the fitted interval; additional variable emission contributes to the observed maximum near 180~s. A correlated-residual Bayesian analysis permits a fainter component and broader dynamical histories, with median $P_0=16.8$~ms and central 68 per cent interval 2.76--286~ms. However, posterior predictive checks reveal that this statistical description typically underpredicts the observed flux level and variability, limiting its physical interpretation. Fallback-modified MAGNETar activity remains a possible descriptive scenario, but these analyses do not establish a unique underlying component or robust constraints on the initial spin and disk-interaction history. We also discuss Lense-Thirring precession and alternative mechanisms as possible origins of the early X-ray variability.
[abstract 27 / 65] (score: 2) - Title: Global MHD simulations of the solar convective zone using a volleyball mesh decomposition. I. PilotAuthors: Andrius Popovas, Åke Nordlund, Mikolaj Szydlarski, Yixiao Zhou,Comments: 14 pages, 10 figures, 3 appendices (5 pages), submitted to A&ASubjects: astro-ph.SR physics.comp-phCreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
Solar modelling has long been split into `internal' and `surface' modelling because of the lack of tools to connect the very different scales in space and time, as well as the widely different environments and the dominating physical effects involved. Significant efforts have recently been put into resolving this disconnect. We address the outstanding bottlenecks in connecting internal convection zone and dynamo simulations to the surface of the Sun, and conduct a proof-of-concept high-resolution global simulation of the convection zone of the Sun, using the task-based DISPATCH code framework. We present a new `volleyball' mesh decomposition, which has Cartesian patches tessellated on a sphere with no singularities. We use our new entropy based HLLS approximate Riemann solver to model MAGNETo-hydrodynamics in a global simulation, ranging between 0.655---0.998 R$_\odot$, with an initial ambient MAGNETic field set to 0.1 Gauss. This paper describes the methods and the pilot runs of the setup. The mesh decomposition exhibits neither unwanted artefacts, nor noise build-up. The simulations develop convective motions with complex, turbulent structures. Small-scale dynamo action twists the ambient MAGNETic field and locally amplifies MAGNETic field magnitudes by more than two orders of magnitude within the initial run-time.
[abstract 28 / 65] (score: 2) - Title: Collisionless relaxation as the origin of the anisotropic, non-thermal, and multi-temperature momentum distributions observed in space plasmasAuthors: Torsten Enßlin, Christoph Pfrommer,Comments: 21 pages, 2 figuresSubjects: physics.plasm-ph astro-ph.HECreated: 2026-11-08; Updated: 2026-11-10; Datestamp: 2026-11-10
Anisotropic, non-thermal, and multi-temperature distributed particle momenta are commonly observed in collisionless space plasmas, such as the solar wind. Using Liouville's theorem, we argue that anisotropic compression or expansion of the plasma, followed by a relaxation of the resulting anisotropic stress must lead to non-equilibrium states that exhibit either anisotropic, non-thermal distribution functions, different electron and ion temperatures, or a combination of these effects. We present arguments showing that a plasma in thermal equilibrium undergoing anisotropic compression or expansion cannot return to thermal equilibrium in the absence of particle collisions. Since most astrophysical plasmas are practically collisionless and experience significant anisotropic compression or expansion, we expect anisotropic, non-thermal, and multi-temperature particle distributions to be ubiquitous, in agreement with solar wind measurements.
[abstract 29 / 65] (score: 2) - Title: The Hunt for Red Dual AGNs I: Spatially-Resolved Mid-IR Dual AGNs in the DESI Legacy Imaging SurveysAuthors: Ryan W. Pfeifle, Kimberly A. Weaver, Barry Rothberg, Miranda McCarthy, Emma Schwartzman, Nathan J. Secrest, Peter G. Boorman, Daniel Stern, Joanna Piotrowska, Kevin McCarthy, Emily Moravec, Jenna M. Cann, Kimberly Engle, Kyla Mullaney, Ryan Tanner, Kelly Whalen,Comments: 39 pages, including 5 tables, 10 figures, and 4 appendix sections. Resubmitted to ApJ; feedback welcome!Subjects: astro-ph.GACreated: 2026-11-05; Updated: 2026-11-10; Datestamp: 2026-11-10
Theoretical studies predict that dual AGNs are a critical stage of galaxy merger-driven supermassive BLACK HOLE growth. Systematic searches for dual AGNs typically target late-stage mergers ($\leq10$ kpc nuclear separations) and select AGNs based on optical diagnostics. Yet, simulations predict that obscuration can occur early in the merger sequence, and that a significant fraction of dual AGNs can be found beyond $10$ kpc. Here, we report on a new sample of 155 spatially resolved mid-IR dual AGNs candidates selected based upon their mid-IR $W1-W2$ colors from the Wide-Field Infrared Survey Explorer and optically classified as galaxy merger candidates using imaging from the DESI Legacy Imaging Surveys. Preliminary spectroscopic results are presented for approximately 2/3 of the sample. 78 candidates have been confirmed to reside in galaxy mergers; among these, 13 have been confirmed as bona fide mid-IR dual AGNs, while 65 represent strong dual AGN candidates that require further examination. 48 candidates have been rejected as non-merger contaminants (foreground-background AGNs, separations inconsistent with interacting galaxies, etc.). 29 candidates still await spectroscopic coverage. The confirmed and high confidence dual AGN candidates exhibit separations of 14.5-129 kpc; $>50%$ reside at separations $>50$ kpc. Confirmed and high confidence candidates also exhibit a diversity of nuclear optical BPT classes. Seyfert-Seyferts and Seyfert-HIIs dominate the overall BPT pairings. 31% of confirmed mid-IR dual AGNs reside in multi-mergers involving three or more galaxies. The diversity in AGN properties and environments identified in this work highlights the importance of multiwavelength selection strategies and analyses in the quest to holistically understand dual AGNs as a population.
[abstract 30 / 65] (score: 2) - Title: Eccentric Stellar-mass Binary Black Holes: Population, Detectability, and Waveform Analysis in the LISA and LIGO EraAuthors: Zeyuan Xuan, Smadar Naoz, Kyle Kremer, Michael L. Katz, Bence Kocsis, Erez Michaely,Comments: 28 pages, 14 figures. Accepted by PRDSubjects: astro-ph.HE gr-qcCreated: 2026-11-06; Updated: 2026-11-10; Datestamp: 2026-11-10
Eccentric binary BLACK HOLEs (BBHs) formed through dynamical interactions can significantly contribute to gravitational wave (GW) detections. In this work, we present a simulated catalog of dynamically-formed, stellar-mass BBHs in the local universe, incorporating contributions from the Galactic field (flyby interactions), Galactic nucleus (eccentric Kozai-Lidov evolution), and globular clusters (N-body interactions). Our results predict a wide, highly eccentric BBH population in the Milky Way (MW), with source counts of $\sim 25, 9, 3, 1, <1$ for a 4-year LISA mission and $\sim 36, 13, 5, 2, 1$ for a 10-year mission, at $\mathrm{SNR} > 1, 3, 8, 20, 50$, respectively. Extending this model to cosmological populations, we show that different dynamical channels can produce distinct eccentricity distributions in the LVK band and can contribute hundreds of additional low-SNR mHz sources. Specifically, our model yields a merger rate of $Γ\sim 9 \mathrm{Gpc}^{-3}\mathrm{yr}^{-1}$ and $\sim 150$ extragalactic mHz BBHs with $\mathrm{SNR} > 1$. However, due to the lower mass and weaker GW signals of stellar-mass BBHs, this number declines sharply at higher detection thresholds (e.g., $\sim 1$ for $\mathrm{SNR} > 8$). We further highlight the impact of eccentric BBH signals on the LISA global fit, showing that their individual harmonics can be independently detected in the Milky Way, and may mimic circular binaries with systematically biased chirp masses. Lastly, we show that post-Newtonian waveforms converge reliably for eccentric BBHs with masses of $\lesssim 10^3 M_\odot$ in the mHz band. Overall, eccentric BBHs represent a prevalent and promising target for future space-based GW observatories. The simulated catalog and the LISA Eccentricity Astrophysics Package (LEAP) developed in this work are publicly available at https://github.com/zeyuanxuan/lisa-leap/.
[abstract 31 / 65] (score: 2) - Title: ElectroMAGNETic duality degeneracy in dynamical BLACK HOLE mergersAuthors: José Ferreira, Gabriele Bozzola, Carlos A. R. Herdeiro, Vasileios Paschalidis, Miguel Zilhão,Comments: 11 pages, 9 figuresSubjects: gr-qc hep-thCreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
ElectroMAGNETic duality is a symmetry of the source-free Einstein-Maxwell equations that rotates electric and MAGNETic fields while leaving the stress-energy tensor invariant. We present the first fully nonlinear realization of this symmetry in dynamical strong-gravity regimes by performing numerical relativity simulations of charged BLACK HOLE mergers across a continuous duality family. Starting from electrically charged binaries, we generate dyonic and MAGNETically charged configurations via duality rotations and evolve them within a common numerical framework. We find that all dual configurations exhibit identical spacetime dynamics, while the emitted electroMAGNETic radiation is related by a rotation of its POLARIZATION equal to the duality angle. Our results demonstrate a degeneracy of gravitational observables under electroMAGNETic duality and provide a concrete mapping between dual configurations at the level of radiation, establishing electroMAGNETic duality as an organizing principle for dynamical Einstein-Maxwell solutions.
[abstract 32 / 65] (score: 2) - Title: Quasi-DNS with chemical kinetics for a single multiple-injection burner element under stable lean conditions for future gas turbine applicationsAuthors: Kazuki Abe, Youhi Morii, Kaoru Maruta,Comments: 25 pages, 15 figures. Title changed; revised following peer review. Published in MethodsXSubjects: physics.flu-dynCreated: 2026-11-08; Updated: 2026-11-10; Datestamp: 2026-11-10
We develop a Quasi-DNS with chemical kinetics for a stable lean condition in a single multiple-injection burner element for future gas turbine applications, as a reusable workflow for a coaxial mixing-tube burner. Here, Quasi-DNS denotes a high-resolution, turbulence-model-free calculation; it is not DNS in the strict sense. The OpenFOAM-based method includes: (i) a simplified 30deg sector geometry capturing vortices at the mixing tube outlet, (ii) boundary conditions reproducing coaxial JETs and preheated air, (iii) a reduced Correa methane-air mechanism compared with GRI 3.0 using Cantera, (iv) mesh-development and grid-sensitivity assessment based on flame structure and the squared gradient of mixture fraction, and (v) post-processing with methane-based flame index. Demonstration at an equivalence ratio phi = 0.45 shows limited in-tube mixing and strong outlet vortices, yielding a more extended heat release region than the RANS solution. - A reusable high-resolution, turbulence-model-free Quasi-DNS workflow with detailed methane-air chemistry is developed for a coaxial mixing-tube burner. - The workflow combines a reduced methane-air mechanism, refined sector-domain meshes, and scalar-field diagnostics for characterizing mixing and heat release regions. - The workflow enables analysis of mixing and flame stabilization under stable lean conditions, and provides a high-resolution numerical reference under the stated assumptions for comparison with RANS-based calculations.
[abstract 33 / 65] (score: 2) - Title: Too shy to spin? Cosmic wallflowers as proto-globular clustersAuthors: Floor van Donkelaar, Lucio Mayer, Pedro R. Capelo,Comments: 9 pages, accepted to MNRASSubjects: astro-ph.GA astro-ph.HECreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
We investigate the rotational properties of star-forming clusters at $z \sim 7.6$ in the high-resolution simulation MassiveBlackPS, focusing on two formation channels: clusters forming in galactic discs via gravitational instability and isolated circumgalactic systems, referred to as cosmic wallflowers, born out of cosmic filaments. Using stellar kinematics, we compare their rotational velocities, $v_{\rm rot}$, and rotational support, $v/σ$, to study whether formation environment leaves a clear dynamical imprint. We find a clear separation, wherein cosmic wallflowers systematically have lower rotational velocities and span a wide range in $v/σ$, whereas the identified disc clusters are strongly rotation-dominated and extend to higher $v_{\rm rot}$. When combined with stellar surface densities, a subset of the low-$v_{\rm rot}$ cosmic wallflowers lie surprisingly close to the observed globular cluster population in the Milky Way, whereas disc clusters remain offset. Within the cosmic wallflower population, we identify two regimes: lower-density, weakly rotating systems that overlap with these globular cluster properties, and denser, more rotationally supported systems that likely follow a different evolutionary pathway, possibly linking them to the origin of massive BLACK HOLE seeds at high redshift. We further find that the gas content correlates with this behaviour, with gas-rich cosmic wallflowers preferentially occupying this low-rotation regime. This all suggests that environment and baryonic content together play a key role in setting the initial dynamical state and possible fate of clusters. In particular, weakly rotating, gas-rich cosmic wallflowers emerge as natural proto-globular cluster candidates, potentially evolving towards present-day systems through angular momentum loss and dynamical heating.
[abstract 34 / 65] (score: 2) - Title: Star Planet InteractionsAuthors: Arghyadeep Paul, Kristina Kislyakova, Manuel Güdel, Rim Fares, Judy Chebly, Sergio Joya, Miljenko Čemeljić, Katja Poppenhäger, Julian Alvarado-Gomez, Silva Järvinen, Cesar Bertucci, Dibyendu Nandy, Antonio García Muñoz, Antoine Strugarek, Mayank Narang, Shyama Narendranath,Comments: Submitted to Space Science ReviewsSubjects: astro-ph.SR astro-ph.EPCreated: 2026-11-08; Updated: 2026-11-10; Datestamp: 2026-11-10
Star-planet interactions (SPIs) describe the continuous exchange of energy, momentum, and mass between exoplanets and their host stars through radiative, tidal, MAGNETic, and particle-driven processes. Together, these interactions shape the structure, evolution, and observable properties of exoplanetary systems. In this review, we bring together current theoretical and observational understanding of SPIs, highlighting how stellar radiation, winds, and MAGNETic activity influence planetary atmospheres, interiors, and orbital evolution, while using the Solar System as a valuable reference for interpreting these processes. High-energy stellar radiation, particularly in the far- and extreme-ultraviolet and X-ray bands, drives atmospheric heating, photochemistry, ionisation, and escape. These effects are further influenced by stellar winds and MAGNETic interactions, which can either protect planetary atmospheres or accelerate their loss over time. Tidal interactions redistribute energy and angular momentum, producing internal heating and driving orbital migration and circularisation. Magnetic star-planet coupling provides additional pathways for energy transfer through RECONNECTion and current systems, potentially enhancing atmospheric escape, heating planetary ionospheres and interiors, and generating observable signatures such as radio emission and enhanced stellar activity. We discuss how these processes work together, emphasising that their long-term impact depends on stellar evolution, planetary properties, atmospheric structure, and MAGNETic field strength. By presenting radiative, tidal, and MAGNETic interactions within a unified framework, this review highlights the physical mechanisms that shape planetary environments and identifies the key observational signatures that will complement future studies of exoplanet evolution and habitability.
[abstract 35 / 65] (score: 2) - Title: The Galactic Neutrino Sky: Predictions from Gamma-ray Source PopulationsAuthors: Leo Seen, Ke Fang,Comments: 7+4 pages, 4+3 figuresSubjects: astro-ph.HECreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
High-energy neutrino emission from the Galactic plane has been detected at a significance of $5.7σ$, with a prominent excess toward the inner Galaxy. We show that this excess can be naturally explained by the spatial distribution of Galactic neutrino sources. By combining $γ$-ray source catalogs spanning GeV-PeV energies and selecting candidate hadronic emitters, we construct ReGal-$γ$, a template of resolved Galactic $γ$-ray sources that may also produce high-energy neutrinos. Compared with models of Galactic diffuse emission, ReGal-$γ$ predicts a neutrino intensity that is more strongly concentrated toward the inner Galaxy. Combined with models of diffuse cosmic-ray emission and unresolved $γ$-ray sources, the template reproduces both the spectral energy distribution and the Galactic longitudinal count profile reported by IceCube without requiring additional renormalization of the emission models. We test this result using an independent $γ$-ray source template constructed from different catalogs and find that our conclusion is robust against uncertainties in source modeling. Future measurements of the energy-dependent longitudinal and latitudinal neutrino distributions will provide tighter constraints on these models and help determine the spatial distribution of Galactic neutrino sources.
[abstract 36 / 65] (score: 2) - Title: Particle acceleration in Alfvénic turbulence with a strong guide fieldAuthors: Daniel Humphrey, Stanislav Boldyrev, Vadim Roytershteyn,Comments: 10 pages, 6 figuresSubjects: astro-ph.HE astro-ph.GACreated: 2026-11-08; Updated: 2026-11-10; Datestamp: 2026-11-10
Magnetically dominated Alfvénic turbulence creates an effective environment for particle acceleration. However, when a strong mean field is present, traditional mechanisms like mirror and curvature acceleration become inefficient at explaining non-thermal particle energy distributions. Based on numerical and phenomenological study, we propose that in such turbulence, particles are accelerated in charge-starved current sheets, corresponding to current velocities approaching the speed of light. The distributions of the electric currents, plasma density, fluctuations of electric charge, as well as the energy distributions of accelerated particles, approximately follow log-normal statistics. Non-thermal particle distributions thus arise from particle acceleration in these charge-starved current sheets rather than from conventional FERMI-type particle acceleration by turbulent eddies.
[abstract 37 / 65] (score: 2) - Title: Transient discs around isolated accreting neutron starsAuthors: Marina D. Afonina, Anton V. Biryukov, Sergei B. Popov, Arthur G. Suvorov,Comments: 21 pages, 6 figures, accepted to JHEAPSubjects: astro-ph.HECreated: 2026-11-06; Updated: 2026-11-10; Datestamp: 2026-11-10
Mature, isolated neutron stars can accrete from the interstellar medium. Due to turbulence, the accreted gas can have a substantial angular momentum and form a disc around the compact object. In this paper, we perform a population synthesis of isolated neutron stars in the Milky Way that specifically tracks the possibility of disc formation, which typically requires a low spatial velocity of the compact object ($\lesssim 40$ km s$^{-1}$). In general, weak MAGNETic fields favour disc formation as the MAGNETosphere occupies a smaller volume. Still, even in the case of fields decaying exponentially over a characteristic timescale of $\sim 1.5$ Gyr, we find that for several realistic models of propeller spin-down, only a small fraction of accretors (down to $\sim 0.02$ %) attain discs. However, disc-accreting isolated neutron stars are relatively numerous among the brightest sources. We estimate that their number can reach a few hundred at X-ray fluxes of $\gtrsim 10^{-14}$ erg s$^{-1}$ cm$^{-2}$. We speculate that disc-accreting isolated neutron stars can manifest as long-period radio transient sources via electron cyclotron maser emission, predicting spectra and critical conditions for quenching.
[abstract 38 / 65] (score: 2) - Title: Energy Partitioning at the Termination ShockAuthors: Judit Szente, Bart van der Holst, Gabor Toth, Merav Opher,Comments:Subjects: astro-ph.SRCreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
We show new results of a global 3D MAGNETohydrodynamic (MHD) simulation of the Boston University outer heliosphere model where we used a newly developed approach that distributes the non-adiabatic shock heating among the cold protons, electrons, and pickup-ions (PUIs), while maintaining total energy conservation of all ions. In previous simulations (E. S. Bair et al. 2025; B. van der Holst et al. 2026) non-adiabatic shock heating was distributed such that the resulting proton temperature jump at the termination shock (TS) was too high. Using a new methodology the simulation results improved with respect to the solar wind proton temperature jump observed at the TS by Voyager 2. Because we directly control the distribution of non-adiabatic heating at the TS, we have the opportunity to study the scenario of a non-adiabatic physical process heating cold plasma and PUIs in the TS and its effect on the global MHD solution. The results show that having a fraction of up to 8.5\% of the non-adiabatic shock heating going towards thermal solar wind protons at the TS reproduces the jump conditions observed along the V2 trajectory. This fraction depends on the thermal proton and PUI number densities. This information is key to understanding the physical processes that shape the heliosphere. As shown by M. Opher et al. (2020), PUIs significantly change the shape of the heliosphere; for example, the presence of hot PUIs results in a thinner inner heliosheath. Our work provides the architecture of how energy partitioning at shocks in kinetic simulations (J. Giacalone et al. 2021) can be utilized in global MHD models.
[abstract 39 / 65] (score: 2) - Title: Resolving the Galactic Center Region's Gamma-Ray Emission and Searching for its Neutrino Counterpart with HAWC and IceCubeAuthors: R. Alfaro, M. Araya, J. Arteaga-Velázquez, R. Babu, P. Bangale, A. Bernal, K. Caballero-Mora, T. Capistrán, A. Carramiñana, F. Carreón, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, C. de León, E. De la Fuente, N. Di Lalla, R. Diaz Hernandez, M. DuVernois, K. Engel, T. Ergin, C. Espinoza, N. Fraija, J. García-González, F. Garfias, N. Ghosh, S. Giri, A. Gonzalez Muñoz, M. González, J. González, J. Goodman, S. Groetsch, J. Gyeong, J. Harding, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, S. Kaufmann, D. Kieda, K. Leavitt, J. Lee, H. León Vargas, A. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, H. Martínez-Huerta, J. Matthews, P. Miranda-Romagnoli, P. Mirón-Enriquez, J. Morales-Soto, E. Moreno, M. Mostafá, M. Najafi, L. Nellen, Y. Niroula, M. Nisa, R. Noriega-Papaqui, M. Osorio-Archila, E. Ponce, Y. Pérez Araujo, E. Pérez-Pérez, D. Rosa-González, M. Roth, A. Sandoval, M. Schneider, J. Serna-Franco, S. Shankar, A. Smith, Y. Son, R. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, E. Varela, L. Villaseñor, H. Wu, X. Wang, Z. Wang, I. Watson, S. Yu, S. Yun-Cárcamo, X. Zhang, H. Zhou, for the HAWC collaboration, R. Abbasi, M. Ackermann, J. Adams, J. Aguilar, M. Ahlers, J. Alameddine, S. Ali, N. Amin, K. Andeen, C. Argüelles, S. Athanasiadou, S. Axani, X. Bai, A. Balagopal V., S. Barwick, V. Basu, R. Bay, J. Beatty, J. Becker Tjus, J. Beise, C. Bellenghi, S. Benkel, S. BenZvi, D. Berley, E. Bernardini, D. Besson, E. Blaufuss, L. Bloom, S. Blot, F. Bontempo, J. Book Motzkin, C. Boscolo Meneguolo, S. Böser, O. Botner, J. Braun, B. Brinson, Z. Brisson-Tsavoussis, L. Brusa, R. Burley, D. Butterfield, K. Carloni, J. Carpio, N. Chau, Y. Chen, Z. Chen, D. Chirkin, S. Choi, A. Chubarov, B. Clark, D. Coloma Borja, A. Connolly, J. Conrad, D. Cowen, C. De Clercq, J. DeLaunay, D. Delgado, T. Delmeulle, S. Deng, P. Desiati, K. de Vries, G. de Wasseige, T. DeYoung, J. Díaz-Vélez, S. DiKerby, T. Ding, M. Dittmer, A. Domi, L. Draper, L. Dueser, D. Durnford, K. Dutta, M. DuVernois, T. Ehrhardt, L. Eidenschink, A. Eimer, C. Eldridge, P. Eller, E. Ellinger, D. Elsässer, R. Engel, H. Erpenbeck, W. Esmail, S. Eulig, J. Evans, P. Evenson, K. Fan, K. Fang, K. Farrag, A. Fattorini, A. Fazely, A. Fedynitch, N. Feigl, C. Finley, D. Fox, A. Franckowiak, S. Fukami, P. Fürst, J. Gallagher, A. Garcia, M. Garcia, E. Genton, L. Gerhardt, A. Ghadimi, C. Glaser, T. Glüsenkamp, J. Gonzalez, S. Goswami, A. Granados, D. Grant, S. Gray, S. Griffin, S. Griswold, K. Groth, D. Guevel, C. Günther, P. Gutjahr, C. Ha, A. Hallgren, F. Halzen, M. Handt, K. Hanson, J. Hardin, A. Harnisch, P. Hatch, A. Haungs, J. Häußler, K. Helbing, J. Hellrung, B. Henke, L. Hennig, F. Henningsen, L. Heuermann, R. Hewett, N. Heyer, S. Hickford, A. Hidvegi, C. Hill, G. Hill, R. Hmaid, K. Hoffman, A. Hollnagel, D. Hooper, S. Hori, K. Hoshina, M. Hostert, W. Hou, M. Hrywniak, T. Huber, K. Hultqvist, K. Hymon, A. Ishihara, W. Iwakiri, M. Jacquart, S. Jain, O. Janik, M. Jansson, M. Jin, N. Kamp, D. Kang, W. Kang, A. Kappes, L. Kardum, T. Karg, A. Karle, A. Katil, M. Kauer, J. Kelley, B. Kern, M. Khanal, A. Khatee Zathul, A. Kheirandish, T. Kim, H. Kimku, F. Kirchner, J. Kiryluk, C. Klein, S. Klein, Y. Kobayashi, S. Koch, A. Kochocki, R. Koirala, H. Kolanoski, T. Kontrimas, L. Köpke, C. Kopper, D. Koskinen, P. Koundal, M. Kowalski, T. Kozynets, A. Kravka, N. Krieger, T. Krishnan, K. Kruiswijk, E. Krupczak, E. Kun, N. Kurahashi, C. Lagunas Gualda, L. Lallement Arnaud, M. Larson, F. Lauber, J. Lazar, K. Leonard DeHolton, A. Leszczyńska, C. Li, J. Liao, C. Lin, Q. Liu, Y. Liu, M. Liubarska, C. Love, L. Lu, F. Lucarelli, W. Luszczak, Y. Lyu, M. Macdonald, E. Magnus, Y. Makino, E. Manao, S. Mancina, A. Mand, I. Mariş, S. Marka, Z. Marka, I. Martinez-Soler, R. Maruyama, J. Mauro, F. Mayhew, F. McNally, K. Meagher, A. Medina, M. Meier, Y. Merckx, L. Merten, J. Mitchell, L. Molchany, S. Mondal, T. Montaruli, R. Moore, Y. Morii, A. Mosbrugger, D. Mousadi, E. Moyaux, T. Mukherjee, M. Nakos, U. Naumann, R. Neshat, L. Neste, M. Neumann, K. Noda, A. Noell, A. Novikov, A. Obertacke, V. O'Dell, A. Olivas, R. Orsoe, J. Osborn, E. O'Sullivan, B. Owens, V. Palusova, H. Pandya, A. Parenti, C. Parisel, N. Park, V. Parrish, E. Paudel, L. Paul, C. Pérez de los Heros, T. Pernice, T. Petersen, J. Peterson, S. Pick, M. Plum, A. Pontén, V. Poojyam, B. Pries, R. Procter-Murphy, G. Przybylski, L. Pyras, C. Raab, J. Rack-Helleis, N. Rad, M. Ravn, K. Rawlins, Z. Rechav, A. Rehman, R. Reimann, I. Reistroffer, E. Resconi, C. Rho, W. Rhode, L. Ricca, B. Riedel, A. Rifaie, E. Roberts, S. Rodan, M. Rongen, A. Rosted, C. Rott, T. Ruhe, L. Ruohan, D. Ryckbosch, J. Saffer, D. Salazar-Gallegos, P. Sampathkumar, A. Sandrock, G. Sanger-Johnson, M. Santander, S. Sarkar, M. Scarnera, M. Schaufel, H. Schieler, S. Schindler, L. Schlickmann, B. Schlüter, F. Schlüter, N. Schmeisser, T. Schmidt, F. Schmitt, A. Scholz, F. Schröder, S. Schwirn, S. Sclafani, D. Seckel, L. Seen, M. Seikh, S. Seunarine, P. Sevle Myhr, R. Shah, S. Shah, A. Sharma, S. Shefali, N. Shimizu, M. Shin, R. Singh, B. Skrzypek, R. Snihur, J. Soedingrekso, D. Soldin, P. Soldin, G. Sommani, D. Song, C. Spannfellner, G. Spiczak, C. Spiering, J. Stachurska, M. Stamatikos, T. Stanev, T. Stezelberger, T. Stürwald, T. Stuttard, G. Sullivan, I. Taboada, S. Ter-Antonyan, A. Terliuk, A. Thakuri, P. Thelen, M. Thiesmeyer, W. Thompson, J. Thwaites, W. Tian, S. Tilav, J. Torres, S. Toscano, D. Tosi, K. Upshaw, A. Vaidyanathan, N. Valtonen-Mattila, J. Valverde, J. Vandenbroucke, T. Van Eeden, N. van Eijndhoven, L. Van Rootselaar, J. van Santen, J. Vara, F. Varsi, M. Velazquez, M. Venugopal, M. Vereecken, S. Vergara Carrasco, S. Verpoest, A. Vijai, J. Villarreal, C. Walck, A. Wang, E. Warrick, C. Weaver, P. Weigel, A. Weindl, J. Weldert, A. Wen, C. Wendt, J. Werthebach, M. Weyrauch, N. Whitehorn, C. Wiebusch, D. Williams, L. Witthaus, J. Woodward, G. Wrede, X. Xu, J. Yanez, Y. Yao, E. Yildizci, S. Yoshida, F. Yu, S. Yu, T. Yuan, A. Zander Jurowitzki, A. Zegarelli, S. Zhang, Z. Zhang, P. Zhelnin, P. Zilberman, C. Zilleruelo Cañas, M. Zimmermann for the IceCube collaboration,Comments: Accepted for publication in ApJ LettersSubjects: astro-ph.HECreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
The Galactic Center (GC) is a prime candidate for petaelectronvolt cosmic-ray acceleration, with gamma-ray emission observed by the High Altitude Water Cherenkov (HAWC) Observatory extending beyond 100~TeV. Using $\sim$2860 days of HAWC data with improved machine-learning gamma/hadron separation, we present the first spatially resolved model of the GC region at the highest gamma-ray energies. The emission is resolved into a point source, HAWC J1745-2857, and a Galactic diffuse emission component that was not significant in previous HAWC analyses. With the diffuse emission accounted for, the point-source spectrum extends beyond 100~TeV with no evidence of a cutoff, showing that the PeVatron interpretation of the GC does not arise from unresolved diffuse emission. Assuming a hadronic origin, we construct the corresponding neutrino signal template and search for it in 12 years of IceCube muon-track data. No significant neutrino excess is found, and we report the first upper limit on the high-energy neutrino flux associated with the multi-component spatial model of the GC derived from HAWC data. The limit is approximately 12 times the nominal neutrino flux predicted from the HAWC gamma-ray model under a hadronic interpretation. Although the limit does not yet test the optically thin hadronic scenario, it quantifies the sensitivity required to test the hadronic origin of the GC PeVatron with future neutrino observations.
[abstract 40 / 65] (score: 2) - Title: First Post-Newtonian Cross Terms in Hierarchical Triple Systems: Multiple-Scale Averaging and its Canonical ConsistencyAuthors: Hideyoshi Arakida,Comments: 29 pages, 3 figures The title of the paper has been changed, and the manuscript has also undergone substantial revision and restructuringSubjects: gr-qcCreated: 2026-11-06; Updated: 2026-11-10; Datestamp: 2026-11-10
We develop a two-stage multiple-scale method for hierarchical triple systems, using osculating orbital elements and time as the independent variable. We examine the disputed cross terms at orders $δ\varepsilon^{3/2}$ and $δ\varepsilon^{7/2}$, for which the multiple-scale results of Lim and Rodriguez (LR) disagree with the effective field theory results of Kuntz, Serra, and Trincherini (KST). Here, $δ$ is the first post-Newtonian (1PN) parameter, and $\varepsilon=a_*/a_2$ ($a_*\simeq a_1$) measures the orbital hierarchy. These terms arise from couplings between RELATIVISTIC interactions and the tidal field of the third body. Our results agree with KST: there is no secular term at order $δ\varepsilon^{3/2}$, while the $δ\varepsilon^{7/2}$ contribution consists of three parts: a direct term, a first-stage coupling between the inner binary's center-of-mass motion and the tidal field, and a second-stage coupling between the 1PN dipole and the quadrupole. Their sum reproduces the inner-orbit secular dynamics generated by KST's MAGNETic 1PN--quadrupole Hamiltonian, including its exact mass dependence, for nonsingular eccentricities and inclinations in the nonresonant, hierarchical weak-field regime. The analysis includes mean-anomaly perturbations and resubstitution of short-period corrections in both directions. We clarify how the choice of averaging variable affects the normalization of the mean elements and establish agreement with canonical perturbation theory. In particular, osculating and canonical mean elements give the same inner-orbit secular rates at this order.
[abstract 41 / 65] (score: 2) - Title: A strategy for astrometric QUASAR selection with Gaia DR3 and its application to discover new luminous $z>2$ QUASARsAuthors: J. Li, J. P. U. Fynbo,Comments: Accepted for publication in A&A. 12 pages, 31 figuresSubjects: astro-ph.GACreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
We aim to provide a cookbook for purely astrometric selection of QUASARs with Gaia DR3 and to provide an example of its use for the identification of very luminous $z>2$ QUASARs. We analyse the Gaia DR3 astrometry of confirmed QUASARs and stationary sources. We show that the proper motion signal to noise $μ/σ_μ$ follows a Rayleigh-like distribution. We also show the importance of properly taking into account the correlation between proper motions in right ascension and declination, as well as the non-linear error propagation. We adopt the Mahalanobis distance to the null proper-motion hypothesis. A scaled $χ^2$ distribution with $k=2$ and scale $s=1.1485$ is fitted to Gaia-CRF3; the corresponding $\pm2σ$ Gaussian-equivalent threshold is $D^2_{M(μ)}<7.097$. The final criteria combine this with the parallax condition and $\mathrm{ruwe}<1.4$. Applying the new criteria to the SDSS DR16Q confirmed QUASARs, the recovery rate is $90.25\%$. The suggested purely astrometric selection significantly improves both completeness and purity compared to other strategies used in the literature, reaching a QUASAR purity of approximately $95\%$ ($\sim2σ$ Gaussian-equivalent). It can be used to improve the selection purity and completeness for future QUASAR surveys. As an example, we use the suggested strategi to locate 24 very bright $z>2$ QUASARs without redshifts in the literature. Our proposed astrometric selection strategy recovers 95\% of known QUASARs. Its potential use for new discoveries is demonstrated by the identification of 24 very luminous $z>2$ QUASARs. Ten of these are new discoveries and for an additional seven we correct the redshifts determined by other methods.
[abstract 42 / 65] (score: 2) - Title: A Common Type II Origin of Galilean and Carroll SuperstringsAuthors: Mehmet Ozkan, Utku Zorba,Comments: 9 pages. Revised version with additional references and clarificationsSubjects: hep-th gr-qcCreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
We show that the RELATIVISTIC Type-II superalgebras, once the fundamental-string winding charge is retained alongside the momentum, admit a single non-Lorentzian contraction with two invariant translation ideals, whose complementary quotients yield Galilean and MAGNETic-Carroll superalgebras. The complementary vector charge required for this structure is thus intrinsic to string theory. The IIA realization is particle-like and the IIB realization string-like, a distinction fixed by chirality, and spacelike T-duality relates the two while preserving each non-Lorentzian structure. The same contraction is finite on the doubled Green--Schwarz action, including all fermion terms and local kappa symmetry, where the two supersymmetries appear as the two POLARIZATIONs of a single worldsheet theory. These results unify two distinct non-Lorentzian corners of string theory within a common Type-II origin and open a route toward a broader web of non-Lorentzian dualities and possible holographic generalizations.
[abstract 43 / 65] (score: 2) - Title: Excitation factors and exceptional points of Kerr--Newman quasinormal modesAuthors: Jun-Kun Zhao, Tieguang Zi,Comments: 14 pages, 6 figures; v2 references addedSubjects: gr-qcCreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
We study excitation factors and investigate exceptional points (EPs) of Kerr--Newman quasinormal modes using the exact separated gravitoelectroMAGNETic equations. At fixed charge, the magnitudes of the excitation factors for the gravitational-led modes studied here decrease with increasing spin, whereas those for electroMAGNETic-led modes exhibit both monotonic and nonmonotonic behavior. The magnitude of the excitation factor for the first overtone can be comparable to or larger than that for the fundamental mode. We identify 42 EPs at which pairs of modes coalesce in the gravitational-led and electroMAGNETic-led sectors. Some EPs form sequences involving successive overtone pairs, with higher-overtone pairs coalescing progressively closer to the extremal limit. The additional EPs identified outside these sequences all share the same mode-pair labels as sequence members, but occur at different values of the BLACK HOLE spin and charge. These findings clarify how rotation and charge shape the relative excitation strengths of different modes and the pattern of mode coalescence in the non-Hermitian spectrum of Kerr--Newman BLACK HOLEs.
[abstract 44 / 65] (score: 2) - Title: Low-Rank Tensor Manifolds for Turbulent Field Reconstruction from Sparse DataAuthors: Nazmus Sakib, Alexander G. Mychkovsky, Hessam Babaee,Comments: We updated the preprint template to remove journal-specific formattingSubjects: physics.flu-dynCreated: 2026-11-07; Updated: 2026-11-10; Datestamp: 2026-11-10
Reconstructing turbulent flow fields from sparse and irregular measurements remains challenging because the underlying inverse problem is severely underdetermined. Here we present MANTRA, a manifold-based tensor framework that represents each velocity component in a continuous tensor-product space while constraining its coefficient tensor to a low-rank Tucker manifold. This structure provides a compact, data-adaptive representation without requiring gridded observations or governing equations. Riemannian optimization and adaptive selection of rank and basis complexity enable the model to exploit coordinate-wise spatiotemporal correlations. In simulations of forced isotropic turbulence and flow over a cylinder, MANTRA recovers multiscale structures at sampling densities orders of magnitude below the underlying grids and remains accurate under Gaussian noise up to 20% of the peak velocity. It also recovers leading coordinate-wise correlation structures from sparse observations. Applied to experimental particle-tracking velocimetry of an oscillating impinging JET, MANTRA reveals time-evolving structures that are not apparent from the scattered measurements alone.
[abstract 45 / 65] (score: 2) - Title: Magnetohydrodynamic spectra and line invariants in the presence of axionsAuthors: P. M. Akhmetiev, M. S. Dvornikov, A. Yu. Smirnov,Comments: 29 pages in LaTeX, 7 pdf figures, accepted for the publication in Theor.Math.PhysSubjects: physics.plasm-ph astro-ph.HE astro-ph.SR hep-phCreated: 2026-11-05; Updated: 2026-11-10; Datestamp: 2026-11-10
A new form of the mean-field equations for MAGNETic fields, which accounts for the interaction with axions, is studied. It is shown that the asymptotic ergodic invariants of MAGNETic field lines play a key role in the evolution of MAGNETic fields, which determine the type of the MAGNETohydrodynamic spectrum of the solutions.
[abstract 46 / 65] (score: 2) - Title: Relativistic Simulations of Self-Gravitating Radiation FluidsAuthors: Bing-Jyun Tsao, Pablo Laguna, Octavio Guerrero,Comments: (10 pages, 4 figures)Subjects: gr-qc astro-ph.HE astro-ph.IMCreated: 2026-11-06; Updated: 2026-11-10; Datestamp: 2026-11-10
We present an approach for numerical simulations of pure radiation fluids within the general RELATIVISTIC hydrodynamics framework. The approach models radiation as a self-gravitating perfect fluid with vanishing rest mass, enabling simulations of radiation fluids in strong-gravity spacetimes. Building on the existing RELATIVISTIC hydrodynamics code Whisky, within the Einstein Toolkit framework, we introduce modifications to incorporate radiation fluids, including updates to the source terms, recovery scheme, and Riemann solvers. Modifications are validated using standard shock tube tests. We present results for radiation accretion onto a single BLACK HOLE, as well as a photon star solution for radiation in unstable hydrostatic equilibrium, demonstrating both collapse and dispersion under perturbations.
[abstract 47 / 65] (score: 2) - Title: Magnetosonic Solitons Driven by a Moving Charged Source: Two-Fluid Modeling and PIC ValidationAuthors: Prince Kumar, S. K. Mishra,Comments: 12 papges, 9 figuresSubjects: physics.plasm-ph physics.space-phCreated: 2026-11-07; Updated: 2026-11-10; Datestamp: 2026-11-10
We develop and validate a one-dimensional electron-ion two-fluid model, self-consistently coupled to Maxwell equations, for MAGNETosonic structures generated by a moving charged source. The model is independently benchmarked against kinetic particle-in-cell (PIC) simulations to assess its ability to reproduce electrostatic and electroMAGNETic responses. In the zero-MAGNETic-field limit, the electrostatic precursor structures are validated using the Korteweg--de Vries amplitude--width invariant. For a finite MAGNETic field, the frequency and propagation speed of the far wake are consistent with the low-frequency fast-MAGNETosonic branch, providing a linear benchmark for the electroMAGNETic response. The model reproduces the transition from a wake-dominated regime to localized forward precursors as the source velocity exceeds the MAGNETosonic speed, and to source-locked pinned structures at higher velocities. Independent PIC simulations recover the principal features of these regimes, supporting the validity of the two-fluid description for the parameters considered. By retaining separate electron and ion dynamics, electron inertia, and charge-separation effects, the validated model provides a framework for investigating source-driven plasma-wave structures across a broader range of plasma conditions and source-MAGNETic-field geometries, with potential applications to interpreting plasma-wave signatures associated with moving charged objects in space plasmas.
[abstract 48 / 65] (score: 2) - Title: Self-organization of MAGNETic islands and zonal MAGNETic fields driven by slab microtearing modes in the absence of MAGNETic shearAuthors: Mitsuyoshi Yagyu, Ryusuke Numata, Seiya Nishimura,Comments:Subjects: physics.plasm-ph nlin.PSCreated: 2026-11-07; Updated: 2026-11-10; Datestamp: 2026-11-10
Self-organization in collisional microtearing turbulence is investigated using gyrokinetic simulations in a slab geometry without equilibrium MAGNETic shear. Unlike MAGNETically driven conventional tearing instabilities, microtearing instabilities are driven by the electron temperature gradient. Electron temperature fluctuations are found to contain most of the gyrokinetic free energy. Although MAGNETic perturbations contribute little to the free energy, the MAGNETic field structure plays a crucial role in the nonlinear evolution of microtearing turbulence. Zonal MAGNETic fields emerge spontaneously through the nonlinear interaction between MAGNETic perturbations and electron temperature fluctuations. These zonal fields provide an effective MAGNETic shear that enables MAGNETic islands to form despite the absence of equilibrium MAGNETic shear. The electron temperature profile is flattened within the islands. This flattening reduces the instability drive and is expected to promote turbulence saturation.
[abstract 49 / 65] (score: 2) - Title: Effect of Turbulence and Inhomogeneities on the Propagation of Kinetic Scale WavesAuthors: Trevor A. Bowen,Comments:Subjects: physics.space-ph astro-ph.SR physics.plasm-phCreated: 2026-11-07; Updated: 2026-11-10; Datestamp: 2026-11-10
Context. ElectroMAGNETic ion-scale waves are well known to occur in the solar wind. Eikonal (WKB) like effects may play an important role in the interplay between the propagation and local kinetic plasma dynamics of ion cyclotron waves. Aims. This Letter aims to explore the interplay of ICW propagation with turbulence and local kinetic plasmas using ray tracing equations for ICWs in a moving medium, in which turbulent gradients are present. Methods. Parker Solar Probe observations of ICWs in the solar wind are studied using ray equations in a moving medium. Gradients in the dispersion relation responsible for WKB evolution of ICW are constrained and compared with a Parker spiral model. Results. The empirical gradients, which contain turbulent motions, greatly enhance the efficiency of WKB effects. However, the typical refraction rates are significantly slower than expected quasilinear evolution of the observed wave populations, which suggests that local kinetic physics dominates over nonlinear expansion effects. Conclusions. Turbulence can effectively increase WKB effects due to gradients caused by nonlinear interactions. In the solar wind these gradients are not sufficient to substantially change an individual ion-scale ICW over its lifetime. Incorporating kinetic effects of expansion may help advance the understanding of generation and absorption of ICW and their role in heating in the solar wind.
[abstract 50 / 65] (score: 2) - Title: Exact analytic anisotropic three-dimensional equilibria with nested MAGNETic surfaces, confined drift orbits and without spatial symmetryAuthors: A. Bhattacharjee, W. Sengupta, V. N. Duarte, L. Fu,Comments:Subjects: physics.plasm-phCreated: 2026-11-07; Updated: 2026-11-10; Datestamp: 2026-11-10
Exact toroidal fluid and kinetic equilibria with nested MAGNETic surfaces and no continuous symmetry are of great interest in laboratory, astrophysical and space plasmas. Their existence and stability have been open in physics and mathematics for decades. We construct such anisotropic-pressure equilibria by applying the Clemente transformation to exact vacuum fields. They connect smoothly to these fields on a fixed regular domain and preserve a regular MAGNETic axis, perfectly nested surfaces and spatially varying rotational transform. To our knowledge, the sheared configurations are the first exact anisotropic equilibria combining these properties with positive pressures and a positive firehose margin. The fixed-boundary Chew--Goldberger--Low (CGL) quadratic energy splits into a nonnegative vacuum-field term and a local pressure term, nonnegative for p_perp/p_parallel <= (3+\sqrt{21})/2 ~ 3.79. For p_parallel >= p_perp each configuration minimizes the finite-amplitude CGL energy over smooth boundary-fixed ideal material deformations. For the current-free configurations, physical guiding-center distributions produce these pressures within the same bound, with no free energy for MAGNETic-moment-conserving electrostatic perturbations. Trapped particles inherit the vacuum field's second adiabatic invariant at a rescaled MAGNETic moment, so local closed action contours carry over. The equilibrium code DESC reproduces them from the exact solution. Kinetic stability for surface-dependent rescalings and against general nonlinear electroMAGNETic perturbations remains open.
[abstract 51 / 65] (score: 2) - Title: Stellar Disruption and Black Hole Retention in Massive Collisions: The Role of Thermonuclear FeedbackAuthors: Hongxuan Jiang, Douglas N. C. Lin,Comments: 12 pages, 6 figures, to be submittedSubjects: astro-ph.SR astro-ph.GA astro-ph.HECreated: 2026-11-07; Updated: 2026-11-10; Datestamp: 2026-11-10
A stellar-mass BLACK HOLE (BH) that collides with a massive star can be captured by drag and settle at its center as a BLACK HOLE star. Hydrodynamic simulations that neglect nuclear reactions have found that the star survives and becomes a BLACK HOLE star (BH*) for BH-to-star mass ratios $q\lesssim0.2$. We perform hydrodynamic simulations of head-on collisions with the \athenak\ code, including CNO burning coupled to the gas, for $q=0.1$ and $0.2$ BHs, stellar masses of $100$ and $500\,M_{\odot}$, solar, metal-deficient, and Helium-rich compositions. In all models (with $q\le0.2$), the energy dissipated by drag is comparable to or less than the binding energy that the captured BH adds to the gas so that it alone does not disrupt the star. But, under compression around the captured BH, gas is heated to $\gtrsim2\times10^8$\,K and undergoes thermonuclear burning at the $β$-limited hot-CNO rate. Within about one dynamical time after the BH settles at the center, the nuclear energy released during the encounter becomes a significant fraction of the star's binding energy $\tfrac32\barβ\int P\,dV$. The star loses most of its mass once the cumulative release reaches this binding energy. Below this threshold, the release rate declines. Merger between a solar-composition star and a BH with a mass ratio $q=0.2$ leads to the disruption of the star after releasing most of its total mass. But a metal-poor star, with nearly the same binding energy and total yield, survives with minor release after merger with an identical BH. After coalescence with a less massive ($q=0.1$) BH, stars with both solar and metal-poor composition survive as BLACK HOLE stars, burning at a rate $\gtrsim 10^{44}\,{\rm erg\,s^{-1}}$, far from thermal equilibrium. Very massive and helium-rich stars, which are weakly bound, are the most easily disrupted.
[abstract 52 / 65] (score: 2) - Title: Analysis of Solid Boron Injection for ITERAuthors: Florian Effenberg, Joseph A. Snipes, Federico Nespoli, Robert Lunsford, Jonathan van Blarcum, Manni Jia, Heinke Frerichs, Alessandro Bortolon, Klaus Schmid, Tom Wauters,Comments:Subjects: physics.plasm-phCreated: 2026-11-08; Updated: 2026-11-10; Datestamp: 2026-11-10
Since ITER will now operate with a full tungsten divertor and first wall, the ITER Organization is considering boron wall conditioning schemes to getter oxygen and reduce tungsten sputtering to avoid excessive radiation to ensure that ITER can reach and sustain high- performance plasma operation. ITER has adopted Glow Discharge Boronization (GDB) in deuterated diborane (B$_2$D$_6$) as its main technique, which can only be performed in the absence of MAGNETic fields, but has also requested a study to determine how effective solid boron injection (SBI), which can be performed during plasma operation, using either an Impurity Powder Dropper (IPD) or a boron pellet injector, might be as a risk mitigation to achieving Q=10. Solid impurity injection has been used for decades as a wall conditioning technique on numerous tokamaks and stellarators around the world. The study presented here begins to assess SBI on ITER by first quantifying the boron source term across a particle size scan from 1 $μ$m to 5 mm diameter and an injection velocity scan from 5 -- 200 m/s for several ITER plasma conditions: 1) Start of Research Operations (SRO) diverted L-mode, 2) Q=10 H-mode, and 3) low plasma current and low power limiter operation. Modeling of the ablation, transport, erosion and redeposition of solid boron is being carried out with the Dust Injection Simulator (DIS), the Neutral Gas Shielding (NGS), EMC3-EIRENE and WallDYN3D models. In the first steps presented here, the DIS and NGS models are compared for calculating the boron source term that is then used as input to EMC3-EIRENE and will later be used with WallDYN3D.
[abstract 53 / 65] (score: 2) - Title: Regulating pedestal pressure profile by microtearing modes in the EAST tokamakAuthors: Jinze Shi, Youwen Sun, Kaixuan Fan, Tonghui Shi, Shifan Wang, Hailin Zhao, Qing Zang, Ziqiang Zhou, Hua Yang, Xuemin Wu, Jinyue Liu, Haoyu Nan, Qun Ma, Hui Sheng, Jinyi An, Jian Xu, Shuai Gu, Huihui Wang, Kaiyang He,Comments:Subjects: physics.plasm-phCreated: 2026-11-08; Updated: 2026-11-10; Datestamp: 2026-11-10
The pedestal pressure profile plays a critical role in determining the overall confinement of tokamak fusion plasmas. This letter reports the first evidence on regulating pedestal pressure profile by microtearing modes (MTMs) via limiting the pedestal gradient, which was thought to be limited by kinetic ballooning modes over the last decades. This is observed in an ITER-baseline-like target plasma in the EAST tokamak. MTMs arrest the recovery of pedestal electron temperature (and hence pressure) by clamping its gradient at a critical value while leaving the density profile essentially unaffected. Global fluid and local gyrokinetic simulations confirm the excitation of MTMs when the pedestal electron temperature gradient exceeds a threshold value in this experiment. This finding reveals MTMs as an alternative electroMAGNETic micro-instability that imposes an additional constraint in determining the pedestal structure in tokamaks.
[abstract 54 / 65] (score: 2) - Title: Directional asymmetry of atmospheric pole-to-pole teleconnectionAuthors: Yechul Shin, Jong-Seong Kug,Comments:Subjects: physics.ao-phCreated: 2026-11-08; Updated: 2026-11-10; Datestamp: 2026-11-10
Paleoclimate proxies show that abrupt Greenland changes were followed by Antarctic responses within decades, suggesting a fast atmospheric pole-to-pole teleconnection involving shifts in the Intertropical Convergence Zone (ITCZ) and reorganization of extratropical JETs. Here, we examine how the mean ITCZ position modulates this interhemispheric teleconnection. Using an aquaplanet slab-ocean model, we apply northern high-latitude forcing in climatologies with different mean ITCZ positions. The southern high-latitude response is about twice as large when the mean ITCZ is in the Southern Hemisphere. The teleconnection is therefore directionally asymmetric. The asymmetry arises in the subtropical JET response per degree of ITCZ shift, because, even with a comparable Hadley cell response, the angular momentum carried into the upper branch depends on the distance of the ITCZ from the equator, so that an ITCZ shift toward or away from the equator reinforces or offsets the JET response. Our results suggest that the southward-displaced glacial ITCZ made Arctic-to-Antarctic transmission more efficient than today, whereas the present-day ITCZ favors the reverse.
[abstract 55 / 65] (score: 2) - Title: Quasinormal modes of a scale-dependent BLACK HOLE in 5D spacetime with cosmological constantAuthors: Ángel Rincón, Zdeněk Stuchlík,Comments: 39 pages, 11 figures, 4 tables. Published in The European Physical Journal PlusSubjects: gr-qcCreated: 2026-11-08; Updated: 2026-11-10; Datestamp: 2026-11-10
In this paper, we investigate the quasinormal modes (QNMs) of a scale-dependent BLACK HOLE in five dimensions with a positive cosmological constant, considering i) scalar, ii) electroMAGNETic, and iii) Dirac perturbations. After deriving exact analytical solutions within the framework of scale-dependent gravity in five dimensions and selecting a different family of solutions (cf. \cite{Contreras:2019fwu}), we analyze the corresponding effective potentials (given by the lapse function) for each perturbation type. We employ a first-order approximation for the lapse function, as it closely matches the exact case for small $\varepsilon$. Since quantum corrections are expected to be small, our focus is on a relatively low range of the scale-dependent parameter $\varepsilon$. We confirm that the WKB semi-analytical approach can be used to compute the QNMs for these perturbations to the background geometry. We calculate the QNM frequencies for the classical case (for comparison) and for cases where the scale-dependent parameter $\varepsilon$, which quantifies deviations from General Relativity, is non-zero. The results are summarized in a series of tables and figures. Finally, we find that, regardless of the perturbation type, the solutions are stable, as the imaginary part of each QNM frequency is negative.
[abstract 56 / 65] (score: 2) - Title: Single and repetitive Penrose processes in genuine uncharged Kerr-Bertotti-Robinson BLACK HOLEAuthors: Ruo-Cen Wu, Hanjun Zou, Meng Xu, Yun-Long Zhang,Comments: 21 pages, 6 figuresSubjects: gr-qcCreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
We establish an analytical framework for the Penrose process in the genuine uncharged Kerr-Bertotti-Robinson (KBR0) black-hole spacetime within a Bertotti-Robinson (BR) electroMAGNETic vacuum, consistently linking particle decay, radial transport, thermodynamic states, and geometric reconstruction by distinguishing coordinate Killing energy from thermodynamic mass-generator energy and performing multibranch parameter mapping from thermodynamic states to background metric parameters. Furthermore, we present the analytical solution for the decay of equatorial massive neutral particles at a common radial turning point inside the ergoregion, the orbital accessibility criteria, and the six physical constraints required for a complete extraction event. Numerical calculations demonstrate that for both near-extremal and lower-spin inputs, in both single and repetitive Penrose processes, the net energy return on investment ($η_{\text{EROI}}$) and the rotational energy utilization efficiency ($η_{\text{EUE}}$) decrease with increasing external MAGNETic field, whereas the rotational energy reservoir consumption rate per unit incident energy ($η_{\text{thermo}}$) increases. For the inputs considered, the feasible domain and the upper bound of the initial MAGNETic field for single extraction are constrained by two boundary mechanisms: the obstruction of parent-particle infall and the loss of negative energy in the captured fragment. Finally, for repetitive extraction processes within the surveyed regime, all sequences terminate due to orbital accessibility obstructions, explicitly local-slope failure and far-field incident-branch closure, with the final black-hole state retaining most of its initial rotational energy reservoir. Moreover, the black-hole state evolves along a common integral curve independent of the parent particle's specific energy, which solely alters the sequence endpoint.
[abstract 57 / 65] (score: 2) - Title: Heterogeneous Acceleration of TRIMEG++ code using OpenMP for Gyrokinetic SimulationsAuthors: Nicola Noventa, Giorgio Daneri, Zhixin Lu, Matthias Hoelzl,Comments: 25 pages, 13 figures, 2 tablesSubjects: physics.plasm-phCreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
Turbulent transport largely determines the performance of MAGNETic-confinement fusion devices such as tokamaks, and gyrokinetic particle-in-cell (PIC) simulations are a principal tool to predict it. Advancing up to hundreds of millions of markers and solving large sparse field systems at every time step makes whole-device simulations among the most expensive in plasma physics. GPUs can accelerate this workload, but porting a complex code requires restructuring its parallelism and memory traffic, ideally without a separate version per vendor. In this work, the gyrokinetic code TRIMEG-C1, whose unstructured triangular mesh and high-order finite elements cover both the confined core and the open-field-line edge of the plasma, is rewritten in C++ as TRIMEG++ and fully offloaded to GPUs with OpenMP target directives, so that one portable code base runs on both AMD and NVIDIA hardware. The particle-to-grid projection is offloaded in its standard and field-aligned formulations, the PETSc-based field solver runs on the GPU through the library's backends, and, together with the previously offloaded particle pusher, every stage whose cost scales with the marker count runs on the GPU. All speedups are node-to-node comparisons against a 256-core CPU node (2x AMD EPYC 9754). On the TCV-X21 tokamak reference case, the offloaded kernels reproduce the CPU results to a relative accuracy of 1e-11, and the full simulation runs 4.1-6.1x faster on a node with two AMD MI300A and 2.1-3.0x faster on a node with four NVIDIA A100, with the speedup growing with problem size. The MI300A, with shared CPU-GPU memory, needs no explicit data transfers, whereas the A100 needs them managed by hand. These results show that directive-based offloading can accelerate a complex gyrokinetic code across GPU vendors, making whole-volume tokamak simulations with hundreds of millions of markers practical on a single GPU node.
[abstract 58 / 65] (score: 2) - Title: Measurement of the Neutrino Spectrum along the Galactic Plane with IceCubeAuthors: The IceCube Collaboration, R. Abbasi, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, S. Ali, N. M. Amin, K. Andeen, C. Argüelles, S. Athanasiadou, S. N. Axani, R. Babu, X. Bai, A. Balagopal V., S. W. Barwick, V. Basu, R. Bay, J. J. Beatty, J. Becker Tjus, J. Beise, C. Bellenghi, S. Benkel, S. BenZvi, D. Berley, E. Bernardini, D. Z. Besson, E. Blaufuss, L. Bloom, S. Blot, F. Bontempo, J. Y. Book Motzkin, C. Boscolo Meneguolo, S. Böser, O. Botner, J. Braun, B. Brinson, Z. Brisson-Tsavoussis, L. Brusa, A. Burgos Mondéjar, R. T. Burley, D. Butterfield, K. Carloni, J. Carpio, N. Chau, Y. C. Chen, Z. Chen, D. Chirkin, S. Choi, A. Chubarov, B. A. Clark, D. A. Coloma Borja, A. Connolly, J. M. Conrad, D. F. Cowen, C. De Clercq, J. J. DeLaunay, D. Delgado, T. Delmeulle, S. Deng, P. Desiati, K. D. de Vries, G. de Wasseige, T. DeYoung, J. C. Díaz-Vélez, S. DiKerby, T. Ding, M. Dittmer, A. Domi, L. Draper, L. Dueser, D. Durnford, K. Dutta, M. A. DuVernois, T. Ehrhardt, L. Eidenschink, A. Eimer, C. Eldridge, P. Eller, E. Ellinger, D. Elsässer, R. Engel, H. Erpenbeck, W. Esmail, S. Eulig, J. Evans, P. A. Evenson, K. L. Fan, K. Fang, A. Fattorini, A. R. Fazely, A. Fedynitch, N. Feigl, C. Finley, D. Fox, A. Franckowiak, S. Fukami, P. Fürst, J. Gallagher, A. Garcia, M. Garcia, E. Genton, L. Gerhardt, A. Ghadimi, C. Glaser, T. Glüsenkamp, J. G. Gonzalez, S. Goswami, A. Granados, D. Grant, S. J. Gray, S. Griffin, S. Griswold, K. M. Groth, D. Guevel, C. Günther, P. Gutjahr, C. Ha, A. Hallgren, F. Halzen, M. Handt, K. Hanson, J. Hardin, A. A. Harnisch, P. Hatch, A. Haungs, J. Häußler, K. Helbing, J. Hellrung, B. Henke, L. Hennig, F. Henningsen, G. Herrera, L. Heuermann, R. Hewett, N. Heyer, S. Hickford, A. Hidvegi, C. Hill, G. C. Hill, R. Hmaid, K. D. Hoffman, A. Hollnagel, D. Hooper, S. Hori, K. Hoshina, M. Hostert, W. Hou, M. Hrywniak, T. Huber, K. Hultqvist, M. Hünnefeld, K. Hymon, A. Ishihara, W. Iwakiri, M. Jacquart, S. Jain, O. Janik, M. Jansson, M. Jin, N. Kamp, D. Kang, W. Kang, A. Kappes, T. Karg, A. Karle, A. Kastanas, A. Katil, M. Kauer, J. L. Kelley, B. Kern, M. Khanal, A. Khatee Zathul, A. Kheirandish, T. Kim, H. Kimku, F. Kirchner, J. Kiryluk, C. Klein, S. R. Klein, Y. Kobayashi, S. Koch, A. Kochocki, R. Koirala, H. Kolanoski, T. Kontrimas, L. Köpke, C. Kopper, D. J. Koskinen, P. Koundal, M. Kowalski, A. Kravka, N. Krieger, T. Krishnan, K. Kruiswijk, E. Krupczak, E. Kun, N. Kurahashi, C. Lagunas Gualda, L. Lallement Arnaud, M. J. Larson, F. Lauber, J. P. Lazar, K. Leonard DeHolton, A. Leszczyńska, C. Li, J. Liao, C. Lin, Q. R. Liu, Y. T. Liu, M. Liubarska, C. Love, L. Lu, F. Lucarelli, Lukas Liland, W. Luszczak, Y. Lyu, M. Macdonald, F. Machingal, E. Magnus, Y. Makino, E. Manao, S. Mancina, A. Mand, I. C. Mariş, S. Marka, Z. Marka, I. Martinez-Soler, R. Maruyama, J. Mauro, F. Mayhew, F. McNally, K. Meagher, A. Medina, M. Meier, Y. Merckx, L. Merten, J. M. Mitchell, N. Moller, S. Mondal, T. Montaruli, R. W. Moore, A. Mosbrugger, D. Mousadi, E. Moyaux, T. Mukherjee, M. Nakos, U. Naumann, R. Neshat, L. Neste, M. Neumann, M. U. Nisa, K. Noda, A. Noell, A. Novikov, A. Obertacke, V. O'Dell, A. Olivas, R. Orsoe, J. Osborn, E. O'Sullivan, B. Owens, V. Palusova, H. Pandya, A. Parenti, C. Parisel, N. Park, V. Parrish, E. N. Paudel, L. Paul, C. Pérez de los Heros, T. Pernice, T. C. Petersen, J. Peterson, S. Pick, M. Plum, A. Pontén, V. Poojyam, B. Pries, R. Procter-Murphy, G. T. Przybylski, L. Pyras, C. Raab, J. Rack-Helleis, N. Rad, M. Ravn, K. Rawlins, Z. Rechav, A. Rehman, I. Reistroffer, E. Resconi, C. D. Rho, W. Rhode, L. Ricca, B. Riedel, A. Rifaie, E. J. Roberts, S. Rodan, M. Rongen, A. Rosted, C. Rott, T. Ruhe, L. Ruohan, D. Ryckbosch, J. Saffer, D. Salazar-Gallegos, P. Sampathkumar, A. Sandrock, G. Sanger-Johnson, M. Santander, S. Sarkar, M. Scarnera, M. Schaufel, H. Schieler, S. Schindler, L. Schlickmann, B. Schlüter, F. Schlüter, N. Schmeisser, T. Schmidt, F. Schmitt, A. Scholz, F. G. Schröder, S. Schwirn, S. Sclafani, D. Seckel, L. Seen, M. Seikh, S. Seunarine, P. A. Sevle Myhr, R. Shah, S. Shah, A. Sharma, S. Shefali, N. Shimizu, M. Shin, R. Singh, B. Skrzypek, R. Snihur, D. Soldin, P. Soldin, G. Sommani, D. Song, C. Spannfellner, G. M. Spiczak, C. Spiering, J. Stachurska, M. Stamatikos, T. Stanev, T. Stezelberger, T. Stürwald, T. Stuttard, G. W. Sullivan, I. Taboada, S. Ter-Antonyan, A. Terliuk, A. Thakuri, P. Thelen, M. Thiesmeyer, W. G. Thompson, J. Thwaites, W. Tian, S. Tilav, K. Tollefson, J. A. Torres, S. Toscano, D. Tosi, K. Upshaw, A. Vaidyanathan, N. Valtonen-Mattila, J. Valverde, J. Vandenbroucke, T. Van Eeden, N. van Eijndhoven, L. Van Rootselaar, J. van Santen, J. Vara, F. Varsi, M. Velazquez, M. Venugopal, M. Vereecken, S. Vergara Carrasco, S. Verpoest, A. Vijai, J. Villarreal, C. Walck, A. Wang, E. H. S. Warrick, C. Weaver, P. Weigel, A. Weindl, J. Weldert, A. Y. Wen, C. Wendt, J. Werthebach, M. Weyrauch, N. Whitehorn, C. H. Wiebusch, D. R. Williams, L. Witthaus, J. Woodward, G. Wrede, X. W. Xu, J. P. Yanez, Y. Yao, E. Yildizci, S. Yoshida, F. Yu, S. Yu, T. Yuan, S. Yun-Cárcamo, A. Zander Jurowitzki, A. Zegarelli, S. Zhang, Z. Zhang, P. Zhelnin, P. Zilberman, C. Zilleruelo Cañas, M. Zimmermann,Comments: 13 pages, 7 figures, 2 tablesSubjects: astro-ph.HE astro-ph.GACreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
We present the first measurement of the variation of the high-energy neutrino flux along the Galactic plane using 10 years of neutrino-induced particle-shower data from the IceCube Neutrino Observatory. In this Letter, we fit both the neutrino flux normalization and the spectral index, in multiple regions along the plane, independent of model expectations. The neutrino flux per solid angle in the inner Galactic region ($\vert l\vert< 30^{\circ}, \vert b\vert < 8^{\circ}$) is approximately five times higher than in the outer Galactic plane ($\vert l\vert>60^{\circ}, \vert b\vert < 8^{\circ}$) at $E_ν=5\mathrm{TeV}$. The spectral indices in the inner and outer region are $γ=2.76^{+0.18}_{-0.15}$ and $γ= 3.13^{+0.57}_{-0.37}$, respectively. Additionally, we compare the same region of Galactic emission measured in $\mathrm{TeV}$ gamma rays by LHAASO ($15^{\circ}
[abstract 59 / 65] (score: 2) - Title: Zeeman-Doppler imaging of early-type stars. Testing Stokes parameter inversions with theoretical MAGNETohydrodynamic modelsAuthors: O. Kochukhov, A. Al Kanale, J. Braithwaite,Comments: 17 pages, 11 figures; accepted for publication in Astronomy & AstrophysicsSubjects: astro-ph.SRCreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
Zeeman-Doppler imaging (ZDI) is widely used to reconstruct MAGNETic fields in early-type stars from time-series spectropolarimetric observations, yet its accuracy has not been systematically validated against physically self-consistent, complex MAGNETic field models. We aim to assess the reliability and limitations of modern ZDI techniques applied to fossil fields of early-type stars. We generated synthetic spectropolarimetric data from three-dimensional MAGNETohydrodynamic (MHD) simulations of fossil MAGNETic fields. The resulting Stokes profiles - individual lines and least-squares deconvolved (LSD) profiles - were inverted with contemporary ZDI codes using Stokes IQUV and IV data. We compared the reconstructed maps with the input MHD surface fields and quantified deviations in field strength, vector orientation, and harmonic energy decomposition. For Stokes IQUV inversions, ZDI recovers field vector components and strength with better than 10% accuracy, while Stokes IV inversions degrade to 15-20% for the most complex geometries. The field inclination is recovered to within 10 deg, with errors increasing to 15-20 deg in the same cases. Full Stokes inversions reproduce poloidal and toroidal energies to within a few percentage points. LSD-based inversions yield accuracy comparable to, and sometimes better than, that achieved with ZDI using individual Fe II lines. Imposing a current-free poloidal constraint, which the input field satisfies, only helps where the unconstrained Stokes IV inversion performs poorly. Cross-talk between MAGNETic and abundance reconstructions is weak, with spurious inhomogeneities at or below 0.1 dex on average. Modern ZDI robustly reconstructs fossil MAGNETic fields in early-type stars, including their smaller-scale non-dipolar features, particularly when full Stokes information is available.
[abstract 60 / 65] (score: 2) - Title: Magnetized plasma modulator for POLARIZATION-tunable ultrahigh-power single-cycle LASERsAuthors: Li-Jia Shuai, Xing-Long Zhu, Zheng-Ming Sheng,Comments:Subjects: physics.plasm-phCreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
Ultrahigh power LASERs with tunable POLARIZATION and few-cycle duration have long been considered the holy grail of high-power LASER science, as they push light-matter interactions into an entirely new physical regime. Yet such pulses remain far beyond the reach of conventional solid-state optics and technologies. Here, we introduce a novel MAGNETized plasma modulator that boosts linearly polarized LASERs from petawatt to exawatt powers while simultaneously enabling tunable POLARIZATION, offering a promising approach for high-power LASER development. This is achieved in density-tailored plasmas by combining dispersive compression of a chirped picosecond LASER pulse with MAGNETo-chiral group-velocity splitting in a few-Tesla MAGNETic field. It can generate circularly or elliptically polarized pulses with extremely high compression ratios (over 1000) and extremely short durations (down to the single-cycle level) in a compact and efficient manner. These findings demonstrate a feasible pathway toward exawatt-class few-cycle LASERs with tunable POLARIZATION, opening new avenues for a wide range of cutting-edge research and applications.
[abstract 61 / 65] (score: 2) - Title: Revisiting the Einstein Cross with X-shooter spectra: New estimates of accretion disk parameters and broad emission line profiles from microlensingAuthors: R. Jerez-Nicurcar, A. Esteban-Gutiérrez, V. Motta, E. Mediavilla,Comments: 13 pages, 9 figures, 3 tables, 1 table appendixSubjects: astro-ph.GACreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
We present a spectroscopic study of the lensed QUASAR Q2237+0305, the Einstein Cross, assessing the best wavelength coverage to date with the X-shooter instrument (from $3000$ to $20000$ $\mathring{A}$), and thus improving the available spectroscopic data for this system. Using as a reference the characteristic emission lines for each QUASAR macro-image, we estimate the chromatic microlensing effect between pairs of images and calculate the extinction curve, confirming no significant differences between spectra $C$ and $A$ caused by extinction in the lens galaxy. In addition, we model the accretion disk characterized by a temperature profile with logarithmic slope $1/p$ and size $r_{s}$, assuming a thin-disk model with a power-law function of the form $r_{s}$ $\propto$ $λ^{p}$. To do this, we calculated a set of three chromatic microlensing measurements compiling previous estimates from the literature to test the wavelength dependence. This temperature profile was also compared to the canonical thin-disk model with $p=4/3$. Finally, we estimated the likelihood between the disk model and the observed data collected from multiple epochs through mock microlensing magnification maps and determined the probability density functions of each parameter from a Bayesian analysis. As a result, our estimated values for the accretion disk size and its exponential index are $r_{s}=4.9^{+2.3}_{-2.6}$ $\sqrt{M/0.3M_{\odot}}$ (lt-day) and $p=0.77^{+0.47}_{-0.28}$, respectively, reinforcing a departure from the standard accretion disk model ($ T \propto r_s^{-3/4}$).
[abstract 62 / 65] (score: 2) - Title: Efficient high-order Discontinuous Galerkin simulations of multi-species high-enthalpy flowsAuthors: Beatriz Fagá, Georgii Oblapenko, Yiyang Zhu, Daniel Doehring, Manuel Torrilhon,Comments:Subjects: physics.flu-dyn cs.NA math.NACreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
Numerical simulation of hypersonic vehicles is an attractive approach to investigate the complex phenomena involved in such technologies. For this, second-order finite volume methods (FVM) are the established method in computational fluid dynamics, with the cost of high dissipation in affordable meshes, thus needing refined ones or adaptive mesh refinements techniques to obtain accurate results. An alternative is to make use of high-order discontinuous Galerkin methods, in particular discontinuous Galerkin spectral element method (DGSEM), once it achieves higher formal order of accuracy on element-local polynomial bases. Therefore the goal of this work is to present the numerical simulations of a two-dimensional scramJET configuration to test and verify the applicability of the DGSEM approach for a complex hypersonic flow where shock-shock interactions occur. Results revealed to be in agreement with reference FVM solvers, thus verifying the code implementation.
[abstract 63 / 65] (score: 2) - Title: Dynamics of singular-JET formation during the collapse of drop-impact cratersAuthors: Nivesh Mishra, Anikesh Pal,Comments:Subjects: physics.flu-dynCreated: 2026-11-05; Updated: 2026-11-10; Datestamp: 2026-11-10
The collapse of a drop-impact crater that bypasses the pinch-off singularity produces exceptionally thin, high-velocity JETs, often referred to as singular-JETs. We perform 2D axisymmetric DNS using Basilisk, employing adaptive mesh refinement to capture the intricate flow features. The numerical results for a drop diameter of $3.64$ mm at ambient pressure match the experiments well under different impact conditions. During the crater collapse, qualitatively different dimple shapes form, including an entrapped bubble beneath the dimple. Quantitatively, an entrapped bubble with a diameter of ~210 μm and a JET velocity of 61.7 m/s for the singular-JET case during cylindrical dimple collapse is obtained from simulations. Subtle morphological changes in crater evolution distinguish the JETting regime, with a critical angle of 109.2 between the crater side wall and its base in the singular-JET case. The simulation provides insight into the internal flow fields, enabling us to delineate the observed phenomenon. The pressure and velocity fields reveal that the high JETting velocity is associated with the formation and rapid collapse of a nearly cylindrical dimple. The resulting pressure distribution drives a strongly upward flow near the dimple base, while the nearly parallel dimple side walls redirect radial liquid motion towards the axis. We extend the simulations into the post-entrainment region and identify another singular-JET near the upper boundary of the entrainment region. The JET reaches a velocity of 63.93 m/s and exhibits morphological characteristics similar to the first singular-JET case. A regime map is constructed from simulations spanning Weber numbers ranging from 100 to 200 and Froude numbers from 45 to 92; the updated lower and upper boundaries for the entrainment region, based on singular-JET formation, are We = 45.5\, Fr^{0.237} and We = 53.5\, Fr^{0.251}, respectively.
[abstract 64 / 65] (score: 2) - Title: Three-dimensional radiative transfer modeling of the scattering POLARIZATION in the solar H$α$ lineAuthors: Jaume Jaume Bestard, Jiri Stepan, Javier Trujillo Bueno,Comments: 12 pages, 11 figures, accepted for publication in A&ASubjects: astro-ph.SRCreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
The H$α$ line probes the solar chromosphere, but its scattering POLARIZATION is difficult to interpret because of MAGNETic fields, plasma motions, and atmospheric 3D inhomogeneities. We investigate its intensity and linear POLARIZATION in a 3D MAGNETohydrodynamic solar-atmosphere model including nonequilibrium hydrogen ionization. Using PORTA, we solve the full 3D non-LTE polarized radiative transfer problem for a multilevel hydrogen atom, accounting for atomic POLARIZATION, Hanle dePOLARIZATION, horizontal radiative transfer, and macroscopic velocities. We degrade synthetic Stokes profiles to the spatial, spectral, and polarimetric resolution of ZIMPOL observations for direct comparison. The modeled center-to-limb variation follows the observed trend, with comparable POLARIZATION amplitudes. The profiles show large spatial variability from symmetry breaking by horizontal inhomogeneities and atmospheric dynamics, as well as diverse line-core asymmetries. Classifying $Q/I$ profiles by asymmetry reveals a statistical correlation between profile morphology and MAGNETic-field strength in the H$α$ formation region, consistent with Hanle dePOLARIZATION: multi-peaked profiles favor stronger fields, whereas asymmetric single-peaked profiles favor weaker fields with smaller vertical strength variations. Thus, H$α$ scattering POLARIZATION reflects the interplay of MAGNETic fields, velocity gradients, and 3D radiative transfer. Our results highlight the need for 3D modeling to interpret H$α$ spectropolarimetry and its potential to diagnose chromospheric MAGNETism and dynamics.
[abstract 65 / 65] (score: 2) - Title: CoilStellaration: A Dataset and Benchmark for Engineering-Aware Stellarator Coilset GenerationAuthors: Jan-Hendrik Ewers, Santiago A. Cadena, Nicolò Foppiani, Andrea Merlo,Comments: 40th Conference on Neural Information Processing Systems (NeurIPS 2026). Track on Evaluations and DatasetsSubjects: cs.LG physics.plasm-phCreated: 2026-11-09; Updated: 2026-11-10; Datestamp: 2026-11-10
Stellarators are fusion devices that use externally generated, three-dimensional MAGNETic fields to confine hot plasma and offer a promising route to commercial fusion. Their electroMAGNETic coils pose a challenging design problem: they must reproduce the target MAGNETic field while satisfying engineering constraints and remaining practical and cost-effective to manufacture. Finding suitable geometries is a highly nonlinear inverse problem that generally has neither a closed-form nor a unique solution. This problem lies at the heart of stellarator design. We introduce CoilStellaration, a dataset and benchmark for learning the mapping between coil geometries from target plasma MAGNETic fields and engineering requirements. The dataset contains 177,000 optimized filamentary coilsets targeting plasma equilibria from ConStellaration, with sampled engineering requirements and achieved geometric and MAGNETic-field metrics. It spans multiple coil counts and field-period numbers, supporting studies of both specialized and shared models across configurations. The benchmark asks models to predict coils conditioned on a target equilibrium and requirements on coil-coil and coil-plasma spacing, curvature, and MAGNETic-field error. We show that MAGNETic-field accuracy remains the main challenge, with learned models rarely satisfying all requirements simultaneously. However, using learned predictions to initialize conventional coil optimization can accelerate early progress. We release baseline models and evaluation code to support reproducible research on both direct coil generation and learned optimization initializations. By lowering the barrier for machine learning and optimization researchers to engage with stellarator coil design, we aim to accelerate progress toward practical, cost-effective stellarator power plants.
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