Current date: 2026-10-09
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Scoring abstracts
Number of records retrieved: 899
Keyword score statistics
score 8 -- 2 abstracts
score 7 -- 2 abstracts
score 6 -- 4 abstracts
score 5 -- 1 abstracts
score 4 -- 5 abstracts
score 3 -- 11 abstracts
score 2 -- 29 abstracts
in total -- 54 abstracts
Articles that appeared on 2026-10-09
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[abstract 1 / 54] Wow! (score: 8)
- Title: Collisionless Accretion of Finite-Angular-Momentum Plasma onto a Spinning Black HoleAuthors: John M. Mehlhaff, Alexander Y. Chen, Martin Luepker, Yajie Yuan,Comments: 11 pages, 4 figures, comments welcome!Subjects: astro-ph.HECreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
In low-luminosity ACTIVE GALACTIC NUCLEi like M87* and Sgr A*, the accretion disk around the central supermassive BLACK HOLE is tenuous and collisionless. As a result, the usual ideal MAGNETohydrodynamics (MHD) approximation may not be applicable. In this Letter, we report on the first fully kinetic simulations of the accretion process where the plasma initially has finite angular momentum, focusing on the case of axisymmetry. The simulated accretion flow behaves remarkably similarly to the MAGNETically arrested disk (MAD) regime of ideal MHD, reproducing episodes of MAGNETic flux saturation and eruption typical of MADs. The resemblance to fluid models owes largely to kinetic instabilities, which regulate pressure anisotropy in the disk, allowing fluid terms to dominate the angular momentum transfer. In addition, by handling vacuum regions effectively, our kinetic approach probes the matter supply to the JET funnel. We observe no efficient penetration of the accreting material into this region, suggesting that a pair discharge may be required to sustain the Blandford-Znajek process. These initial findings represent important groundwork to be checked and built upon by future kinetic accretion simulations, especially in 3D.
[abstract 2 / 54] Wow! (score: 8) - Title: A morphological search for stable year-scale modulation in gamma-ray BLAZARsAuthors: Adithiya Dinesh, Alberto Domínguez, Alba Rico, Pablo Peñil, Marco Ajello, Sara Buson,Comments:Subjects: astro-ph.HECreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
Year-scale quasi-periodic oscillations (QPOs) in BLAZAR gamma-ray light curves have been proposed as signatures of supermassive binary BLACK HOLEs and precessing JETs. Red noise can mimic periodicity, and detection alone does not establish persistence or period stability. We develop and calibrate a morphological framework to characterize year-scale modulation and constrain the incidence of stable modulation in BLAZARs. We analyze 120 FERMI-LAT light curves spanning 18.1 yr. Singular spectrum analysis selects the oscillatory mode and period, while weighted wavelet Z-transform ridge tracking measures persistence, period drift, and cycle-to-cycle volatility. Flux randomization, 10,000 red-noise simulations, and about 20,000 injections calibrate the classification. Of 97 quality-selected sources, two show persistent, coherent modulation consistent with a stationary period (Rank I: PG 1553+113 and B2 1215+30), six show coherent modulation whose stationarity cannot be established (Rank II), and 89 form Rank III. Neither Rank I nor Rank II significantly exceeds red-noise expectations. Stationary 1-3 yr injections reach Rank I in 63-97% of trials at signal-to-noise ratio (SNR) = 1, depending on period, and 100% at SNR = 2; 92% of drifting injections reach Rank II. These results limit stable, approximately sinusoidal 1-3 yr modulation to at most 7% of the sample at SNR >= 1 and 5% at SNR >= 2 (95% confidence). PG 1553+113 has the lowest false-alarm probability, 4.7% after trials. Stable year-scale modulation is uncommon, and no source is established as periodic. The framework distinguishes persistent, stationary modulation from coherent variability whose period may evolve or fluctuate, but not the physical mechanism. PG 1553+113 and B2 1215+30 are candidates for monitoring and continuous gravitational-wave searches, although their stability does not establish a binary origin.
[abstract 3 / 54] Wow! (score: 7) - Title: Widespread steep X-ray spectra of luminous $z\simeq5.85-7.5$ QUASARs and their implications for future X-ray surveysAuthors: A. Tortosa, L. Zappacosta, E. Piconcelli, I. Saccheo, G. Lanzuisi, E. Bertola, F. Vito, M. Bischetti, M. Brazzini, M. Castellano, S. Carniani, A. Comastri, S. Gallerani, R. Gilli, F. La Franca, P. Madau, R. Maiolino, G. Miniutti, B. Musiimenta, C. Piscitelli, F. Salvestrini, F. Tombesi, R. Tripodi, C. Vignali, M. Volonteri, A. Bongiorno, L. Borrelli, M. Brusa, I. V. Chilingaria, F. Civano, S. Cristiani, V. D'Odorico, D. De Cicco, C. Done, M. Elvis, X. Fan, C. Feruglio, F. Fiore, A. Grazian, M. Guainazzi, F. Haardt, A. Luminari, N. Menci, R. Middei, F. Nicastro, M. Paolillo, M. Perna, S. Puccetti, R. Schneider, V. Testa, R. Valiante, L. Vallini, E. Vanzella, G. Vietri,Comments: Revised version submitted to A&ASubjects: astro-ph.HE astro-ph.GACreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
Luminous QUASARs (QSOs) at the Epoch of Reionization (EoR, $z\gtrsim6$) host billion-solar-mass BLACK HOLEs assembled within the first Gyr of cosmic time. Their X-ray emission probes the innermost accreting regions and constrains the physical state of the corona during early supermassive BLACK HOLE (SMBH) growth. Previous results from the HYPerluminous QUASARs at the Epoch of ReionizatION (HYPERION) sample of $z \gtrsim 6$ QSOs, powered by the most rapidly accreted SMBHs, suggested a link between X-ray spectral slope and long-term growth efficiency. We test whether the steep X-ray spectra of luminous z>6 QSOs are a general property of early SMBH growth or a peculiarity of the most efficiently grown SMBHs, using a sample extended mainly to the lowest growth efficiencies. We analysed the largest and most X-ray sensitive sample of 28 luminous QSOs at $z \simeq 5.85-7.56$ (26 used in the correlation analysis), combining HYPERION targets, luminous non-HYPERION sources, and QSOs powered by moderately accreting SMBHs newly observed in our XMM-Newton Large Programme. We re-derived BLACK HOLE masses and growth indicators for the entire sample homogeneously, incorporating the latest JWST-based spectroscopic measurements to ensure the most consistent and high-quality characterization across all targets. We found no statistically significant correlation between coronal spectral parameters and BH growth indicators: luminous $z \gtrsim 6$ QSOs systematically show steep X-ray continua, with high photon indices and/or low high-energy cutoffs, consistent with cold coronae, possibly linked to rapid accretion. Finally, if steep X-ray slopes are common among early AGN, they may significantly reduce count rates, at fixed intrinsic luminosity, in future surveys of the EoR, affecting the detectability of steep-spectrum X-ray sources and thus the census of the early AGN population.
[abstract 4 / 54] Wow! (score: 7) - Title: Accreting Neutron Stars in Low-Mass X-ray BinariesAuthors: M. C. Baglio, S. E. Motta, A. P. Nitindala, J. Poutanen,Comments: 37 pages, 10 Figures. Accepted for publication in SSRvSubjects: astro-ph.HE astro-ph.SRCreated: 2026-10-07; Updated: 2026-10-09; Datestamp: 2026-10-09
Neutron star low-mass X-ray binaries (NS LMXBs) are systems in which a neutron star accretes matter from a Roche-lobe-filling companion via an accretion disc, releasing gravitational energy with an efficiency of order 10-20% of the rest-mass energy. Unlike BLACK HOLEs, neutron stars possess a solid surface and a MAGNETic field, making NS LMXBs uniquely rich laboratories for high-energy astrophysics and dense-matter physics. In this chapter we review the current understanding of accretion onto neutron stars in LMXBs, tracing matter from the outer disc radii to the stellar surface across five decades of observational discovery. We survey the principal classes of accreting neutron star systems - canonical atoll and Z-sources, ultracompact X-ray binaries, accreting millisecond pulsars, and transitional millisecond pulsars - and discuss how their spectral states, timing properties, and multiwavelength behaviour encode the physics of the inner accretion flow. We examine thermonuclear Type-I X-ray bursts as probes of nuclear burning and neutron star structure, and review the boundary and spreading layers where accreted matter decelerates onto the stellar surface. We discuss RELATIVISTIC JETs and ionised disc winds as regulators of the accretion-ejection cycle. Finally, we present X-ray polarimetric results from the Imaging X-ray Polarimetry Explorer (IXPE), which for the first time provide new, though model-dependent, constraints on the geometry of the emission regions - disc, corona, spreading layer, and JETs - that spectroscopy alone cannot resolve, alongside complementary optical and infrared polarimetric observations.
[abstract 5 / 54] Yes (score: 6) - Title: PEARLS: NUSTAR and XMM-Newton Extragalactic Survey of the JWST North Ecliptic Pole Time-Domain Field V: Unraveling X-ray Spectral VariabilityAuthors: Samantha Creech, Francesca Civano, Daniel Wik, Núria Torres-Alba, Ross Silver, Xiurui Zhao, Tonima Ananna, Gibson Bowling, Norman A. Grogin, Anton M. Koekemoer, Peter Maksym, Sylvia Mesicek, Rafael Ortiz, Payaswini Saikia, Steven Willner, Rogier Windhorst,Comments: 36 pages, 13 figures; accepted by ApJSubjects: astro-ph.HECreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
As one of the first deep time-domain surveys in the hard X-ray band, the NUSTAR campaign in the JWST North Ecliptic Pole Time Domain Field (NEP-TDF) offers a prime opportunity to measure variability in a faint population of Active Galactic Nuclei (AGN) in the medium-to-high redshift universe. In the X-ray band, AGN variability is generally caused by changes in the brightness of the corona ($F_{int}$ variability) or changes in the column density of obscuring material near the SMBH ($N_H$ variability). Broad-band spectroscopy ($\sim$0.5-24 keV) is required to reliably disentangle these two phenomena. With simultaneous NUSTAR and XMM-Newton coverage---as well as 1.8 Ms of Chandra monitoring---the X-ray surveys in the NEP-TDF are ideally situated for this purpose. This work presents the first spectral modeling of the 52 NUSTAR-identified sources discovered in the latter half of the campaign, as well as a spectroscopic variability study of the entire 112-source NUSTAR NEP-TDF catalog. Seven variable candidates are identified. We find that $\gtrsim 1000$ total counts split across many ($\gtrsim 10$) epochs are needed in order to detect variability. Additionally, variable sources are compared to the survey sensitivity in order to inform population synthesis models of how variations can affect the detectability of faint AGN, which dominate the SMBH accretion history. Lastly, the timescale of $N_H$ variability is investigated as a probe for the obscurer location. Significant variability is slightly more common on $> 100$ day timescales, suggesting that the torus may have only slight dominance in driving $N_H$ variability in faint AGN.
[abstract 6 / 54] Yes (score: 6) - Title: Wind-Fed Magnetic Flux and the Emergence of X-ray Coronae in Active Galactic NucleiAuthors: Rostom Mbarek,Comments: Under ReviewSubjects: astro-ph.HECreated: 2026-10-07; Updated: 2026-10-09; Datestamp: 2026-10-09
We propose a scenario for the onset of radiatively efficient Active Galactic Nuclei (AGN) in which circumnuclear stellar and SUPERNOVA-driven winds supply mass and partially ordered MAGNETic flux to a compact disk reservoir around a supermassive BLACK HOLE. A coherent poloidal component surviving advection to small radii strengthens inward, lowering the gas plasma beta until mean Maxwell stresses overtake MRI turbulence, compress the disk vertically, and open a MAGNETically dominated wedge above it. Within a quasi-force-free description of this wedge, the field self-organizes toward a critical twist at which the net radial transport changes sign, defining a MAGNETic saturation radius $r_c\sim10\,r_g$. The MAGNETic squeezing of the disk fixes the pressure balance at the interface between the disk and wedge, confining the accumulated flux at $r_c$: flux advected toward this boundary is preferentially shed, fixing $B_r\propto r^{-2}$ in the interior. From the field topology alone we then derive a normalized saturation flux $ϕ\sim 50$, consistent with the MAD plateau of GRMHD simulations. The resulting compact, time-dependent saturation region is a natural candidate for the AGN X-ray corona, being collisionless, MAGNETized, and, at high compactness, plausibly pair-rich, with hadronic pair injection providing a conditional additional channel. Its size, variability, and spectral hardness are controlled by $r_c$, the compactness, and the MAGNETization. We connect these scalings to observed coronal sizes, variability, and the power partition between the corona and JET. We further propose that Little Red and Blue Dots could represent a disk-reservoir phase preceding luminous AGN activity.
[abstract 7 / 54] Yes (score: 6) - Title: From GeV to PeV: Orbital Modulation and Wind-Regulated Ultrahigh-energy Emission in Cygnus~X-3Authors: Su-Yu Wan, Ruo-Yu Liu, Xing-Fu Zhang, Dmitriy Khangulyan,Comments: 8 pages, 3 figures, 1 table, including appendixSubjects: astro-ph.HECreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
Recent LHAASO observations reveal ultrahigh-energy (UHE) gamma-ray emission from Cygnus~X-3 with evidence for orbital modulation, providing a rare opportunity to study particle acceleration and transport on binary scales. We develop a common binary--JET model that jointly explains the contemporaneous GeV--PeV spectra and orbital light curves. The GeV emission is produced by anisotropic inverse-Compton scattering of stellar photons by RELATIVISTIC electrons, while multi-PeV protons escaping from the inner region produce TeV--PeV gamma rays through photohadronic and hadronuclear interactions. The GeV orbital modulation constrains the binary--JET geometry, allowing the UHE observations to probe the escaping proton population and its interaction with the circum-binary environment. We find that the UHE emission is strongly regulated by the accretion-driven wind structure. In the present state, a fast disk wind displaces much of the denser Wolf--Rayet (WR) wind from the escaping-proton trajectories, suppressing hadronuclear emission. Changes in the strength, collimation, or orientation of the disk wind can expose the escaping protons to a much denser WR wind and enhance the PeV gamma-ray luminosity by orders of magnitude. This provides a possible connection to the much brighter, though unconfirmed, PeV activity reported in the 1980s, and links UHE gamma-ray activity to the accretion and outflow state of the binary.
[abstract 8 / 54] Yes (score: 6) - Title: Magnetic flux cancellation in a 3D MAGNETohydrodynamic simulation of an emerging flux tube with a non-uniform twistAuthors: V. Agalianou, S. Patsourakos, V. Archontis,Comments: 15 pages, 15 figures, accepted for publication in Astronomy & AstrophysicsSubjects: astro-ph.SRCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
Flux emergence is often accompanied by flux cancellation, which may drive dynamic phenomena in the solar atmosphere. We studied MAGNETic flux cancellation in a three-dimensional resistive MAGNETohydrodynamic (MHD) simulation of an emerging flux tube with a non-uniform twist profile. We solved time-dependent resistive MHD equations to model flux emergence into a MAGNETised background atmosphere. We identified several cancellation sites, estimated their cancellation rates, and examined the MAGNETic topology and associated JET activity. The non-uniform twist produced multiple opposite photospheric polarities, leading to a complex multipolar MAGNETic configuration rather than a simple dipolar structure. Interactions between inner secondary MAGNETic patches resulted in flux cancellation of the photospheric $B_z$ along their polarity inversion line (PIL). These interactions led to the formation of concave-up loops and a cancellation rate of $1.1 \times 10^{19}$ Mx hr$^{-1}$. During cancellation, MAGNETic RECONNECTion between converging opposite polarities progressively created a coherent MAGNETic flux rope above the cancellation region. The evolution of the rope was associated with a blowout JET, as the rope expanded and released part of its stored twist into the overlying corona. We also examined two smaller secondary cancellation events at photospheric heights. Our results highlight the role of internal flux cancellation in restructuring the MAGNETic field and driving blowout-JET activity in emerging regions.
[abstract 9 / 54] Yes (score: 5) - Title: Funnel Leakage of the Wien Fireball in the Early Nebula after a Binary Neutron Star MergerAuthors: Shao-Ze Li, Yun-Wei Yu, He Gao, Peng-Cheng Yang, Yu Qu,Comments: 12 pages, 8 figures, submitted to ApJSubjects: astro-ph.HECreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
A newborn neutron star (NS) that survives after a binary NS merger can inject its rotational energy into the surrounding ejecta while the ejecta are still optically thick. The injected energy is redistributed by the pair cascade, and the nebula becomes a radiation-dominated plasma composed of photons and e^+- pairs. Compton scattering then governs the energy exchange while the photon number is conserved in scattering. This nebula is evolved with a one-zone model that includes pair creation, annihilation, photon injection, diffusion, and in particular the leakage through the JET-induced polar funnel. For typical parameters, we find that the Compton parameter y is much larger than unity at early times. The nebula therefore remains in saturated Comptonization for 100 s to a few thousand seconds, depending on the MAGNETic field strength of the post-merger NS. The radiation field takes a Wien spectrum with a Compton equilibrium temperature. The nebula is then a so-called Wien fireball. The Compton temperature decreases from tens of keV to a few keV at early times. As long as the ejecta are optically thick, the funnel leakage is comparable to or exceeds the adiabatic loss. The funnel emission is quasi-thermal, and its isotropic-equivalent luminosity is much higher than the spin-down luminosity. We suggest that the quasi-thermal components observed in the extended emission of short GAMMA-RAY BURSTs could come from the funnel leakage of the nebula fireball.
[abstract 10 / 54] Yes (score: 4) - Title: High-resolution Very Large Array Radio Observations of the Boomerang Pulsar Wind NebulaAuthors: Paul C. W. Lai, Chi-Yung Ng, Shumeng Zhang,Comments: 11 pages, 6 figures, published on ApJSubjects: astro-ph.HECreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
We present a radio polarimetric study of the Boomerang pulsar wind nebula G106.65+2.96 with Very Large Array (VLA) observations at the 6 GHz band. Our high-resolution image discovers new small-scale features in the nebula, including an elliptical core of $40''\times20''$ surrounding the central pulsar and a $2'$-long arc wrapping around the core in the north. The latter shows a gap from the core, and it consists of a bright lobe in the northwest and a tongue-like structure in the northeast. These could be resulting from the pulsar wind interaction with the environment. Our POLARIZATION measurement reveals a highly ordered MAGNETic field with toroidal geometry. The small scale features are all highly linearly polarized. In particular, the lobe has a POLARIZATION fraction of $\sim$60%, close to the SYNCHROTRON limit. This is also much higher than the value measured at a lower frequency, implying significant dePOLARIZATION. We show that this can be explained by Faraday rotation in the nebula, and we constructed a simple 3D model accordingly to estimate a MAGNETic field strength of $\sim$25-70$ μ$G assuming a median inclination angle of $60^\circ$, which uncertainty arises from the uncertainty in the flux measurement and its distance.
[abstract 11 / 54] Yes (score: 4) - Title: Point-like Off-pulse GeV Emission from the Millisecond Pulsar PSR J0437-4715Authors: Ziwei Ou,Comments: comments are welcomeSubjects: astro-ph.HECreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
PSR J0437-4715 is a gamma-ray millisecond pulsar, which has been detected by FERMI-LAT. For understanding the nature, we analyze the GeV gamma-ray data obtained with FERMI-LAT around the pulsar region. Based on the pulsar timing ephemeris, we derived the gamma-ray pulse profile and defined on-pulse and off-pulse phase intervals. A binned likelihood analysis was performed to investigate the spectral properties of the pulsar across different phase ranges. No spatial extension was detected for off-pulse, with an upper limit radius of 0.12 degree. We further investigate the relationship between gamma-ray luminosity, X-ray luminosity, and bow-shock radius for a sample of pulsars with detected bow-shock PWN. The relationship between gamma-ray luminosity and X-ray luminosity is explored. The conversion efficiency from spin-down power to GeV emission of outer gap model is consistent with a termination shock located close to the pulsar. We discuss the potential nature of off-pulse GeV emission and the connection to bow shock pulsar wind nebulae.
[abstract 12 / 54] Yes (score: 4) - Title: Collisionless Shock Driven by a Supersonic Velocity ShearAuthors: Kazuki Kamiido, Yutaka Ohira,Comments: 5 pages, 5 figureesSubjects: astro-ph.HE physics.plasm-phCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
The long-term evolution of a RELATIVISTIC collisionless velocity shear in an unMAGNETized electron-positron plasma is investigated using a first-principle particle-in-cell simulation. The Alves instability converts the shear kinetic energy into thermal and MAGNETic field energy. The resulting pressures push the plasma, leading to the formation of collisionless shocks. The generated collisionless shocks would accelerate high energy particles, which is a possible solution to the injection problem of shear acceleration. In addition, the collisionless shocks generate a MAGNETic field turbulence that is required for the shear acceleration to work.
[abstract 13 / 54] Yes (score: 4) - Title: First uGMRT Constraints on Rotation Measure in the Radio-Quiet Seyfert Galaxy NGC 4235Authors: Salmoli Ghosh, Preeti Kharb, Janhavi Baghel,Comments: Accepted for publication in the Journal of Astrophysics and AstronomySubjects: astro-ph.GACreated: 2026-10-07; Updated: 2026-10-09; Datestamp: 2026-10-09
We present a multi-frequency polarimetric study of the radio-quiet Seyfert galaxy NGC 4235 using the upgraded Giant Metrewave Radio Telescope (uGMRT), aimed at constraining the Faraday rotation properties of its kpc-scale radio emission. This marks the first-ever analysis of POLARIZATION across two frequency bands of the uGMRT and the first constraints on rotation measure (RM) at lower frequencies for a weak radio source (17.1$\pm$1.7 mJy at 1.3 GHz, 27.7$\pm$2.8 mJy at 663 MHz). We detect linearly polarized radio emission associated with the `core' and the extended lobes of NGC 4235. Broadband polarimetric analysis yields an RM value of {$\sim200$ rad m$^{-2}$} in the `core', indicating Faraday rotation by MAGNETized plasma external to the SYNCHROTRON-emitting regions. Using these RM constraints, we estimate an average electron density of the Faraday-rotating medium of $\sim$3$\times10^{-2}$ cm$^{-3}$ for a characteristic perturbation scale of $\sim$0.3 parsec within an assumed MAGNETized region of size $\sim$1.3 kpc, consistent with a diffuse MAGNETized sheath or AGN-driven wind. These results extend classical Faraday rotation diagnostics to the low-power, radio-quiet AGN regime and demonstrate the potential of uGMRT broadband polarimetry for probing MAGNETized environments in and around such AGN.
[abstract 14 / 54] Yes (score: 4) - Title: Disk Structure May Determine AGN Variability and Explain the Accretion Disk Size Problem: No Broad Line Region RequiredAuthors: Amy Secunda, Yan-Fei Jiang, Jenny E. Greene,Comments: submitted to ApJSubjects: astro-ph.HE astro-ph.GACreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
Variability is a crucial probe of ACTIVE GALACTIC NUCLEi (AGN) disks, but the impact of the structure and internal physics of the disk on this variability is poorly understood. We perform 3D multi-frequency radiation MAGNETohydrodynamic simulations of the $1300-5940~\rmÅ$ emitting region of an AGN disk. This turbulent disk simulation happens to stochastically have different disk thickness above and below the midplane. Light curves emitted from the thin top of the disk are broadly consistent with traditional variability models, where the X-ray irradiation emitted from the corona is the main driver of variability in UV-optical light curves. Conversely, the UV-optical light curves emitted from the thicker bottom of the disk are not strongly correlated with the X-ray light curve and have disk continuum reverberation mapping lags that are $3-5\times$ longer than the light travel time. While these features are inconsistent with traditional variability models, they are in good agreement with numerous recent observations. Our simulations allow us to interpret these recent observations with a new model for AGN disks, where the thicker disk leads to greater X-ray absorption, less X-ray reprocessing at larger disk radii, and a stronger signal from intrinsic variability driven by fluctuations in the AGN disk. In our simulations, we can measure the inflow timescale of these fluctuations as a long lag between light curves emitted from different disk radii. Understanding how disk structure impacts AGN variability and reverberation mapping can allow us to predict the thickness of AGN disks using UV-optical AGN light curves.
[abstract 15 / 54] (score: 3) - Title: Superposition model for energy reconstruction and mass identification in COSMIC RAY spectraAuthors: Hu Liu, Fanping Li, J. Zhao, L. Y. Wang, Zhe Li, S. Z. Chen,Comments: 16 pages, 16 figures, Accepted for publication in Physical Review DSubjects: astro-ph.HE astro-ph.IMCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
The "knee" of COSMIC RAY spectra may reflect the maximum energy accelerated by galactic COSMIC RAY sources or the limit of the galaxy's ability to bind COSMIC RAYs. Measurements of individual energy spectra are a crucial tool to understand the origin of the knee. Energy reconstruction and composition identification are foundations of the individual energy spectra measurements. One of the main scientific goals of Large High Altitude Air Shower Observatory (LHAASO) is measuring the COSMIC RAY energy spectra and composition from ~10 TeV to ~EeV. In this work, a novel method for reconstructing energy and logarithm mass (lnA) based on a superposition model is introduced. Energy and lnA are reconstructed using two universal, composition- and energy-independent calibration lines. For zenith angle below 40 degree, the energy and lnA biases are within +-5% and +-0.3, respectively, across all compositions. The method uses particle densities-measured by LHAASO's electroMAGNETic and muon detectors at a fixed distance from the shower axis-rather than integrated particle counts in annular bands. The density-based approach improves resolution for both energy and lnA, especially for heavy nuclei. The resulting energy resolution ranges from below 5% to ~15% above 1 PeV, the best mass resolution for iron achieved is below 25% above 10 PeV. The hadronic model dependencies of energy and lnA are also reported. These dependencies scale with lg(E/A) and are nearly independent of primary composition.
[abstract 16 / 54] (score: 3) - Title: Examining Temporal Characteristics of GCRs in the AMS-02 eraAuthors: Cheng-Rui Zhu, Yu-Lu Liu, Mei-Juan Wang, Tian-Hao Li, Yi-Hua Zhu, Kai-Kai Duan,Comments: 16 pages, 9 figures, accepted by ApJSubjects: astro-ph.HECreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
The energy spectra of Galactic COSMIC RAYs (GCRs) serve as critical probes of their astrophysical origins and propagation mechanisms through the interstellar medium. Among the key physical processes shaping the observed spectra, solar modulation, driven by turbulent heliospheric MAGNETic fields and the variability of the solar wind, plays a dominant role in modifying GCR fluxes within the inner heliosphere. The recent release of time-dependent flux measurements for He, Li, Be, B, C, N, and O by AMS-02 provides unprecedented precision to investigate solar modulation phenomena. In this study, we demonstrate that Li, Be, B, C, N, and O nuclei exhibit solar modulation parameters consistent with those of protons (p) and He within a modified force-field approximation (FFA) framework incorporating rigidity-dependent modulation potentials. By positing that GCRs with the same charge-sign sharing the solar modulation parameters, we further forecast daily fluxes of Ne, Mg and Si from 2011 to 2020.
[abstract 17 / 54] (score: 3) - Title: Cosmic Duets II. Growth and accretion in Gaia Multi-Peak dual AGN at Cosmic NoonAuthors: M. Scialpi, F. Mannucci, D. Izquierdo-Villalba, A. Marconi, J. Singh, M. Volonteri, C. Marconcini, Q. D'Amato, B. Moreschini, M. V. Zanchettin, G. Tozzi, M. Ceci, L. Ulivi, E. Bertola, S. Bonoli, C. Bracci, E. Cataldi, C. Cicone, A. Ciurlo, M. Colpi, G. Cresci, A. De Rosa, M. Dotti, M. Fumagalli, M. Ginolfi, I. Lamperti, E. Nardini, M. Parvatikar, M. Perna, F. Rigamonti, K. Rubinur, B. Sala, A. Sesana, P. Severgnini, C. Spingola, D. Spinoso, G. Venturi, C. Vignali, S. Yeh,Comments: 22 pages, 11 figuresSubjects: astro-ph.GACreated: 2026-10-07; Updated: 2026-10-09; Datestamp: 2026-10-09
We present the first statistical characterization of the physical properties of Cosmic Duets: dual AGN in the redshift range 0.5 $\leq$ z $\leq$ 3.0 with projected separations of 1-7 kpc, corresponding to systems in which both AGN are expected to reside within the same merger remnant. We analyze the largest homogeneous sample currently available, consisting of 30 spectroscopically confirmed Cosmic Duets selected via the Gaia Multi-Peak technique. Using rest-frame UV-to-optical integral-field spectroscopy for all targets, primarily with VLT/MUSE, VLT/ERIS, and Keck/OSIRIS, we spatially resolve the two AGN components and extract separate spectra for each system. We decompose the continuum, emission lines, and Fe II complexes through spectral fitting. We derive BLACK HOLE masses of log($M_{BH}/M_{sun}$) ~ 7.4-10.1 and bolometric luminosities of log($L_{bol}/erg s^{-1}$) ~ 44.8-47.2, consistent with those of single AGN at similar redshifts. We finally carry out the first comparison of dual AGN properties with semi-analytical models and hydrodynamical simulations, including L-GalaxiesBH and Astrid. Astrid provides a closer match to the observed black-hole mass-ratio distribution, but its selected systems are predominantly at lower redshifts, resulting in lower bolometric luminosities at fixed G-band magnitude. L-GalaxiesBH perfectly reproduce the observed parameter space, but it predicts more heterogeneous pairs, with higher primary-bolometric luminosity, lower-mass secondary SMBHs, and higher Eddington ratios, resulting in an excess of near-Eddington accreting AGN due to its adopted accretion prescription. Our results suggest that, in GMP-selected systems, secondary SMBH growth is more efficient than predicted by current models, leading to more comparable black-hole masses and accretion power between the two components.
[abstract 18 / 54] (score: 3) - Title: Prevalence of radio Active Galactic Nuclei in galaxy groups since z=3.5 in the COSMOS-Web fieldAuthors: F. Ubertosi, I. Delvecchio, I. Prandoni, G. Toni, G. Zamorani, E. Daddi, M. Gitti, M. Sargent, A. Traina, C. Spingola, F. Vito, L. Moscardini, G. Gozaliasl, D. Kakkad, W. Wang, S. Sanjaripour, Z. Ghaffari, M. N. Isla Llave, R. M. Samir, G. Peluso, M. Maturi, V. Smolcic, C. Casey, J. Kartaltepe, H. J. McCracken, J. Rhodes, B. Robertson, M. Franco, D. Liu, M. Shuntov, H. Akins, O. Ilbert, A. A. Khostovan,Comments: Under review for Astronomy & Astrophysics (referee report received)Subjects: astro-ph.GACreated: 2026-10-07; Updated: 2026-10-09; Datestamp: 2026-10-09
Radio ACTIVE GALACTIC NUCLEi (AGN) are key tracers of kinetic feedback from supermassive BLACK HOLEs. Although the dependence of their triggering on host stellar mass is well known, the impact of the large-scale environment across cosmic time is poorly understood. We investigate the role of the environment in triggering radio AGN activity, while also studying the dependence on stellar mass ($10\leq\log M_{\ast}\,{\rm [M_{\odot}]}\leq11.4$), radio luminosity ($22\leq\log L_{1.4}\,{\rm [W\,Hz^{-1}]}\leq26$), and redshift ($0.1\leq z \leq 3.5$). We combine the VLA-COSMOS 3 GHz Large Project with the COSMOS-Web galaxy and group catalogs, selecting radio-excess AGN and building radio luminosity functions (RLF) and radio AGN fractions separately for sources in galaxy groups (124 radio AGN) and in the field (405 radio AGN), out of the total of 20203 galaxies and 1678 galaxy groups. We fit the RLF to derive the cosmic evolution of radio AGN in different environments, and we provide a new parametric description of the radio AGN fractions as a function of environment, $M_{\ast}$, $L_{1.4}$, and z. Besides confirming the known positive correlation of radio AGN fraction with host $M_{\ast}$ in both groups and in the field, more importantly we find that the activation of a radio AGN in groups is enhanced relative to the field by a factor of 3--30 in space density and of 2 in radio AGN fraction at fixed stellar mass; the enhancement is also a function of $M_{\ast}$, $L_{1.4}$, and z. Furthermore, in all z bins, the radio AGN fractions peak within $r \leq 0.2R_{200}$. Overall, dense environments enhance radio AGN triggering out to at least z=3.5. We suggest the existence of a possible transition in the dominant triggering mechanism of radio AGN activity around z~1.5, potentially related to the intragroup medium in the core of groups at lower z and to merger and structure growth at earlier cosmic times.
[abstract 19 / 54] (score: 3) - Title: Understanding how Coronal Heating and Magnetic Field Scaling Affect Global Properties of the Low and Middle CoronaAuthors: Caroline L. Evans, Cooper Downs, Donald Schmit,Comments: Accepted to ApJSubjects: astro-ph.SRCreated: 2026-10-07; Updated: 2026-10-09; Datestamp: 2026-10-09
The MAGNETic field of the Sun is a key driver of coronal heating and solar wind acceleration. In tandem, these influence the observable morphology of the corona, along with defining the MAGNETic connectivity and magnitude of open MAGNETic flux. Here,we investigate how coronal heating affects the MAGNETothermal state of the 3D global corona by analyzing a series of data-constrained, thermodynamic MAGNETohydrodynamic (MHD) simulations for solar minimum conditions. We vary the overall heat deposited in the corona via modifying the input Poynting flux of a wave-turbulence-driven (WTD) model for coronal heating and by scaling the inner boundary MAGNETic field. We quantify the MAGNETic, thermodynamic, and combined MAGNETothermal effects on our simulations. We find that increasing the overall amount of heat leads to a higher magnitude of open flux and a more visibly open white-light morphology in the K-Corona between 1.5 and 6 Rsun. We quantify how plasma beta evolves and drives morphological differences between simulations. We also compare these runs to an extremely high-resolution reference solution that includes small-scale MAGNETic information in the surface boundary condition. This latter comparison provides insight into the further development of 'subgrid' corrections for low(er) resolution models to best represent the structure and observables of the corona and inner heliosphere.
[abstract 20 / 54] (score: 3) - Title: Reaching high fusion gain with grams of spin-polarized fuelAuthors: J. F. Parisi,Comments: 10 pages, 6 figuresSubjects: physics.plasm-phCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
Building on recent ignition-access work of Delgado-Aparicio, Ono, and Menard, we show that even a single-use, gram-scale quantity of spin-polarized fuel (SPF) is useful for increasing fusion power and gain in MAGNETic confinement fusion machines such as tokamaks and stellarators. While fueling a fusion power plant continuously with SPF requires $\sim$kilograms per day, far beyond present capabilities, a single-use short pulse of SPF allows a fusion plasma to cross into a high-gain regime, and stay there, even after switching back to regular unpolarized fuel. With continuous polarized fueling, POLARIZATION also makes high-gain plasmas easier to control: a resonant wave that depolarizes the fuel lowers the reactivity quickly, on a much faster timescale than transport. Grams of polarized fuel can therefore improve plasma performance and open a path to scaling SPF sources and usage, from small first experiments to continuous fueling.
[abstract 21 / 54] (score: 3) - Title: Improved analysis of time delays between radio wavelengths and X-ray of Sgr A* flares in the shock oscillation modelAuthors: Ramiz Aktar, Toru Okuda, Chandra B. Singh,Comments: 12 pages, 8 figures, Accepted for publication in MNRASSubjects: astro-ph.HECreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
We present an improved analysis of the time delays between radio and X-ray flares from the supermassive BLACK HOLE Sagittarius A* (Sgr A*), extending our previous shock oscillation model by incorporating Compton scattering. Our simulations predict delay times of 1-4 h between X-ray and radio flares, 20-40 min and 0.5-1 h between 334 GHz and 4.5 $μ$m and 2-8 keV flares, and 7-20 min and 0.5-1 h between 22-43 GHz and 350 GHz radio flares, respectively, in good agreement with recent observations. The delay time between the radio emissions (SYNCHROTRON) and X-ray emissions (bremsstrahlung) is interpreted as the transit time for sound waves traveling from the central core near the event horizon to the location of the oscillating shock. Additionally, the delay time observed between different radio wavelengths corresponds to the transit time of sound waves moving between the frequency-dependent effective radii $R_{\rm eff}(ν)$, where the optical thickness $τ_ν(R)$ at frequency $ν$ equals one on the surface of the accretion disc. The X-ray emission and the radio emission at lower frequencies peak later than the radio emission at higher frequencies. This delay occurs because the acoustic perturbations created by SYNCHROTRON emission peak near the event horizon and then expand outward. Conversely, an inverse delay happens when the acoustic waves generated by the upstream shock wave travel toward the event horizon. The predicted delay times from this interpretation qualitatively match the numerical results obtained in simulations.
[abstract 22 / 54] (score: 3) - Title: The Hand of God Revisited: Revealing the Shell Structure and Jet-Supernova Remnant Interaction in MSH 15-52Authors: Lingxiao Dang, Isabel Sander, Samar Safi-Harb, Christopher Fryer,Comments: 21 pages, 17 figures. Accepted for publication in The Astrophysical JournalSubjects: astro-ph.HECreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
We present an X-ray analysis of the SUPERNOVA remnant (SNR) MSH 15-52 associated with the young rotation-powered pulsar PSR B1509-58, using Chandra, XMM-Newton, and eROSITA, complemented by MeerKAT radio data. We report the discovery of the missing southern counterpart to the bright northern RCW 89 region and identify a foreground X-ray source that may be a previously unidentified SNR candidate. Imaging and spectroscopy with XMM-Newton and eROSITA reveal the shell properties of MSH 15-52 and suggest that both the southern and northern shell-like structures are consistent with shocked interstellar medium associated with the forward shock, while their low ionization timescales and possible hard power-law components indicate possible influence from particle injection or additional heating by the pulsar wind nebula (PWN) JETs. New Chandra spectral maps of the southern JET reveal a region of hard non-thermal emission, with a photon index of approximately 1.6, suggesting interaction between the PWN and the reverse shock and possible re-acceleration of the pulsar outflow. Spatially resolved spectroscopy of the RCW 89 northern clumps reveals high-velocity, metal-rich ejecta with enhanced Ne and Mg abundances. Comparison with core-collapse nucleosynthesis models favors a massive progenitor with an initial mass of approximately 29 solar masses in one-dimensional yield models, while asymmetric explosion models show that lower-mass progenitors can also reproduce the observed abundance ratios. Our study supports a picture in which RCW 89 is part of a larger asymmetric SNR shell interacting with energetic pulsar JETs, making the system a valuable laboratory for probing pulsar-PWN-SNR interaction.
[abstract 23 / 54] (score: 3) - Title: Investigating the nature of MAGNETic turbulence in Tycho's SNR using X-ray observationAuthors: Ashwin Aravindaraj, Hui Zhu, Adrien Picquenot, Hsiang-Kuang Chang,Comments: Accepted for publication in MNRASSubjects: astro-ph.HECreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
Supernova remnants (SNRs) are widely regarded as the primary sources of Galactic COSMIC RAY acceleration and the particles are energized at the shock front of SNRs through the diffusive shock acceleration (DSA) mechanism, gaining energy by repeatedly crossing the shock. Magnetic turbulence plays a crucial role in scattering these particles back and forth, making the investigation of turbulence essential to understanding the acceleration process. In this study, we apply the two-point correlation method to derive the MAGNETic energy spectrum from the non-thermal X-ray flux image of Tycho's SNR. This image was obtained using Poissonian-based Generalized Morphological Component Analysis (pGMCA). The turbulence length scale observed in the resulting spectrum is shorter than the turbulence scale derived from previous studies of radio observations of Tycho's SNR. Additionally, we use the X-ray rim thickness measured across Tycho which is an indicator of MAGNETic field strength to estimate the MAGNETic energy spectrum. The turbulence scale inferred from this method is consistent with that obtained from the non-thermal X-ray flux analysis.
[abstract 24 / 54] (score: 3) - Title: Volume Dependence of Helicity-based Eruption Diagnostics in Recurrent Coronal JetsAuthors: Chang Zhou, Jinhan Guo, Yang Guo, Jiajia Liu, Zekun Lu, Yuhang Gao,Comments: 9 pages, 5 figures. Accepted for publication in The Astrophysical Journal LettersSubjects: astro-ph.SRCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
Recurrent solar coronal JETs originate from the same source region, providing a useful setting for studying the buildup, redistribution, and release of MAGNETic energy and helicity. However, how these quantities can characterize MAGNETic evolution and the onset conditions of the eruptions remains unclear. We perform a full three-dimensional (3D) thermodynamic MAGNETohydrodynamic simulation of recurrent JETs driven by converging motions imposed at the bottom boundary. The simulation naturally produces two successive eruptions. The current-carrying helicity $H_J$ decreases during the first JET and gradually recovers between the two JETs. In contrast, the free MAGNETic energy $E_{\mathrm{free}}$ shows no clear accumulation after its first release. This difference indicates that $H_J$ provides information on MAGNETic evolution beyond that provided by $E_{\mathrm{free}}$. Furthermore, the commonly used helicity ratio $H_J/H_V$ reaches different peaks near the onset of the two JETs and is sensitive to the integration volume. By comparison, the locally normalized quantity $H_J/Φ_{\mathrm{closed}}^2$ reaches similar peaks near the onset of both JETs and is relatively insensitive to the choice among the tested integration volumes, where $Φ_{\mathrm{closed}}$ is the single-polarity MAGNETic flux of the closed-field domain. These results reveal the local nature of the eruptions and suggest that $H_J$ normalized by the square of the closed MAGNETic flux may be a useful diagnostic of eruptive conditions.
[abstract 25 / 54] (score: 3) - Title: Kinetic wave activity and proton heating in 3D hybrid simulations of decaying balanced and imbalanced Alfvénic turbulenceAuthors: C. A. González, T. A. Bowen, A. Mallet, A. Tenerani,Comments:Subjects: physics.plasm-ph physics.space-phCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
We investigate turbulent dynamics from large to sub-proton scales, the kinetic wave activity and resulting proton heating in three-dimensional hybrid-kinetic simulations of freely decaying balanced and imbalanced Alfvénic turbulence. We considered initial fluctuations with same amplitude and spectral shape but different degrees of correlation between velocity and MAGNETic field perturbations (i.e., normalized cross-helicity), which define the corresponding turbulent regimes. We found that our balanced turbulence simulation exhibits stronger energy dissipation and more efficient proton heating compared to the imbalanced case. On the large fluid scales, the two simulations undergo distinct nonlinear dynamic and energy cascades, leading to different spectral properties once turbulence is well developed. At sub-proton scales, fluctuations are predominantly oblique with right-hand POLARIZATION, a property common to both regimes. In contrast, only the imbalanced simulation displays substantial wave power parallel to the guide MAGNETic field, with clear signatures of ion-cyclotron waves. These waves are excited in regions with strong temperature anisotropy that arise during the initial nonlinear steepening of Alfvénic fluctuations, a process that simultaneously generates parallel-propagating proton beams. Furthermore, non-Maxwellian features emerge in velocity space, indicating different heating mechanisms in balanced and imbalanced regimes and providing evidence for the role of kinetic instabilities in regulating the turbulent dynamics. Overall, these results show that cross-helicity is a key parameter controlling the large-scale evolution, kinetic activity, and energy dissipation in collisionless turbulent plasmas.
[abstract 26 / 54] (score: 2) - Title: Revising the Spin and Kick Connection in Isolated Binary Black HolesAuthors: Vishal Baibhav, Vicky Kalogera,Comments: 21 pages, 12 figuresSubjects: astro-ph.HE gr-qcCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
The origin of BLACK HOLE (BH) spins remains one of the least understood aspects of BHs. Despite many uncertainties, it is commonly assumed that if BHs originated from isolated massive star binaries, their spins should be aligned with the orbital angular momentum of the binary system. This assumption stems from the notion that BHs inherit their spins from their progenitor stars. In this study, we relax this long-held viewpoint and explore various mechanisms that can spin up BHs before or during their formation. In addition to natal spins, we discuss physical processes that can spin BHs isotropically, parallel to natal kicks, and perpendicular to natal kicks. These different mechanisms leave behind distinct imprints on the observable distributions of spin magnitudes, spin-orbit misalignments and the effective inspiral spin of merging binaries. In particular, these mechanisms allow even the binaries originating in the field to exhibit precession and retrograde spin ($χ_{\rm eff}<0$). This broadens the parameter space allowed for isolated binary evolution into regimes which were previously thought to be exclusive to dynamically assembled binaries.
[abstract 27 / 54] (score: 2) - Title: Deep learning in the abyss: a stratified Physics Informed Neural Network for data assimilationAuthors: Vadim Limousin, Nelly Pustelnik, Bruno Deremble, Antoine Venaille,Comments:Subjects: physics.ao-ph physics.flu-dynCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
The reconstruction of deep ocean currents is a major challenge in data assimilation due to the scarcity of interior data. In this work, we present a proof of concept for deep ocean flow reconstruction using a Physics-Informed Neural Network (PINN), a machine learning approach that offers an alternative to traditional data assimilation methods. We introduce an efficient algorithm called StrAssPINN (for Stratified Assimilation PINNs), which assigns a separate network to each layer of the ocean model while allowing them to interact during training. The neural network takes spatiotemporal coordinates as input and predicts the velocity field at those points. Using a SIREN architecture (a multilayer perceptron with sine activation functions), which has proven effective in various contexts, the network is trained using both available observational data and dynamical priors enforced at several collocation points. We apply this method to pseudo-observed ocean data generated from a 3-layer quasi-geostrophic model, where the pseudo-observations include surface-level data akin to SWOT observations of sea surface height, interior data similar to ARGO floats, and a limited number of deep ARGO-like measurements in the lower layers. Our approach successfully reconstructs ocean flows in both the interior and surface layers, demonstrating a strong ability to resolve key ocean mesoscale features, including vortex rings, eastward JETs associated with potential vorticity fronts, and smoother Rossby waves. This work serves as a prelude to applying StrAssPINN to real-world observational data.
[abstract 28 / 54] (score: 2) - Title: New Signs Pointing Toward a Correlation Between Astrophysical Neutrinos and Radio FlaresAuthors: Yjan A. Gordon, Peter S. Ferguson, Eric J. Hooper, Michael N. Martinez,Comments: 15 pages, 11 figures, 5 tables. Published in OJAp. Supplementary data available at https://zenodo.org/records/23223067Subjects: astro-ph.GA astro-ph.HECreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
We use data from the first two epochs of the Very Large Array Sky Survey (VLASS) and the IceCube Neutrino Observatory to search for evidence of a correlation between radio variability and the detection of astrophysical neutrinos. Our work probes the radio population down to $S_{3\,\text{GHz}}\gtrsim$ a few mJy, more than an order of magnitude fainter than previous analyses that aim to cross correlate radio variability with neutrino detections. We find an excess number of associations between flaring radio sources and neutrinos that were detected between the first and second VLASS observations at $>2σ$ confidence. This excess is consistent with radio flares contributing $\sim13\,\%$ of the astrophysical neutrinos observed by IceCube. Notably, $\sim90\,\%$ of the radio flares associated with neutrinos are not detected at either $γ$-ray or X-ray wavelengths, highlighting the importance of deep radio observations for identifying potential electroMAGNETic counterparts to astrophysical neutrinos. No excess in the number of associations between the wider radio-variable population and the IceCube neutrinos is seen when no time constraint is placed on the neutrino detection. We predict that data from future VLASS epochs will see an excess number of associations between radio flares and neutrinos at the $>3σ$ level, and expected improvements to the positional constraints on the neutrinos may increase that confidence to $>5σ$, should our results be representative.
[abstract 29 / 54] (score: 2) - Title: Stable mass transfer in massive binaries leading to merging BLACK HOLEsAuthors: Xiao-Tian Xu, Norbert Langer, Jakub Klencki, Chen Wang, Xiang-Dong Li,Comments: Published in Nature Astronomy with a different title "The formation of merging black holes via stable mass transfer in massive binary stars". Link to the paper https://www.nature.com/articles/s41550-026-03000-7 . This is pre-review versionSubjects: astro-ph.SR astro-ph.HE gr-qcCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
The vast majority of massive binary systems in the universe is evidently unsuited to produce merging binary BLACK HOLEs. However, several narrow evolutionary paths of isolated massive binaries towards this goal have recently been identified. Due to the high degree of simplification and assumptions applied in previous modelling of these paths, conclusions remained vague so far. For one of these paths, the stable mass transfer channel, we now construct detailed binary evolution models which include internal differential rotation as well as mass and angular momentum transfer between the stars, all the way from the zero-age main sequence to the formation of the BLACK HOLEs, only skipping the rapid late burning stages. This allows us to follow the mass and chemical structure evolution of the mass accreting component, which turns out to have a key influence on the phase of reverse mass transfer, that allows the obtained BLACK HOLE spins and mass ratios to naturally fall into the regime observed for the gravitational-wave source in the 10--25$M_\odot$ primary BLACK HOLE mass range. As for this channel, also a large number of progenitor binaries are known, we conclude that it likely contributes to the observed population of gravitational wave sources.
[abstract 30 / 54] (score: 2) - Title: Probing near-zone MAGNETic fields with extreme mass-ratio inspiralsAuthors: Jin-Lu Hu, Xin-Dong Du, Peng-Cheng Li, Tieguang Zi,Comments: 12 pages, 6 figures, to be published in JCAPSubjects: gr-qcCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
We investigate whether weak near-zone MAGNETic fields can leave observable imprints on extreme-mass-ratio inspiral (EMRI) waveforms. The central massive BLACK HOLE is modeled by the MAGNETized Schwarzschild, or Ernst, solution, and the secondary compact object is treated as a neutral point particle on equatorial circular geodesics. We compute the MAGNETic corrections to the circular-orbit quantities and the innermost stable circular orbit, and then evolve the inspiral using a hybrid, source-corrected Regge--Wheeler--Zerilli approximation, in which the Schwarzschild wave-propagation potentials are kept fixed while the source is evaluated on the MAGNETized orbit. For a fiducial system with \(M=10^6M_\odot\) and \(μ=10M_\odot\), a field strength \(B\simeq 4\times10^{-5}M^{-1}\), corresponding to \(B_{\rm phys}\sim10^9\,{\rm G}\), produces a one-year dephasing of about \(1.3\) rad and \ccr{a LISA-noise-weighted mismatch which, after maximization over the relative arrival time and initial GW phase, remains slightly above the adopted distinguishability threshold at one year}. Our results suggest that EMRIs can in principle probe extremely strong near-zone MAGNETic fields, whereas ordinary MAGNETic environments around massive BLACK HOLEs are likely too weak to produce detectable effects within the present approximation.
[abstract 31 / 54] (score: 2) - Title: A Variational Framework for Guiding-Center Kinetics, Anisotropic Equilibria, and Quasisymmetry in StellaratorsAuthors: Lanke Fu, Amitava Bhattacharjee,Comments:Subjects: physics.plasm-phCreated: 2026-10-07; Updated: 2026-10-09; Datestamp: 2026-10-09
We present a variational framework in which (i) guiding-center kinetics, (ii) macroscopic force balance with gyrotropic pressure, and (iii) quasisymmetry (QS) appear as facets of a single structure. Starting from a guiding-center Vlasov--Maxwell action, constrained variations yields the guiding-center kinetic equation and Maxwell equations. Without phenomenological closure, momentum conservation yields $\mathbf J \times \mathbf{B}/c = \nabla \cdot Π$. This framework recovers the classical result that, for any equilibrium distribution built on the invariants of the reduced motion, the parallel projection of this balance holds identically, so that pressure anisotropy is a kinematic consequence of MAGNETic-moment conservation together with the variation of $B$ along field lines, rather than a modeling choice. We connect QS to an integrability condition expressed in coordinate-free form. We then derive an explicit expression for the current crossing the flux surfaces. Its flux-surface average vanishes identically in a QS field, but it vanishes pointwise only if $p_\parallel+p_\perp$ is a flux function. Combined with the parallel identity this forces $p_\parallel = p(ψ) + K(ψ)B^2$ and $p_\perp = p(ψ) - K(ψ)B^2$, consistent with the anisotropic equilibria obtained from a constrained Kruskal--Kulsrud functional, in which $(p_\parallel+p_\perp)/2$ is a flux function [Phys. Rev. E 104, 015213 (2021)]. The structure arises from the kinetic moments without a Lagrange multiplier. For such equilibria the parallel current in a QS field follows in closed form, with a single resonance at $ι= N/M$ in place of the dense set of resonant obstructions of a generic three-dimensional field. Finally, QS is a Noether symmetry, so its breaking is measured by the non-conservation of the associated momentum. We construct a distribution-weighted residual and relate it to existing QS metrics.
[abstract 32 / 54] (score: 2) - Title: Will a Supernova explode in CD-30°11223?Authors: L. Piersanti, L. R. Yungelson, E. Bravo, I. Dominguez,Comments: 10 pages, 8 figures, Accepted for the publication in Astronomy & AstrophysicsSubjects: astro-ph.SR astro-ph.HECreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
Accretion of He-rich matter onto a low-mass CO WD from a He-rich donor may lead to an explosive event of SN Ia proportion, though with low peak luminosity and peculiar nucleosynthesis. Recently such a possibility for some binaries with He-accreting WDs has been questioned, suggesting that, if the effects of rotation are accounted for in the evolution of the accretor, the latter does not explode, but it becomes a WD with a massive He-buffer. We investigate the expected evolution of the currently detached binary CD-3011223 harboring a 0.74Msun CO WD and a 0.47Msun donor with a He-burning core and a very thin H-envelope. We use the stellar evolution code FuNS to compute the evolution of CD-3011223 up to the epoch when the two components come into contact and through the RLOF phase of the donor. With respect to our earlier study of the system PTF J2238+743015.1, we also include the transport of angular momentum due to MAGNETic instabilities (MAGNETic model). During the H-accretion phase, the effects of rotation in the accretor are negligible. In the "MAGNETic model", the angular momentum deposited by the accreted matter is very efficiently redistributed along the whole WD due to MAGNETic instabilities, so that the angular velocity of the accreted layers remains very low. During the He-accretion phase, the accretor experiences two very strong He-flashes, which result in the ejection from the binary system of a large part of the matter previously accreted. The system ends its life as a CO core capped by a massive He/C/O-envelope (Delta M_env ~ 0.194Msun) and an extremely low-mass companion, remnant of the donor, like in a rotating model not including the effects of MAGNETic field. The system CD-3011223 cannot be regarded as the potential progenitor of Supernova Ia. Such a conclusion applies also to all detached binary systems having similar masses of components and orbital periods.
[abstract 33 / 54] (score: 2) - Title: Existence Conditions for Darboux Curves and Analytic First Integrals of a Liénard-Type Quadratic Vector FieldAuthors: Shaoxuan Huang,Comments:Subjects: nlin.SI cs.SCCreated: 2026-10-07; Updated: 2026-10-09; Datestamp: 2026-10-09
We study the rational quadratic differential equation \[ \frac{\mathrm{d}y}{\mathrm{d}x} = \frac{ay^2+by+cx}{y^2}, \qquad a,b,c\in\C, \] under the non-degeneracy assumptions \[ c\neq 0,\qquad 2ay+b\not\equiv 0. \] Equivalently, after clearing the denominator, we consider the polynomial vector field \[ \dot{x}=y^2,\qquad \dot{y}=ay^2+by+cx. \] We give a complete, directly checkable classification of its Darboux curves. If $a=0$, no non-constant Darboux polynomial exists. If $a\neq 0$, a non-constant Darboux polynomial exists if and only if \[ c=-ab\qquad\text{or}\qquad c=-2ab. \] In these two cases the unique irreducible Darboux polynomials, up to non-zero constant multiples, are respectively \[ y-ax,\qquad y^2-2bx. \] Consequently every non-constant Darboux polynomial is a non-zero constant multiple of a positive integral power of the corresponding irreducible factor. We then place this classification in the framework of Riccati (R-)integrability and rational potentials. Excluding the exceptional branch $c=-2ab$, the analytic integrability theorem identifies $c=-ab$ as the branch admitting a global Riccati-type analytic first integral. For $c=-2ab$, we compute the first four transverse variational groups along the transformed Darboux divisor over the rational function field. Their dimensions are $1,2,3,4$; the fourth is the full group of invertible fourth-order transverse JETs. We prove that this exceptional branch admits no Riccati first integral and hence is not R-integrable. Finally, we relate the branch $c=-ab$ to the Quartic Inverse Riccati (QIR) class and discuss an invariant-based classification problem for quartic Abel equations.
[abstract 34 / 54] (score: 2) - Title: Gravitational-Susceptibility Dip Behind DESI's results: Addressing the Phantom Crossing by Local limit of Nonlocal GravityAuthors: Aria Hemmatian, Yahya Mohammadi, Javad Tabatabaei, Shant Baghram,Comments: 13 pages, 4 figures, 2 tables. Updated references and minor improvementsSubjects: astro-ph.CO gr-qcCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
The second data release of the Dark Energy Spectroscopic Instrument (DESI), based on more than fourteen million galaxies and QUASARs, prefers a DARK ENERGY component whose equation of state is dynamical. In the simplest two-parameter description of this behavior, the Chevallier--Polarski--Linder (CPL) parametrization, the data favor the quadrant $w_0>-1$, $w_a<0$, which implies that the equation of state crosses the phantom divide $w=-1$ at a redshift $z\simeq0.4$. We show that the local limit of nonlocal gravity, a teleparallel extension of general relativity governed by a scalar function called gravitational susceptibility $S(x)$, offers a natural explanation. In this model a cosmological constant is not allowed; DARK ENERGY is necessarily dynamical. The phantom crossing seen by an observer is an effective phenomenon generated by the time evolution of $S(z)$. We establish a correspondence: to every general-RELATIVISTIC DARK ENERGY model with equation of state $w(z)$, there corresponds a modified TEGR cosmology with $w=-1$ and a suitable susceptibility $S(z)$ that are indistinguishable at the level of the background expansion. We construct the susceptibility functions that reproduce the CPL behavior favored by DESI data, and we confront the model with the combined CMB,BAO, and SNe data using Boltzmann solver codes. The recovered susceptibility displays a characteristic low-redshift dip with depth $β= -0.025 \pm 0.007$ at $z\simeq 0.4 $, and its derivative changes sign at a redshift equal to the phantom-crossing epoch.
[abstract 35 / 54] (score: 2) - Title: PQLS: A Quasilinear Gyrokinetic Transport Solver with a Bayesian Saturation-Rule ClosureAuthors: F. Wilms, A. Agrawal, J. J. Freigang, T. F. Neiser, B. J. Frei, O. Meneghini,Comments:Subjects: physics.plasm-phCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
Quasilinear models make gyrokinetic turbulent-transport predictions sufficiently fast for integrated modelling, but their predictive capability is limited by two factors: the physical and geometrical applicability of the linear solver, and the validity of the saturation rule used to close the model. We present the Predictive Quasilinear Solver (PQLS), a quasi- linear gyrokinetic transport solver formulated in general MAGNETic geometry. Its implementation as an eigenvalue solver retains electroMAGNETic and collisional effects, provides access to dominant and subdominant modes and is differen- tiable with respect to all plasma parameters. Linear benchmarks against GENE reproduce the growth rates, frequencies, and eigenfunctions. We additionally formulate the saturation-rule closure as a Bayesian inference problem that distin- guishes uncertainty in its fitted coefficients from the residual model-form uncertainty. The approach is demonstrated by calibrating the SAT3 rule on PQLS quasilinear weights against published nonlinear CGYRO cases. In addition to improving the robustness of the calibration, the new method also quantifies the uncertainty in each of the fit coefficients. Such uncertainty is propagated through transport calculations to produce error-aware profiles that are compared to the ones obtained from the full gyrokinetic simulation, showing excellent agreement.
[abstract 36 / 54] (score: 2) - Title: Theory of Equivalent Tokamaks for Characterizing Turbulent Transport in Quasi-symmetric StellaratorsAuthors: Hongxuan Zhu, R. Gaur, X. Wei, Z. Lin, A. Bhattacharjee,Comments:Subjects: physics.plasm-phCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
It is well known that quasi-symmetric (QS) stellarators are isomorphic to tokamaks in terms of their neoclassical-transport properties, and the corresponding transport coefficients can be calculated in the same manner as in tokamaks. However, less is known regarding the turbulent-transport properties of QS stellarators, e.g. the transport coefficients from the ion-temperature-gradient (ITG) mode. In this work, a systematic theory of the ``equivalent tokamaks'' for QS stellarators is presented based on the local gyrokinetic formulation and the near-axis expansion theory. It is shown that to zeroth order in the minor radius, the equivalent tokamaks can be chosen to have circular flux surfaces and can be characterized by three geometric quantities: the aspect ratio, the rotational transform, and the MAGNETic shear. To achieve first-order accuracy, however, not all QS stellarators have equivalent tokamaks, but good approximations can be found for some cases either as global or local equilibria. Local and global gyrokinetic simulations of ITG transport are performed for a selection of QS configurations, and quantitative agreement in the turbulent transport levels is found between the stellarators and their equivalent tokamaks.
[abstract 37 / 54] (score: 2) - Title: Discovery of thermal radio recombination line emission toward the high-mass protostar IRAS18162$-$2048Authors: R. Fedriani, J. F. Gomez, Y. Cheng, M. Osorio, G. Anglada, C-Y. Law, J. M. Masque, A. F. Placinta-Mitrea, G. Blazquez-Calero, G. Cosentino,Comments: 4 pages, 4 figures, 4 appendices. Accepted in A&A Letters. Version after language editorSubjects: astro-ph.GACreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
The physical conditions within the innermost few tens of au of high-mass protostars ($M_*>8~M_\odot$) remain largely unexplored. At these scales, ionised emission may trace photoionised gas, accretion disks, or the base of protostellar JETs. We search for ionised emission in the form of radio recombination lines (RRLs) in high-mass star-forming regions. We use archival data from the Atacama Millimeter/submillimeter Array (ALMA) interferometer in band 6 ($\sim$1.3 mm) with a resolution of $θ_\mathrm{beam}\sim53~\mathrm{mas}\times42~\mathrm{mas}$ to examine the high-mass protostar IRAS18162$-$2048, driving source of the Herbig-Haro (HH) objects HH80-81. We detect, for the first time in this protostar, the thermal emission of the RRL H30$α$ ($\mathrm{rest~frequency}=231.90093$ GHz). The ionised emission is spatially unresolved in our observations, but we estimate an emitting region $\lesssim50$ au at the source distance of 1.4 kpc. The H30$α$ line profile is broad and spectrally resolved with a Local Standard of Rest velocity of $\sim-14~\mathrm{km~s^{-1}}$ (i.e., $\sim-26~\mathrm{km~s^{-1}}$ blue-shifted with respect to the systemic velocity of the cloud) and a full width at half maximum of $\sim82~\mathrm{km~s^{-1}}$. These observations suggest that the H30$α$ line is tracing outflowing blue-shifted material in the well-known radio JET from this object. This detection opens the possibility of detailed studies of the kinematics and physical properties of ionised JETs.
[abstract 38 / 54] (score: 2) - Title: Exemplary Merging Clusters II: XMM-Newton and Chandra X-ray Observations of MACS J1752.0+4440 and ZwCl 1856.8+6616Authors: K. HyeongHan, K. Finner, W. Lee, E. Silich, W. Forman, C. Jones, A. Tümer, S. Randall, J. ZuHone, M. James Jee, D. Wittman, R. J. van Weeren, M. Troxel,Comments: 27 pages, 14 figures, submitted to ApJSubjects: astro-ph.HECreated: 2026-10-07; Updated: 2026-10-09; Datestamp: 2026-10-09
Using deep XMM-Newton and Chandra observations, we compare the double-radio-relic galaxy cluster mergers MACS J1752.0+4440 and ZwCl 1856.8+6616. Both are 1:1 mass-ratio mergers with similar relic separations but differing nearly an order of magnitude in total mass. In MACS J1752.0+4440, the surface-brightness discontinuity at the northeastern relic yields Mach $M_ρ=1.4\pm0.2$, while the temperature jump provides a weaker constraint, corresponding to $M_{kT}\lesssim2.3$ at the $2σ$ level, lower than the radio-derived $M_{\rm radio}=3.1\pm0.1$. No discontinuity is detected at the southwestern relic. Thermodynamic maps and axial profiles reveal surviving relatively low-entropy cores embedded in Mpc-scale stripped-gas structures. The nearly uniform X-ray tail brightness and a southwestern plateau coincident with a third lensing mass peak favor a non-zero impact parameter and complex assembly history. In ZwCl 1856.8+6616, we do not detect a clear surface brightness discontinuity at either relic. The northern X-ray peak leads its brightest cluster galaxy (BCG) and lensing peak, while the hotter southern X-ray peak is laterally offset from its BCG and lensing peak. The asymmetric intracluster emission favors a phase near or after first apocenter, when displaced gas can develop a slingshot-like morphology. We present two TNG-Cluster analogs in which a minor merger followed by an off-axis major collision produces extended X-ray tails resembling MACS J1752.0+4440 and later leads to gas structures resembling ZwCl 1856.8+6616. X-ray morphology independently confirms the merger phases inferred from relic-based chronometry, placing MACS J1752.0+4440 before and ZwCl 1856.8+6616 after first apocenter, and demonstrating that similar relic and lensing configurations can correspond to distinct dynamical states.
[abstract 39 / 54] (score: 2) - Title: Discovery of a Nearby Ultra-fast Magnetic White Dwarf Propeller: Common Pathways to Magnetic Cataclysmic VariablesAuthors: Antonio C. Rodriguez, Kareem El-Badry, R. Michael Rich, Kevin N. Ortiz Ceballos, Ingrid Pelisoli, Casey J. Law, Kaya Mori, Boris Gaensicke, Edo Berger, Liam Connor, Ilkham Galiullin, Ilaria Caiazzo, Matthew Graham, Samuel Whitebook,Comments: Submitted to the Open Journal of Astrophsyics; comments welcomeSubjects: astro-ph.HECreated: 2026-10-07; Updated: 2026-10-09; Datestamp: 2026-10-09
The fastest spinning white dwarfs (WDs), which approach break-up speeds, are found in close binary systems. In the two known MAGNETic WD ``propellers'', AE~Aqr and LAMOST J0240+1952, the MAGNETic WD spins so rapidly that it ejects the material transferred by its Roche-lobe-filling companion rather than accreting it. We report the discovery of the third such system, 1eRASS J042633.5$-$250226 (1eRASS J0426/Valeria), at only 265 pc, identified by combining SRG/eROSITA and \textit{Gaia} data via the ``X-ray Main Sequence''. TESS photometry shows AE~Aqr-like flaring and orbital modulation with $P_{\mathrm{orb}} \approx 6.62$ hr, and ZTF shows month-long high/low state changes. Phase-resolved Palomar/DBSP spectroscopy confirms the orbital period and yields a donor radial velocity of $K_2 = 202\pm7$ km s$^{-1}$. High-speed Palomar/CHIMERA photometry detects optical pulsations on three nights with the strongest detection at $P_\textrm{spin} = 26.8$ sec, though further observations are needed to confirm this as the WD spin. Spectral fitting of the donor in the low state reveals a late K-type star with $T_{\mathrm{donor}} = 4100\pm150$ K. Zeeman splitting in the optical spectrum yields a candidate field strength of $B_{\mathrm{WD}} = 26 \pm 3$ MG, meaning the system will evolve into a polar. Like other WD propellers, the system is X-ray faint ($L_X \approx 7\times 10^{30}$ erg s$^{-1}$), but is not detected in the radio, and a spin period is not detected in X-rays by SRG/eROSITA. The proximity of this system and evolutionary model constraints on the timeframe of the propeller phase yield a birth rate density of $\sim8\times10^{-16} \textrm{pc}^{-3} \textrm{yr}^{-1}$, which agrees with that of MAGNETic CVs, suggesting that a substantial fraction of MAGNETic CVs pass through a propeller phase.
[abstract 40 / 54] (score: 2) - Title: The Origin of the FERMI Halo-like Emission: A New Model of the FERMI BubblesAuthors: Ilias Cholis, Leo Qiyuan Hu, Yi-Ming Zhong,Comments: 30 pages, 20 figures, 11 tables and four appendices, ZENODO link with model maps: https://zenodo.org/records/23199004Subjects: astro-ph.HE astro-ph.CO hep-phCreated: 2026-10-07; Updated: 2026-10-09; Datestamp: 2026-10-09
We study the gamma-ray sky at high latitudes for energies between 0.3 and 900 GeV. We search for a contribution in the high-latitude sky and in the region of the Galactic Stellar Halo that would be beyond known astrophysical emissions, i.e., the galactic diffuse emission, the isotropic mostly extragalactic gamma-ray background, the FERMI Bubbles, Loop I, the contribution from the Galactic Center Excess, and the known point and extended gamma-ray sources detected by the FERMI-LAT Collaboration. We perform a sequence of template fits to the FERMI gamma-ray data, testing different regions of interest of the galactic sky, utilizing a large set of alternative galactic diffuse emission models, and implementing alternative fitting schemes to assess the impact of increased modeling complexity of the gamma-ray sky. We find that the halo-like emission recently reported by Totani (2025) is real, but it is likely due to emission from the FERMI Bubbles rather than DARK MATTER annihilation in the Galactic halo. We provide new templates for the FERMI Bubbles, including an updated model for the Flat Bubbles and a detailed model of their substructures, the Cocoons and the Inner Bubbles. In combination, these components account for the previously reported halo-like emission. We also estimate the associated fluxes and spectral properties of the Flat Bubbles, the Inner Bubbles, and the Cocoons. This updated model for the FERMI Bubbles provides new input toward understanding their origin.
[abstract 41 / 54] (score: 2) - Title: Observational Signatures of Dyonic Black Holes in Non-Linear ElectrodynamicsAuthors: Sobhan Kazempour, Sichun Sun, Zhiqing He, Chengye Yu,Comments: 22 pages, 32 figuresSubjects: gr-qc astro-ph.HE hep-phCreated: 2026-10-07; Updated: 2026-10-09; Datestamp: 2026-10-09
We study the observational features of thin-disk accretion and emission spectra for static, spherically symmetric dyonic BLACK HOLEs in non-linear electrodynamics (NLED). In contrast to classical Maxwell theory, where electroMAGNETic duality assumes equal charges, the coupling parameters in NLED introduce a new gravitational potential and modify the geometry in the strong-field regime. We also study the kinematic characteristics of particles on circular orbits, such as their angular velocity, specific energy, and specific angular momentum. It is found that modifications of NLED lead to a shrinkage of the ISCO radius, resulting in a shift of the radiation spectrum thermal maximum towards smaller radii and, consequently, an increase in the local effective temperature in comparison with the standard Schwarzschild and Reissner-Nordström solutions. Additionally, we compute null-geodesic orbits to determine the optical edge of both the photon sphere and the BLACK HOLE shadow. In order to assess the observational validity of the aforementioned alternatives, we carry out a $χ^2$ goodness-of-fit test through the angular diameter constraints at the horizon scale collected by the Event Horizon Telescope (EHT) concerning Sagittarius A* ($\text{Sgr A}^*$). We prove that both these dyonic NLED and purely MAGNETic models have good statistical agreement with experimental data.
[abstract 42 / 54] (score: 2) - Title: Reconstruction of Multiscale Plasma Dynamics Across Operating RegimesAuthors: Maryam Reza, Farbod Faraji,Comments: 27 pages, 17 figuresSubjects: physics.plasm-ph cs.LGCreated: 2026-10-07; Updated: 2026-10-09; Datestamp: 2026-10-09
Reconstructing spatially resolved plasma dynamics from few sensors is essential for diagnostics, reduced-order modelling and control, yet remains difficult because the sparse measurements incompletely constrain multiscale, regime-dependent degrees of freedom. The Shallow Recurrent Decoder (SHRED) partially addresses spatial sparsity by using measurement histories; however, its fully connected decoder provides no explicit mechanism for resolving spatial structure across scales or explicit parametric dependency. We introduce the Recurrent Multiscale Affine-modulated Inference Network (ReMAIN), which preserves SHRED's recurrent temporal encoding but replaces its decoder with a U-Net whose feature hierarchy is conditioned by the recurrent state through feature-wise linear modulation. The temporal representation supplies both a dense prior and scale-specific modulation throughout the U-Net. A parametric extension jointly embeds the operating condition and sensor history, enabling reconstruction to adapt as the governing dynamics change with operating regime. ReMAIN is first benchmarked against SHRED on six one-dimensional nonlinear PDEs representing diverse dynamics. Across all benchmarks, it reduces reconstruction errors on unseen trajectories and more faithfully resolves sharp transitions, localized extrema and fine-scale variations. The parameter-conditioned model is then demonstrated on a collisionless $E \times B$ plasma subject to perpendicular axial electric and radial MAGNETic fields, with the electric-field strength serving as the operating parameter. ReMAIN reconstructs the high-dimensional, multiscale plasma state and recovers its regime-dependent spatiotemporal dynamics at electric-field strengths withheld from training. Together, ReMAIN improves sparse-sensor full-state reconstruction and, through parameter conditioning, generalizes across plasma operating regimes.
[abstract 43 / 54] (score: 2) - Title: Beam filamentation instability drives deuterium-tritium fusion with polarized neutron emissionAuthors: Guanqi Qiu, Deji Liu, Dongchi Cai, Ronghao Hu, Zheng Gong, Xueqing Yan,Comments:Subjects: physics.plasm-ph nucl-th physics.app-phCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
Filamentation instabilities are generally regarded as detrimental to fast-electron transport in fusion plasmas because they increase beam divergence and redistribute deposited energy. Here, we use two-dimensional particle-in-cell simulations coupled to a spin-dependent deuterium-tritium fusion module to investigate whether filamentation can instead transfer energy from counterstreaming electrons to prepolarized fusion ions. The simulations show that MAGNETic filaments, together with longitudinal inductive and transverse charge-separation electric fields, accelerate initially stationary deuterons and tritons to energies at which fusion reactions occur. Over the parameter range examined, the calculated neutron yield increases with the saturated MAGNETic-field energy. The model further predicts anisotropic, spin-resolved neutron emission. The direction of maximum neutron POLARIZATION is approximately perpendicular to the dominant deuterium-tritium collision direction and evolves with the angular distribution of the reacting ions. These results suggest that beam filamentation can couple RELATIVISTIC-electron energy to fusion ions and that polarized neutron emission may provide a reaction-weighted signature of the underlying plasma dynamics.
[abstract 44 / 54] (score: 2) - Title: Direct Numerical Comparison of Data Driving Strategies for Solar Flux Emergence in Magnetohydrodynamics: B-driving vs E-drivingAuthors: Kyriakos Christos Tapinou, Axel Raboonik, David I. Pontin, Michael S. Wheatland, Mark C. M. Cheung, Hannah Schunker,Comments: Accepted for publication in ApJSubjects: astro-ph.SR physics.plasm-phCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
Data driving is an important technique for modelling realistic MAGNETic field and plasma evolution in regions of the solar atmosphere where direct observations are either absent or insufficient. This technique uses observational data to drive the evolution of the simulation, while the modelled solar atmosphere evolves self-consistently. A common approach for data-driven simulations is B-driving, which uses the observed MAGNETic field at the surface of the Sun as a boundary condition. However, only prescribing B at the boundary does not generally determine its numerical evolution when the update depends on the reconstructed interface states or fluxes. To address this, E-driving provides an alternative approach by instead driving the simulation using the electric field on the boundary, which directly controls the MAGNETic field update. We systematically quantify the performance of B- and E-driving in a controlled set of numerical experiments. We test both methods in the Athena++ solver using (a) an analytical flux-emergence model (Y. Fan & S. Gibson 2003) and (b) a "ground-truth" reference simulation (S. Toriumi & S. Takasao 2017; S. Toriumi et al. 2020) of active region emergence. For E-driving, the electric field is incorporated into Athena++'s constrained-transport (CT) update, preserving the discrete solenoidal constraint. We assess the reproduction of (i) boundary MAGNETic flux, (ii) relative MAGNETic helicity, (iii) total and free MAGNETic energy, and (iv) MAGNETic morphology. Across these diagnostics, E-driving gives better overall reproduction of the reference evolution than B-driving. For the configurations considered in an Eulerian CT scheme, E-driving is more accurate than the commonly used ghost-cell B-driving strategies and simpler than constructing an update-consistent B-driving boundary condition.
[abstract 45 / 54] (score: 2) - Title: Testing Extra-Dimensional Gravitational-Wave Polarizations with Compact-Binary ObservationsAuthors: Hai-Tian Wang, Dicong Liang, Lijing Shao, Yu-Xiao Liu,Comments: 12 pages, 2 figures, 3 tablesSubjects: gr-qc astro-ph.HECreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
Extra spatial dimensions arise naturally in theories beyond four-dimensional general relativity (GR), but direct observational evidence remains elusive. Gravitational waves offer a distinctive probe: geometric projection onto the observable three-dimensional spatial subspace can produce apparent tensor, vector, and scalar POLARIZATIONs. We consider one additional spatial dimension and a two-mode tensor-wave ansatz for which the projected POLARIZATION components are fixed linear combinations of the same two underlying GR tensor waveforms. These components enter the measured strain through the standard detector antenna patterns. A frequency-domain Bayesian analysis of five compact-binary events constrains two rotation angles for two noncommuting orderings of rotations that preserve propagation within the observed subspace. Two events are further analyzed for four orderings that allow propagation to tilt into the extra dimension. For GW250114, the maximum GR quantiles among the tested rotation orderings are $Q_{\mathrm{GR}}\simeq0.6\%$ for the two-angle fits and $Q^{\mathrm{marg}}_{\mathrm{GR}}\simeq4.6\%$ for the three-angle fits after marginalizing over the third angle. Across the full event sample, the GR reference point lies inside the estimated 90% highest-posterior-density region in every case.
[abstract 46 / 54] (score: 2) - Title: WEST advanced wall protection achievements toward long pulse operationAuthors: R. Mitteau, M. H. Aumeunier, L. Dubus, J. Gerardin, V. Gorse, E. Grelier, V. Moncada, S. Vives, X. Litaudon, M. Jakubowski, J. Fellinger,Comments:Subjects: physics.plasm-phCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
Long pulse operation in MAGNETic fusion devices requires well controlled plasma power exhaust to the divertor \& wall, and avoidance of wall hot spots that could evolve in wall damage. At WEST, 10 major plasma facing components are monitored using 10 series of temperature/power indicators, based on multiple diagnostic systems, among which the infrared viewing system is especially relevant. These indicators span from the most basic ones (temperatures, power and energy from deterministic models) to advanced processes using artificial intelligence acquired through machine learning. Some advanced processes do operate in real time, and feedback on power actuators through the plasma control system, providing active control toward remaining within the safe operational domain. Other advanced processes intervene as forensic tools post discharge to identify possible dangerous situations regarding the power loading to the wall, so that the discharge run plan is adjusted to avoid running into aggravating wall events. No critical wall power event happened during the campaigns C9 to C11 (2024-2025), totalling about 13h of plasma, that would have affected the campaign plan. While it cannot be demonstrated that the active \& intelligent wall protection enabled the new plasma duration record of 1337 seconds, the wall protection system as a whole plausibly contributed to obtaining these record durations by preventing wall hot spots to become critical during the campaigns.
[abstract 47 / 54] (score: 2) - Title: Compressional heating above 1 keV on the LM26 MAGNETized target fusion machineAuthors: S. J. Howard, D. Krotez, P. Carle, J. Sanchez Rojo, R. Underwood, A. Froese, M. Reynolds, N. Sirmas, K. Conquergood, K. Epp, P. Forysinski, D. Plant, R. Zindler, E. Love, D. P. Brennan, N. Kumar, C. MacDonald, A. Wong, W. Zawalski, B. Rablah, W. Kozicki, C. Preston, A. Lee, X. Feng, M. Schellenberg-Beaver, R. Tingley, J. Gorenstein, V. Suponitsky, Z. Seifollahi Moghadam, D. Froese, E. Cessford, J. Pratt, J. Crofts, J. Sardari, G. Faust, D. Ross, J. Wilkie, S. Bernard, C. Connor, S. Bolanos, C. Gutjahr, E. Chan, C. Eyrich, A. Mahoney, M. Davidson, M. Laberge,Comments:Subjects: physics.plasm-phCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
The LM26 device has achieved a peak electron temperature of $T_e = 1180 \pm 65$ eV as measured by filtered X-ray diodes, supported by adjacent Thomson scattering measurements of $T_e = 1090 \pm 40$ eV, with a deuterium ion temperature of $T_i = 459 \pm 33$ eV as inferred from neutron yield. LM26 compresses a spherical tokamak plasma inside an initially 1.76 m diameter solid lithium liner imploded by theta-pinch coils. Radial compression by a factor of 2.75 increases $T_e$ over fivefold, while $T_i$ increases as much as twofold. The integrated observation of MAGNETic flux compression, electron heating, ion heating, and neutron production in a MAGNETized plasma compressed by a large lithium liner is an important milestone for MAGNETized target fusion
[abstract 48 / 54] (score: 2) - Title: FHiVI$^{2}$: A Fast High-Voltage approach for Ionisation Improvement in the context of plasma-assisted MAGNETron sputteringAuthors: R. Jean-Marie-Desiree, L. De Poucques, S. Cuynet,Comments: 12 pages, 12 figuresSubjects: physics.plasm-phCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
Ionisation control remains a key challenge in plasma-assisted processes and more particularly in MAGNETron sputtering. In this context, the former directly governs species transport and thin-film properties. Although HiPIMS substantially enhances the ionisation rate of sputtered species, its performance remains constrained by the coupling between sputtering and ionisation, which limits discharge tunability. Here, we introduce Fast High Voltage for Ionisation Improvement (FHiVI$^{2}$), a new transient electrical regime designed to improve the ionisation rate without requiring additional elements. By applying an ad hoc very short, high-voltage pulse during plasma sputtering processes, FHiVI$^{2}$ regime is expected to induce a strongly anisotropic electric-field burst intended to enhance sputtered metallic species ionisation while limiting back-attraction losses and sputtering. To assess the ionising potential of this regime, optical emission spectroscopy together with mass spectrometry were carried out. More particularly, mass spectrometry measurements show an improvement of the ionisation rate by a factor of 2.7 compared with the HiPIMS regime, for an applied voltage of 2 kV which correspond to an additional mean power of only 1.2 W, using a 2-inch tungsten target. These findings suggest that FHiVI$^{2}$ provides a flexible route towards improved ionisation control in MAGNETron sputtering and opens new perspectives for plasma-assisted processes.
[abstract 49 / 54] (score: 2) - Title: Gravitational radiation from a photon on the light ring: multipole fluxes and the logarithmic divergenceAuthors: Enrico Barausse,Comments: 12 pages, 2 figures. Companion repository at github.com/enricobarausse/photon-lightring-fluxesSubjects: gr-qcCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
A massless particle on the circular null geodesic of a Schwarzschild or Kerr BLACK HOLE radiates gravitational waves at all multipoles $\ell$ with a power that falls off only as $1/\ell$, so that the total instantaneous power is logarithmically divergent. We derive this result analytically from the Zerilli--Regge--Wheeler and Teukolsky equations with a null stress-energy tensor as source, and find that both the power radiated to infinity and the power absorbed by the horizon approach $\dot{E}_\ell\to g(a) κE^2/(M^2\ell)$, where $E$ is the energy of the particle, $M$ the mass of the BLACK HOLE and $a$ its spin, with $κ=0.063653$ and a spin factor $g(a)$, for which we obtain, for any spin, the closed form $g=27M^2(r_0-M)/[r_0^2(r_0+3M)]$ in terms of the radius $r_0$ of the Kerr light ring. The $1/\ell$ behavior has two causes: the near-resonance of the photon with the quasinormal modes, which prevents any exponential suppression at large $\ell$, and a cancellation in the source that is specific to massless particles, which reduces the power per multipole by a factor $\ell^2$ with respect to a generic source. At leading order half of the radiation falls into the BLACK HOLE, and we compute the first correction to this equal split in the non-spinning case. The same analysis describes massive particles on orbits close to the light ring, where the mass turns the $1/\ell$ law into an exponential cut-off. We recover the dominant, even-parity term of the geodesic SYNCHROTRON radiation formulae for massive particles of Breuer, Ruffini, Tiomno and Vishveshwara (1973), but we find that their odd-parity term is too small by a factor of four. All results are checked against numerical solutions, up to $\ell=12800$ in Schwarzschild and $\ell=800$ in Kerr.
[abstract 50 / 54] (score: 2) - Title: Minimal-Length Corrections to Hyperon Polarization in Rotating Quark Gluon PlasmaAuthors: Behnam Pourhassan, Sameer Ahmad Mir,Comments: 15 pages, 3 figuresSubjects: hep-phCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
Hyperon POLARIZATION in RELATIVISTIC heavy-ion collisions sensitively probes thermal vorticity and the operator structure of local equilibrium. We investigate an isotropic generalized uncertainty principle (GUP) via a spin-independent scalar deformation of the one-particle phase-space density of states in the local rest frame (LRF). We employ the Belinfante-Rosenfeld local-equilibrium operator, the standard on-shell dispersion relation, and the Pauli-Lubanski/axial-Wigner representation of the spin-$1/2$ observable, retaining terms linear in the GUP coefficient and in hydrodynamic gradients. The same scalar GUP factor appears in the scalar and axial phase-space contributions and cancels from the local mean-spin ratio at fixed spacetime point and momentum. Thus, the leading GUP contribution to an experimentally relevant POLARIZATION observable arises through the Cooper-Frye freeze-out integrals and can be expressed as a covariance between the LRF momentum invariant and the local spin kernel. This cancellation is a consequence of the scalar density-of-states modification within a fixed pseudogauge and does not imply pseudogauge independence of the POLARIZATION observable. For $Λ$ hyperons, a Maxwell-Boltzmann thermal estimate shows that the dependence on freeze-out temperature and fluid-dynamical correlations is substantially larger than the FERMI-Dirac correction, which remains negligible over the temperature range considered. Present LHC precision corresponds only to a formal linear sensitivity of order $10$-$30~\mathrm{GeV}^{-2}$. Since this interval lies beyond the domain in which the linear GUP expansion is reliable, no exclusion limit is inferred. Differential measurements of hyperon POLARIZATION as functions of momentum, rapidity, collision centrality, and azimuthal harmonic structure provide the most direct experimental avenue for testing the predicted covariance dependence.
[abstract 51 / 54] (score: 2) - Title: Autocorrelation in BLACK HOLE flare movies: Departures from KerrAuthors: Fang-Stars Wei, Zelin Zhang, Zhenyu Zhang, Bin Chen,Comments: 8 pages, 3 figuresSubjects: astro-ph.HE gr-qcCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
Autocorrelation in BLACK HOLE movies encodes the time delays and angular separations between gravitationally lensed images, offering a means of testing the spacetime geometry. Using an orbiting hot spot in the parametrized Johannsen-Psaltis metric with a single deformation parameter, we investigate the ability of lensing-induced correlations to distinguish departures from Kerr. From ray-traced movies, we extract the slope (k) and intercept (b) of an approximately linear secondary ridge in the time-angle autocorrelation map as potential future observables. Variations in the spin and the metric deformation parameter produce distinctive trajectories in the (k,b) plane, allowing the two observables to jointly constrain both parameters when the orbital radius, observer inclination, and orbital angular velocity are specified. By varying the orbital angular velocity, we construct a Kerr reference region in the (k,b) plane, and we find that, for some low-spin configurations with negative deformation parameters, the measured slope-intercept pairs of the secondary peaks lie outside this reference region. This feature appears for sub-Keplerian, Keplerian, and super-Keplerian motion, indicating that secondary-ridge measurements from BLACK HOLE flare movies have the potential to distinguish non-Kerr signatures.
[abstract 52 / 54] (score: 2) - Title: Evidence for orbital eccentricity supports a hierarchical origin for GW231123Authors: Baoxiang Wang, Tao Yang, Zhoujian Cao, Bin Hu, Xikai Shan, Rong-Gen Cai,Comments: 12 pages, 7 figures, comments welcomeSubjects: astro-ph.HE gr-qcCreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
GW231123 is the most massive binary BLACK HOLE merger observed to date and one of the most intriguing hierarchical merger candidates in the pair-instability mass gap. Its exceptionally large inferred component spins and remarkably short in-band duration make the source highly sensitive to waveform physics near merger. Here we show that GW231123 is better described as an eccentric binary black-hole merger. We analyse data over 11--448 Hz using the eccentric, spin-precessing effective-one-body waveform model TEOBResumS--Dalí, accounting for detector calibration uncertainty. We measure $e_{5.5\,\mathrm{Hz}}=0.34^{+0.12}_{-0.23}$ at 90\% credibility and obtain a Bayes factor of 10.2 in favour of the eccentric model over its quasi-circular counterpart. GW231123-like injection--recovery studies further show that analyses starting at 20 Hz, as in previous studies, can obscure this eccentricity. Including eccentricity substantially changes the spin inference, weakening the preference for a near-extremal secondary spin and lowering its posterior median to $a_2\simeq0.7$, close to the characteristic spin expected for a black-hole merger remnant. These results provide a coherent dynamical interpretation of GW231123, in which residual eccentricity, a mass-gap BLACK HOLE, and a remnant-like spin arise naturally from a hierarchical merger channel in a dense environment.
[abstract 53 / 54] (score: 2) - Title: ACORN I. Massive Black Hole Seeding and Tidal Disruption Events from Star Clusters in Cosmological SimulationsAuthors: Yihao Zhou, Tiziana Di Matteo, Claire E. Williams, Aklant Kumar Bhowmick, Marta Reina-Campos, Carl L. Rodriguez, Elena González Prieto, Laura Blecha, Rupert Croft,Comments: 32 pages, 24 figures. Comments are welcome!Subjects: astro-ph.GA astro-ph.HECreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
JWST has revealed massive star clusters at $z\gtrsim 6$, which provide promising environments for massive BLACK HOLE (MBH) seed formation. We introduce a new MBH seeding model for cosmological simulations, physically motivated by the runaway collisions in star clusters. Subgrid star clusters are generated according to the local ISM and evolved through stellar evolution and two-body relaxation. The masses of MBH seeds formed through runaway collisions are determined by the properties of their host clusters, including the effects of metallicity-dependent stellar winds. We further follow tidal disruption events (TDEs) with the evolving clusters, which can be enhanced in MBH binaries, and account for gravitational-wave (GW) recoil following MBH mergers. We implement this model in a constrained simulation of a 5$σ$ overdense region, where seeds of $10^{3}-10^{5.6}\,M_\odot$ form in clusters with $10^{4}\leq m_{\rm SC}\leq 10^{8}\,M_\odot$. Because both the seed abundance and mass are directly connected to the local environment, we have a more physical $M_{\rm BH}\!-\!M_{\rm galaxy}$ scaling for low-mass galaxies ($M_{\rm galaxy}\sim10^{6-9}\,M_\odot$), a regime poorly described by previous seeding models. Multiple MBHs are naturally allowed to form in-situ within individual halos, producing a spatially clustered population. This increases the MBH merger rate by $\sim100$ relative to other seeding models, significantly enhancing the expected LISA event rate. TDEs can dominate the growth of $10^{3-4}\,M_\odot$ MBHs and produce luminous flares of $L_{\rm peak}\sim 10^{42-43}\,{\rm erg\,s^{-1}}$, increasing the observability of low-mass seeds. This seeding prescription accelerates early MBH growth at $z\gtrsim 8$, while subsequent self-regulated gas accretion drives the central MBH toward similar masses $\sim10^{8.6}\, M_\odot$ by $z=6$ across different seeding models.
[abstract 54 / 54] (score: 2) - Title: Listening to the Horizon: Probing Near-Horizon Reflectivity with GW250114Authors: R. Prasad, Subhodeep Sarkar, Sudipta Sarkar,Comments:Subjects: gr-qc astro-ph.HECreated: 2026-10-08; Updated: 2026-10-09; Datestamp: 2026-10-09
Testing the horizon properties of astrophysical BLACK HOLEs is a central goal of gravitational-wave astronomy. The recently identified Direct Wave (DW), a prompt non-quasinormal component of GW250114, provides a new probe of near-horizon physics. While it remains unclear whether the DW itself carries horizon information, we show that it enables a novel null test of horizon reflectivity. If the remnant is an exotic compact object (ECO) with a partially reflecting surface, inward plunge radiation is reflected and leaks back through the gravitational potential barrier, producing a delayed DW echo whose amplitude is set by the surface reflectivity ($|\mathcal{R}_s|$). We construct the corresponding echo template, normalized by the observed DW, and search for it in quasinormal-mode-filtered data. We find no evidence for an echo ($\ln\mathcal{B}=-2.9$) and obtain the 90\% credible bound $|\mathcal{R}_s|<0.06$, corresponding to a reflected energy fraction below $0.4\%$, for surfaces from $0.1\, M_f$ to a Planck length from the would-be horizon. Our method thus turns the prompt ringdown signal into a direct test of horizon reflectivity.
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