Current date: 2026-10-02
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Created/updated limit: 2026-09-25 (7 days ago)
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Scoring abstracts
Number of records retrieved: 947
Keyword score statistics
score 11 -- 1 abstracts
score 10 -- 1 abstracts
score 8 -- 2 abstracts
score 7 -- 1 abstracts
score 6 -- 3 abstracts
score 5 -- 4 abstracts
score 4 -- 5 abstracts
score 3 -- 8 abstracts
score 2 -- 14 abstracts
in total -- 39 abstracts
Articles that appeared on 2026-10-02
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[abstract 1 / 39] Wow! (score: 11)
- Title: Search for Anisotropic Pair Halos Associated with Blazar JetsAuthors: Ao Zhang, Wenlei Chen, Manel Errando,Comments: Accepted for publication in JCAP. Minor revisions addedSubjects: astro-ph.HECreated: 2026-09-30; Updated: 2026-10-02; Datestamp: 2026-10-02
The origin of intergalactic MAGNETic fields (IGMFs) remains one of the key open questions in cosmology. Gamma-ray pair halos produced by electroMAGNETic cascades from TeV-emitting BLAZARs provide a powerful indirect probe of these fields. In this work, we present a novel search for pair halos that explicitly exploits their expected anisotropic morphology, aligning with the projected orientation of BLAZAR JETs on the sky. Using a Monte Carlo framework to model the spatial distribution of cascade emission, we identify an optimal sample of 21 high-SYNCHROTRON-peaked BL Lac objects with well-constrained JET position angles from radio interferometry. By rotating and stacking \textit{FERMI}-LAT observations of these sources along their JET directions, we enhance sensitivity to anisotropic extended emission that would be diluted in traditional orientation-agnostic analyses. Applying a likelihood analysis to the combined dataset, we find evidence for a non-zero IGMF, excluding the null hypothesis at $3.8σ$ level and obtaining a best-fit field strength of $B_0 = 2.8 \times 10^{-16}\,\mathrm{G}$, with a $99\%$ confidence interval of $0.9 \times 10^{-16}\,\mathrm{G} < B_0 < 8.9 \times 10^{-16}\,\mathrm{G}$. Our result is consistent with previous constraints from spectral, spatial, and temporal studies, while demonstrating that incorporating anisotropic information provides a significant gain in sensitivity. This approach opens a new avenue for probing intergalactic MAGNETism and highlights the potential of future high-angular-resolution gamma-ray observations to directly image pair halos and map MAGNETic fields in cosmic voids.
[abstract 2 / 39] Wow! (score: 10) - Title: 25 Years of Mrk 421 with XMM-Newton: Unveiling Structured Jets and Energy-Dependent EscapeAuthors: Tek P. Adhikari, Gopal Bhatta, Sangeetha Kizhakkekalam, Navaneeth P K, Alex Markowitz, Zhicheng He, Santanu Mondal,Comments: 26 pages, 10 figures, submittedSubjects: astro-ph.HE astro-ph.GACreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
We present a long-term X-ray spectral and timing analysis of the TeV BLAZAR Mrk~421 based on nearly a quarter century of archival \textit{XMM-Newton}/pn observations obtained between 2000 and 2025. Our sample comprises 76 epochs obtained with the pn instrument in both IMAGING and TIMING modes, allowing us to trace the source's variability and spectral evolution. Mrk~421 exhibits flux variations by approximately an order of magnitude, with prominent flaring periods interspersed with low-activity states. A clear harder-when-brighter trend is observed, accompanied by scatter in the hardness ratio (HR), suggesting flux alone does not uniquely determine the spectral state. Fractional variability in the hard band ($2-10$ keV) correlates tightly with that in the soft band ($0.3-2$ keV), with a steeper slope indicating pronounced variability at higher energies. The flux distribution is non-Gaussian and lognormal-like, dominated by moderate flux levels with a tail of bright flares. Spectral analysis shows that power-law model is not sufficient; 59 epochs are best described by a broken power-law (BPL) and 17 by a log-parabola (LP). This fluctuation between BPL and LP models suggests the emission region transitions between a distinct acceleration shockfront and downstream stochastic turbulence. The spectral break energy of BPL remains predominantly clustered around $2$ keV across all flux states, while the average spectral steepening above the break is mild ($ΔΓ\approx 0.19$), inconsistent with standard one-zone cooling models. Our results support structured JET scenarios or energy-dependent electron escape, providing key constraints on the long-term behavior of RELATIVISTIC JETs in high-SYNCHROTRON-peaked BLAZARs.
[abstract 3 / 39] Wow! (score: 8) - Title: Unveiling Multimessenger Emission from Hidden Cores of MicroQUASARsAuthors: Yu-Jia Wei, Kohta Murase, B. Theodore Zhang,Comments: 30 pages, 11 figures, 6 tables; accepted for publication in ApJSubjects: astro-ph.HECreated: 2026-09-30; Updated: 2026-10-02; Datestamp: 2026-10-02
MicroQUASARs are radio-emitting X-ray binaries with RELATIVISTIC JETs and are established sources of $\sim 100$~TeV gamma rays, making them promising candidates for cosmic-ray acceleration. Motivated by recent detections of $\sim 100~$TeV photons from Cygnus~X-1 and multi-PeV photons from Cygnus~X-3, we employ the Astrophysical Multimessenger Emission Simulator (AMES) to model their multimessenger emission from radio to ultrahigh-energy gamma rays. Our modeling suggests that particle acceleration is extremely efficient in the JET region. The observed $\gtrsim 0.1$~PeV gamma rays can originate from either $pγ$ or $pp$ interactions, depending on the location and physical conditions of the emission region, while also reproducing the lower-energy spectra. These configurations yield observationally testable predictions. In the poorly constrained $0.1$-$10$~TeV band, the models predict either a deep valley, a mild suppression, or a power-law spectrum. Additionally, models involving compact emission regions comparable to the orbital separation predict strong variability, while those invoking more extended and static external zones show more stable behavior. We also provide a possible qualitative explanation for the energy-dependent modulation patterns, relying primarily on changes in the Doppler factor and external $γγ$ absorption. In particular, explaining the PeV emission from Cygnus~X-3 favors a compact emission region, for which a MAGNETic field strength of order $10^2~\mathrm{G}$ is required. Finally, after accounting for pion and muon cooling, the predicted neutrino flux is suppressed, implying that detection is more challenging than previously thought.
[abstract 4 / 39] Wow! (score: 8) - Title: Ring Position Angles and Spin in M87* and Sgr A*Authors: Nicholas S. Conroy, Michi Bauböck, Vadim Bernshteyn, Paul Tiede, Abhishek V. Joshi, Cora Prather, Charles F. Gammie,Comments: Published in the Open Journal of Astrophysics (15 pages, 9 figures, 1 table)Subjects: astro-ph.HECreated: 2026-09-30; Updated: 2026-10-02; Datestamp: 2026-10-02
Event Horizon Telescope (EHT) images of BLACK HOLEs appear as rings with a brightness asymmetry. Here, we expand on our previous study of the asymmetry magnitude $a_1$ to study the position angle of the peak brightness asymmetry $\mathrm{PA}_1$ in general RELATIVISTIC MAGNETohydrodynamic (GRMHD) models. For larger spin magnitudes ($a_{*}>0$ and $a_{*}\lesssim-0.5$), the mean $\mathrm{PA}_1$ falls within $1σ$ of the approaching limb of the BLACK HOLE, regardless of viewing inclination, disk MAGNETization, or source. By comparing the $(a_1, \mathrm{PA}_1)$ distribution in M87* observations with models, we demonstrate that we can mildly disfavor low-magnitude spins and strongly disfavor all spin vectors that point toward Earth. The alignment of $\mathrm{PA}_1$ relative to the large-scale JET axis may suggest that M87*'s disk does not have a large tilt. By combining $\mathrm{PA}_1$ with the pattern speed measured in optimistic 2026 M87* video conditions, the EHT can constrain whether M87* is prograde or retrograde with $\sim 84\%$ accuracy. In Sgr A*, we show that a detection of $(a_1, \mathrm{PA}_1)$ could constrain the magnitude and direction of the galactic center spin vector. Finally, if future EHT expansions increase the sample of horizon-scale sources, a simple set of observables (ring diameter, asymmetry magnitude, and asymmetry angle) could enable robust constraints on BLACK HOLE mass, spin, and inclination.
[abstract 5 / 39] Wow! (score: 7) - Title: The Impact of a Clumpy Ambient Medium on the Dynamics and Synchrotron Emission of AGN JetsAuthors: Ivan Almeida, Christian Fendt, Bhargav Vaidya,Comments: 19 pages, 13 figures, accepted for publication in MNRASSubjects: astro-ph.HE astro-ph.GACreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
Relativistic JETs from AGN are expected to propagate through an inhomogeneous ISM, but the role of small-scale gas inhomogeneities in shaping their early evolution remains uncertain. We investigate this problem using 3D special-RELATIVISTIC MAGNETohydrodynamic simulations with PLUTO, following a JET with a Lorentz factor of 10 propagating through a pc-scale medium. We compare a homogeneous ambient medium with two clumpy ambient-medium models, motivated by dense gas in the nuclear ISM, in which clouds occupy volume filling factors of $0.1$ and $1$ per cent. We compute synthetic SYNCHROTRON maps and spectra from Lagrangian macro-particles that have been accelerated by diffusive shock acceleration. Jet-cloud interactions deflect the flow, enhance shock formation, and produce a more asymmetric cocoon than in the homogeneous ISM case. Altogether, this results in a substantially stronger mass loading: the entrained mass increases from $0.43$ M$_{\odot}$ in the homogeneous run to $5.3$ and $8.8$ M$_{\odot}$ in the clumpy runs. The clumpy ISM also modifies the turbulence and the material mixing within the JET cocoon. The dynamical differences we find translate into brighter and more irregular SYNCHROTRON emission. For the same injected JET, the models with a clumpy medium produce stronger frequency-integrated SYNCHROTRON emission than the homogeneous run, with the largest differences in the SED occurring from the sub-mm to the infrared/optical bands. Our results demonstrate that including a small-scale ISM structure provides a more complete description of the early dynamical evolution of young AGN JETs and their radiative properties.
[abstract 6 / 39] Yes (score: 6) - Title: X-ray Through Radio Observations and Modeling of the Soft X-ray Flash GRB 250419AAuthors: Genevieve Schroeder, Anna Y. Q. Ho, Gavin P. Lamb, Tanmoy Laskar, Daniel A. Perley, Ore Gottlieb, Tomas Ahumada, Igor Andreoni, Aleksandra Bochenek, Michael Bremer, Michael Camilo, Jonathan Carney, S. Bradley Cenko, Alessandra Corsi, Michael W. Coughlin, James Freeburn, Erica Hammerstein, Rahul Jayaraman, Mansi M. Kasliwal, Noel Klingler, Brendan O'Connor, Cassie Sevilla, Gokul P. Srinivasaragavan, Robert Stein, Jada L. Vail, Sylvain Veilleux, Lin Yan,Comments: 30 pages, 10 figures, submitted to ApJSubjects: astro-ph.HECreated: 2026-09-30; Updated: 2026-10-02; Datestamp: 2026-10-02
Soft X-ray flashes (XRFs) are predicted from a variety of hypothesized phenomena, including "dirty fireballs" (RELATIVISTIC JETs with significant baryon loading), and GAMMA-RAY BURSTs viewed marginally off-axis. For a given burst, detailed multiwavelength observations are necessary for distinguishing between possible progenitor scenarios, but the number of XRFs with such data remains small. Here we present X-ray, optical, and radio (mm to cm) data of GRB 250419A, an XRF (with peak energy $E_p<4\,$keV) discovered by the Space-based multi-band astronomical Variable Objects Monitor. We observe a clear achromatic break in the X-ray and optical bands, and likely two spectral components in the radio emission. The afterglow is similar to the long-duration GAMMA-RAY BURST population, but slightly underluminous, and the optical afterglow has an unusually shallow decay phase at $\lesssim2\,$d. We find that the event is well explained by a high-Lorentz factor JET with low kinetic energy ($E\sim10^{49}$-$10^{50}\,$erg), with energy injection that could arise from radial stratification and/or the JET being viewed marginally off-axis. We conclude that at least some X-ray flashes are an extension of classical GAMMA-RAY BURSTs down to lower energies.
[abstract 7 / 39] Yes (score: 6) - Title: Eight Gamma-Ray Bursts Observed with the FERMI Gamma-ray Burst Monitor: Significant Quasi-Thermal Components and Conditional Jet ConstraintsAuthors: Ze-lian Du, Zhao-Yang Peng, Jia-Ming Chen, Yue Yin, Ting Li,Comments: 23 pages, 8 figures, 6 tables,accepted for publication in ApJSubjects: astro-ph.HECreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
The composition of GAMMA-RAY BURST (GRB) JETs remains uncertain. We analyze eight FERMI Gamma-ray Burst Monitor (GBM) GRBs with reported redshift information, selected from 126 events by prespecified fluence and spectral criteria. After excluding compound-model DIC evaluations classified as unstable by the posterior-stability tests, a stable added-blackbody (BB) comparison gives $Δ\mathrm{DIC}>10$ in 203 of 215 accepted bins (60--100\% per burst); independently, a multicolor-blackbody plus power-law (mBB+PL) decomposition gives $F_{\rm mBB}/F_{\rm tot}>0.5$ in 214 of 215 bins. The cutoff-power-law (CPL)--mBB correlations ($r=0.83$ and 0.78) exceed the Band--mBB correlations ($r=0.41$ and 0.48), demonstrating model dependence. Time-integrated BB fractions span 0.005--0.311, with six of eight below 0.12. We then apply the non-dissipative photosphere prescriptions of \citet{2013A&A...551A.124H} (H2013) and \citet{2015ApJ...801..103G} (G2015). After excluding boundary or physically inadmissible inversions, the H2013 numbers with $ε_{\rm Th}>0.5$ are 1/2, 1/4, and 2/8 among valid solutions at $R_0=21$, 100, and 1000~km, respectively; the corresponding G2015 numbers with $σ_0<1$ are 0/1, 1/4, and 1/8. The large number of invalid solutions at small $R_0$ (six and seven at 21~km for H2013 and G2015) is itself evidence that those assumed radii are incompatible with the adopted inversion for most events. Among bursts having valid solutions at more than one radius, increasing $R_0$ generally lowers $ε_{\rm Th}$ and raises $σ_0$. Thus launch radius, efficiency, and spectral decomposition dominate the conditional JET constraints; no universal JET class or unique non-thermal mechanism is inferred.
[abstract 8 / 39] Yes (score: 6) - Title: Disk-Like Matter Outflow from a Kerr-Type Wormhole: Possible Observational Manifestations and Magnetic EffectsAuthors: Mikhail Piotrovich, Stanislava Buliga, Tinatin Natsvlishvili,Comments: 18 pages, 5 figuresSubjects: astro-ph.HECreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
We present a phenomenological study of a hypothetical compact object with a traversable 2 Kerr-type WORMHOLE geometry connecting two asymptotically distinct regions. One mouth of the WORMHOLE is assumed to reside in an ACTIVE GALACTIC NUCLEus (AGN) environment with ongoing accretion, while the second mouth is located in a comparatively quiescent galactic nucleus without accretion activity. In such a configuration, matter accreted near the AGN-side mouth may traverse the WORMHOLE throat and emerge from the opposite mouth. Because the inflowing matter possesses angular momentum, the resulting outflow is expected to be predominantly equatorial, producing a disk-like structure fundamentally different from a conventional accretion disk around a BLACK HOLE. Several dynamical regimes are considered depending on the outflow velocity relative to the local escape and orbital velocities. Possible observational manifestations, thermal properties, recombination signatures, and MAGNETic field effects are discussed. Special attention is given to the possibility of JET formation in the absence of a conventional accretion disk. We explicitly distinguish the weak-field, large-radius Newtonian classification used for the outer flow from the strong-field region near the throat, where the dynamics should be treated in a general-RELATIVISTIC and MAGNETohydrodynamic framework. We further discuss the specific energy and angular momentum inherited from the inner edge of the accretion flow, the possible modification of these quantities by MAGNETic stresses and energy-extraction processes, and the effects of an intrinsic dipolar MAGNETic field of the WORMHOLE.
[abstract 9 / 39] Yes (score: 5) - Title: Extension of a multi-region free-surface MHD solver beyond the inductionless approximationAuthors: Min Ki Jung, Brian Wynne, Francisco Saenz, Yufan Xu, Jabir Al-Salami, Yong-Su Na, Egemen Kolemen,Comments:Subjects: physics.comp-ph physics.plasm-phCreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
Free-surface liquid metal flows are a leading candidate for the plasma-facing components of future fusion reactors, but existing transient, three-dimensional, free-surface MHD solvers rely on the inductionless approximation, in which the induced MAGNETic field is neglected. This paper extends the open-source solver FreeMHD [B. Wynne et al., Phys. Plasmas 32, 013907 (2025)] beyond that approximation, resolving the induced field self-consistently with a vector-potential formulation that enforces $\nabla\cdot\boldsymbol{B}=0$ by construction while preserving the original multi-region, two-phase framework. It is verified against the analytical Shercliff and Hunt duct flows, against flows driven by a time-varying applied field, and against the deformation of a free liquid metal JET crossing a non-uniform field, and validated against free-surface height measurements from the LMX-U experiment. The experiment validates the overall free-surface solution rather than finite-$R_m$ effects, which the transient-field cases verify. To our knowledge this is the first open-source, fully three-dimensional free-surface liquid metal solver to resolve the evolution of the induced MAGNETic field, providing a basis for modeling the finite MAGNETic Reynolds number conditions expected in large-scale, transient fusion events.
[abstract 10 / 39] Yes (score: 5) - Title: Relativistic outflows power a quasi-periodic eruption: constraints on energetics, mass loss, and emission mechanismsAuthors: Joheen Chakraborty, Erin Kara, Wenbin Lu, Brian D. Metzger, Peter Kosec, Riccardo Arcodia, Itai Linial, Olivia Aspegren, Ehud Behar, Sudip Bhattacharyya, Margherita Giustini, Lorena Hernandez-Garcia, Daniel Kasen, Giovanni Miniutti, Frits Paerels, Erwan Quintin, Claudio Ricci, Daniele Rogantini, Paula Sanchez-Saez, Fatima Zaidouni,Comments: Final version accepted to ApJ LettersSubjects: astro-ph.HE astro-ph.GACreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
Quasi-periodic eruptions (QPEs) are recurring bursts of X-ray radiation originating from supermassive BLACK HOLEs (SMBHs). They are an unprecedented type of structured, high-amplitude SMBH variability, but the physical origins of their regularity, timescales, energetics, and emission are uncertain. We present new XMM-Newton observations of the QPEs in ZTF19acnskyy/"Ansky", constituting the deepest observations of individual bursts in any source thus far. The X-ray spectra reveal time-evolving P Cygni profiles comprising blueshifted absorption and redshifted emission from L-shell transitions of Fe XIX-XXIV, with column densities $N_H\sim 10^{22-23}$ cm$^{-2}$ and bulk velocities of $|v_w/c|\sim 0.2$, indicating RELATIVISTIC mass ejections during each eruption. We construct a time-dependent analytical model of a wind turning on to self-consistently compute its evolving luminosity and ionization properties, and find that the light curve and spectral lines can be simultaneously produced by a wide-angle outflow with $\dot{M}\sim 10^{-9}-10^{-8}\,M_\odot$ s$^{-1}$ kinetically powering the X-rays with an efficiency of $L_X/\dot{E}_K\sim 0.1$. For a covering fraction $f_Ω\sim0.5$, each eruption ejects $\sim 10^{-3}\,M_\odot$ and $\gtrsim 10^{49}$ erg of kinetic energy, setting an upper bound on the QPE lifetime of $\lesssim1000$ bursts if the underlying mass reservoir is $\sim1 M_\odot$, and implying that the bursts may result in detectable multiwavelength signatures of reverberation and feedback. These measurements provide new quantitative constraints on QPE energetics, emission mechanisms, and the mass/energy they recycle into their circumnuclear environments, as well as an observational probe for direct comparison with physical models and hydrodynamical simulations of QPEs.
[abstract 11 / 39] Yes (score: 5) - Title: AT2018hyz: Predictions for a Sky Projection from a Delayed Off-Axis JetAuthors: Ranadeep Ghosh Dastidar, Paul C Duffell,Comments: 10 Pages of manuscript without references, with 6 figures including one schematic diagramSubjects: astro-ph.HECreated: 2026-09-30; Updated: 2026-10-02; Datestamp: 2026-10-02
Initially discovered optically, Tidal Disruption Event (TDE) AT2018hyz was first detected in radio 972 days later. The continued monitoring of the event revealed a late-time (1370-2160 days) radio brightening. The source for this radio brightening has been associated with an afterglow originating from an off-axis JET or a delayed mildly RELATIVISTIC outflow. In this work, we explored the conditions required for a delayed off-axis JET to explain the observed radio brightening. We find that the combined effect of different delay times (t_delay) and observer angles (theta_obs) can produce radio afterglow, as observed for AT2018hyz. The further off-axis from the JET core an observer is, the shorter is the delay inferred between the optical disruption and launching of the JET. This presents a degeneracy between different theta_obs and tdelay. We estimate the sky projection of the JET for these different combinations to break this degeneracy. The spread in sky images ranges from 0.6 mas for a 30 deg off-axis observer to 0.3 mas for an observer perpendicular to the JET core. Future VLBI observations should be able resolve these structures. Thus a combined observation of the light curve and sky images for AT2018hyz (and other JETted TDEs) can be used to narrow down the observer angle and any delay in launching of the underlying JET.
[abstract 12 / 39] Yes (score: 5) - Title: Slingshot on compact binaries in the nuclear region of galaxies as the origin of large offset GAMMA-RAY BURSTsAuthors: Juan C. Rodríguez-Ramírez, Viviane Alfradique, Clécio R. Bom, Davi C. Rodrigues,Comments: 21 pages, 12 figuresSubjects: astro-ph.HECreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
A growing number of GAMMA-RAY BURSTs (GRBs) have been observed at large projected offsets from the centres of their putative host galaxies, sometimes extending to several tens of kiloparsecs. When the GRB is associated with a kilonova, a compact binary with at least one neutron star is expected to be involved, and the cause of the offset can be attributed to the neutron star natal kick. In this work, we explore an alternative mechanism: the gravitational scattering of compact binaries populating the nuclear region of the host galaxy, by an intermediate-mass BLACK HOLE or secondary supermassive BLACK HOLE. We specifically consider populations of neutron star-neutron star (NS-NS), neutron star-BLACK HOLE (NS-BH), and neutron star-white dwarf (NS-WD) binaries, and analyse the ejection of bound systems from the nuclear region through a gravitational-slingshot effect. We proceed analytically to derive the conditions for binary survival and to parametrise the post-encounter velocity. To quantify the associated merger offsets, we numerically integrate the post-slingshot trajectory of the binary centre-of-mass in host-galaxy potentials that include the primary SMBH, the stellar component, and the dark-matter halo, considering both elliptical-like and spiral-like galaxy profiles. Our parameter sampling shows that NS-NS and NS-WD binaries typically merge farther from the galactic centre than NS-BH systems, with approximately 30-45% of successful ejections merging at three-dimensional distances exceeding 100 kpc; these extreme-offset mergers occur within $\sim$0.1-10 Gyr after ejection. These results motivate the analysed mechanism as a candidate channel for observed extreme-offset transients.
[abstract 13 / 39] Yes (score: 4) - Title: The impact of RELATIVISTIC AGN JETs on realistic galaxy cluster environmentsAuthors: K. Hervella-Seoane, M. Perucho, S. Planelles, J. M. Martí, V. Quilis,Comments: Accepted in Astronomy & AstrophysicsSubjects: astro-ph.GA astro-ph.HECreated: 2026-09-30; Updated: 2026-10-02; Datestamp: 2026-10-02
Context. Low-power FRI-like radio JETs dominate the AGN population, yet the main mechanism of heating the intracluster medium (ICM) and its efficiency remain a matter of debate. Aims. We investigate the impact of intermediate-power FRI-like RELATIVISTIC JETs on the inner region of realistic ICM, focusing on the role of weak shocks on heating and the environmental coupling in regulating energy deposition. Methods. We present six three-dimensional RELATIVISTIC-hydrodynamic simulations of (1e44 - 1e45) erg/s FRI-like JETs propagating through the central regions of realistic ICM environments extracted from cosmological GADGET-3 runs. Each simulation tracks 20 Myr of continuous JET activity with radiative cooling included. Results. Despite their intermediate power and mildly RELATIVISTIC speed at injection, they decelerate rapidly to trans-sonic velocities (average Mach numbers ~ 2.3) and generate weak bow shocks that dominate the energy transfer. Approximately, 80% of the injected kinetic power is converted into internal energy of the ambient ICM, and bremsstrahlung cooling noticeably reduces the temperature of the shocked shells as they expand. Conclusions. Our results demonstrate that heating of the intergalactic and intracluster medium is highly efficient even in the case of weak shocks in FRI-like sources. This finding suggests low-power JETs are a viable solution to the long-standing cooling-flow problem and likely regulate STAR FORMATION across diverse galaxy cluster environments.
[abstract 14 / 39] Yes (score: 4) - Title: The X-ray and optical emission of the intermediate polar SWIFT J0614.0+1709Authors: Nikita Rawat, Domitilla De Martino, David A. H. Buckley, Koji Mukai, Martina Veresvarska, Zackery A. Irving, Simone Scaringi, Nicola Masetti,Comments: 16 pages, 10 figures, accepted for publication in A&ASubjects: astro-ph.HECreated: 2026-09-30; Updated: 2026-10-02; Datestamp: 2026-10-02
We present the first detailed X-ray and optical study of the intermediate polar SWIFT J0614.0+1709 based on a pointed XMM-Newton observation complemented by long-term optical photometry from TESS. A strong coherent modulation at the white dwarf spin period was detected in X-rays, with a period of $\sim$1411 s, confirming the MAGNETic nature of the system. The X-ray spin pulse exhibits a pronounced energy dependence, with the modulation amplitude decreasing towards higher energies, consistent with phase-dependent absorption in the accretion flow. Phase-resolved spectroscopy further shows that the spin variability is primarily driven by changes in the covering fraction of the partial-covering absorber. The broadband X-ray spectrum is well described by a partially absorbed thermal plasma model with a temperature of $\sim$12 keV and a soft blackbody component at $\sim$63 eV. The inferred bolometric luminosity of $\sim$5$\times$10$^{34}$ erg s$^{-1}$ places the source among the more luminous intermediate polars. The TESS observations reveal substantial sector-to-sector variability in the relative strengths of the orbital and spin modulations. While the spin signal remains persistently dominant, the beat modulation varies significantly and disappears entirely in one Sector, suggesting temporal changes in the contribution of the reprocessing region(s). The orbital and, to a lesser extent, spin modulation amplitudes show some tendency to be stronger during brighter optical states, suggesting that changes in the mass transfer rate may influence the optical emission and modulation amplitudes. Overall, SWIFT J0614.0+1709 is a comparatively X-ray luminous intermediate polar exhibiting complex optical variability characterised by changes in pulse morphology and recurrent brightening events, making it a valuable target for future simultaneous optical and X-ray studies.
[abstract 15 / 39] Yes (score: 4) - Title: Normal-Field Evolution and the Breakdown of Classical Tearing in Current SheetsAuthors: Grzegorz Kowal, Diego A. Falceta-Gonçalves,Comments: 13 pages, 3 figures. Submitted to Physical Review ESubjects: physics.plasm-ph physics.space-phCreated: 2026-09-30; Updated: 2026-10-02; Datestamp: 2026-10-02
Classical resistive tearing theory assumes a prescribed current-sheet equilibrium, but a finite normal MAGNETic field can evolve the background on the tearing timescale. For a transversely pressure-balanced Harris profile of initial half-thickness $a$ and asymptotic RECONNECTing-field magnitude $B_0$, threaded by uniform $B_n$ ($ξ=B_n/B_0$), we derive an exact evolution in ideal MAGNETohydrodynamics: counter-propagating Alfvenic fronts broaden the neutral layer and generate a central sheet-parallel flow with shear at its flanks. Inner-layer estimates recover $ξ_{\mathrm{crit}}\sim S^{-3/4}$ for breakdown of the classical resistive balance, where $S$ is the Lundquist number based on $a$. Numerical frozen-profile calculations show loss of central resistive dominance and decreasing tearing growth as the neutral layer expands. Eigenfunction comparisons at fixed wavenumber and predominantly Doppler-shifted propagation support a normal-field-modified continuation of classical tearing. The normal field supplies no net perturbation energy. Energy extraction from the RECONNECTing-field gradient weakens as the sheet broadens. The velocity-gradient contribution becomes comparable when the neutral-layer width approaches the initial sheet thickness, without reversing the decline in growth. For $S=10^6$, $\mathrm{Pr}_m=0$, and $ξ=10^{-4}$, the maximum growth rate falls by a factor of about ten from its initial value at neutral-layer half-width $w\simeq1.59a$, where the growth and broadening times become equal. Only about 0.18 additional upper-envelope e-folds are estimated between this crossing and $w/a=2$, where the growth rate is about 25 times smaller than its initial value. These results support dynamical suppression of further linear amplification over the sampled evolution, even though the instantaneous spectrum remains unstable.
[abstract 16 / 39] Yes (score: 4) - Title: High-energy neutrinos from shocked circumnuclear material around optically-bright and infrared-only tidal disruption eventsAuthors: Mainak Mukhopadhyay, Shigeo S. Kimura, Tatsuya Matsumoto,Comments: 23 pages, 11 figuresSubjects: astro-ph.HE hep-phCreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
Tidal disruption events (TDEs) can launch sub-RELATIVISTIC outflows that drive shocks into the surrounding circumnuclear material (CNM), providing a natural site for COSMIC RAY (CR) acceleration and high-energy neutrino production through hadronuclear ($pp$) interactions. We model this emission for optically bright and infrared (IR)-only TDEs, the latter motivated by a recently identified population of luminous IR transients with weak or absent optical counterparts, consistent with TDEs embedded in dusty, obscured nuclear environments. We semi-analytically compute the shock dynamics, CR acceleration and transport, and neutrino production, including the radiative cooling and compression in dense environments. While optical TDEs remain inefficient $pp$ neutrino sources with comparatively small neutrino yields, radiative compression in dense IR-only TDEs enhances the target density and allows the pp efficiency to approach the calorimetric regime, yielding up to $\sim 10\%$ of the observed diffuse neutrino flux at $100$ TeV, given the rate uncertainties. The long-lasting neutrino emission and low individual source yield motivate joint electroMAGNETically informed stacking searches. We forecast such searches for IceCube, IceCube-Gen2, KM3NeT, and HUNT, and conclude that a future $\sim 30\ {\rm km^3}$ neutrino observatory can reach $3σ$ sensitivity for nearby ($z \lesssim 0.4$) IR-only TDEs with multi-year search windows. Growing optical and IR TDE samples can therefore enable population-resolved searches that can test whether dense, obscured nuclear environments are efficient high-energy neutrino sources.
[abstract 17 / 39] Yes (score: 4) - Title: A New Framework for Modeling Solar Flares from MHD to Kinetic ProcessesAuthors: Joel C. Allred, Graham S. Kerr, Silvina E. Guidoni, Joel T. Dahlin, Marc Swisdak, Judith T. Karpen, Valeriy Tenishev,Comments: 21 pages, 12 figures, accepted for publication by Astrophysical JournalSubjects: astro-ph.SRCreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
Physical processes in solar flares span many orders of magnitude in spatiotemporal scales, so a single unified model accounting for all relevant processes remains computationally intractable. Instead, specialized codes have been developed, targeting specific domains that tackle specific aspects of the solar flare problem. Here, we present a comprehensive framework that links three models to capture flare initiation and energy release, the subsequent particle acceleration, the propagation and thermalization of those particles, and ultimately the heating of the lower solar atmosphere. We use the 2.5D ARMS MAGNETohydrodynamics (MHD) code to model stressing of the MAGNETic field in a simulated active region, the formation of a current sheet, MAGNETic RECONNECTion, and the evolution of newly formed flare loops. We use the conditions in the ARMS' current sheet to initialize the kglobal model, which predicts time-dependent nonthermal electron and proton distributions. Finally, we use RADYN+FP to inject these distributions into a newly RECONNECTed ARMS loop and compute subsequent particle transport, atmospheric heating, and radiative emissions. This is the first detailed presentation of a RADYN+FP simulation tracking nonthermal electrons and protons in the same loop. As well as discussing the interesting physics that takes place, we note how this results in white-light flare emission height consistent with observations. This work is a first step toward building a fully 3D flare modeling framework.
[abstract 18 / 39] (score: 3) - Title: Gravitational wave detectability range informed by external messengersAuthors: S. Ronchini, A. Chopra, T. Dal Canton, B. Banerjee, A. L. De Santis, M. Branchesi,Comments:Subjects: astro-ph.HE gr-qcCreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
A rapid estimate of gravitational-wave (GW) detectability associated with astronomical transients is crucial for optimizing multi-messenger follow-up strategies and for constraining the physical origin of the transient itself. We introduce here the Targeted Detectability Range (TDR), designed to evaluate, with minimal computational effort, the detectability of compact binary coalescences under the hypothesis of association with an external messenger, such as an electroMAGNETic or neutrino signal. Unlike the standard GW range, which is based on averaged source parameters, the TDR incorporates prior information from observations of the external messenger, including sky localization, inclination constraints, and physically motivated bounds on component masses. We report the TDR of all short- and long-duration GAMMA-RAY BURSTs, observed during the first three observing runs of Advanced LIGO and Advanced Virgo. The method is validated by performing a systematic comparison with the 90$\%$ exclusion distances provided by modeled targeted GW searches. In the absence of a coincident detection by all-sky, all-time GW searches, the TDR provides a rapid and quantitative constraint on a possible merger origin of the astrophysical source. Its low-latency implementation and public availability would enable timely prioritization of follow-up observations and optimized allocation of observational resources, with direct impact on the physical interpretation of astronomical transients.
[abstract 19 / 39] (score: 3) - Title: Three New Likely Spider Millisecond Pulsar Binaries and Optical Kinematic Tracers of Intrabinary ShocksAuthors: Jay Strader, Rebecca Kyer, Laura Chomiuk, Elias Aydi, Peter Craig, Thomas M. Do, Isabella Molina, Teresa Panurach, Subhroja Roy, Kirill V. Sokolovsky, Samuel J. Swihart, Ryan Urquhart,Comments: MNRAS in pressSubjects: astro-ph.HECreated: 2026-09-30; Updated: 2026-10-02; Datestamp: 2026-10-02
We report the discovery of three candidate spider millisecond pulsars via multi-wavelength follow-up of unassociated FERMI Large Area Telescope gamma-ray sources. All have optical spectroscopy from the SOAR 4.1-m telescope and X-ray data from SWIFT. Two optical/X-ray sources are exceptionally strong redback candidates, sitting close to the centres of the localization ellipses of the gamma-ray sources 4FGL J1020.4-5314 and 4FGL J1408.7-3747. We show that both optical sources are spectroscopic binaries with orbital periods (0.15-0.3 d) and mass functions (0.6-0.9 Msun) typical for redbacks. 4FGL J1020.4-5314 shows bright, very broad (full width at half maximum 2100 km/s) H-alpha emission in all spectra obtained over two years. Remarkably, the H-alpha radial velocities are offset in phase from the absorption-line velocities of the secondary, and match the signal expected for an emission source near the primary. This demonstrates, for the first time for any spider, that the H-alpha emission can be associated with an intrabinary shock that wraps around the pulsar, opening up the possibility of using optical emission lines as kinematic tracers of the intrabinary shock in some redbacks. A third candidate spider is less secure in its association with the gamma-ray source 4FGL J1429.8-0739, but has unusual properties, including a 30.5-hour orbital period, a potential subgiant secondary, and a high X-ray luminosity, making it worthy of further investigation.
[abstract 20 / 39] (score: 3) - Title: Rapid Vacuum Response Calculations for Non-axisymmetric Plasma GeometriesAuthors: Jacob Halpern, Nikolas Logan, Carolin Nührenberg, Elizabeth Paul, Carlos Paz-Soldan,Comments: 13 pages, 4 figuresSubjects: physics.plasm-phCreated: 2026-09-30; Updated: 2026-10-02; Datestamp: 2026-10-02
We present a fast, open-source calculation of the vacuum response matrix and surface inductance in non-axisymmetric geometries capable of running with up to 10^5 boundary points in tens of seconds on a laptop. Ideal MAGNETo-hydrodynamic (MHD) stability modeling for free boundary modes requires the perturbed vacuum energy. We extend the VACUUM code to non-axisymmetric geometries in the new Julia implementation of the Generalized Perturbed Equilibrium Code, combining a collocation approach to the boundary integral equations with a high-order singularity correction scheme. The correction is recast into explicit quadrature weights acting on the collocation values, which allows the corrected operator to be assembled explicitly rather than applied to a given surface field, and the structure of that matrix under field-period and stellarator symmetry is then exploited to reduce storage and solve cost. We find that the vacuum response matrix converges at fourth order or greater in the grid spacing, reaching a given accuracy on a coarser grid than previous implementations without the high-order method. The non-axisymmetric calculation converges to the axisymmetric VACUUM result for a tokamak and the CAS3D result for a W7-X stellarator equilibrium. This work enables fast free boundary ideal MHD stability and perturbed equilibrium calculations in stellarators.
[abstract 21 / 39] (score: 3) - Title: Early Emergence of SSS emission in RS OphAuthors: J. -U. Ness, J. P. Osborne, M. Orio, S. Starrfield, S. Mitrani, E. Behar,Comments: Accepted for A&A, 12 pagesSubjects: astro-ph.HE astro-ph.SRCreated: 2026-09-30; Updated: 2026-10-02; Datestamp: 2026-10-02
Early in the 2006 outburst of the recurrent nova RS Oph, SWIFT detected the onset of the super-soft-source (SSS) phase. An XMM-Newton observation on day 26.1 revealed an unusual soft X-ray spectrum containing transient narrow emission features that could not be identified with known transitions and are atypical of SSS spectra. We analyse a new XMM-Newton observation obtained at a comparable stage of the 2021 outburst and compare it with spectra from other epochs and with similar novae. A blackbody model reproduces the low-resolution 2006 EPIC/pn spectrum but fails to describe the simultaneous high-resolution RGS data. The 2021 spectrum closely resembles that observed in 2006 and consists of a slowly fading shock component and a highly variable soft component containing several unidentified features. While the shock emission evolves on timescales of days, the soft component varies on hourly timescales and dominates the observed variability. Its properties resemble those of the novae V1494 Aql and V1716 Sco, but not those of the persistent SSS Cal 87. No significant 35-s periodicity is detected. The results demonstrate that low-resolution observations can miss the complex line-dominated emission revealed by high-resolution spectroscopy. The rapidly variable soft component, together with radiative recombination continua, Fe X emission, and the previously detected 35-s period, suggests the presence of a hidden photoionising source. We conclude that these enigmatic spectra form an intermediate class between the SSe and SSa categories of Ness et al. (2013), together with V1494 Aql and V1716 Sco. Future modelling will be required to determine the relative importance of photoionisation, charge exchange, and other processes in shaping this class of intermediate SSS spectra.
[abstract 22 / 39] (score: 3) - Title: Probing Accretion and Outflow in V1180 Cas through High-Resolution Optical SpectroscopyAuthors: Tarak Chand, Saurabh Sharma, Koshvendra Singh, Joe P. Ninan, Arpan Ghosh, Devendra K. Ojha, Jyotirmoy Dey, Manojit Chakraborty, Kartik Gokhe, Aayushi Verma, Mamta, Ajay Kumar Singh,Comments: Accepted for publication in the Journal of Astrophysics and Astronomy (JoAA), 17 pages with 5 figuresSubjects: astro-ph.SRCreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
We present an analysis of a high-resolution optical spectrum of V1180 Cas obtained with HIRES at the W. M. Keck Observatory during a bright photometric state of the source. The spectrum is dominated by strong emission lines, including H$α$, the Ca II infrared triplet, He I, and O I, along with numerous Fe I and Fe II transitions and several forbidden lines such as [O I] and [S II], indicating ongoing accretion and mass-loss activity. A weak Li I $λ$6708 absorption feature confirms the youth of the source. Using the Li I absorption and selected Fe I emission lines, we report for the first time a radial velocity of $-16 \pm 3$ km s$^{-1}$ for V1180 Cas. The H$α$ and H$β$ profiles exhibit asymmetric structures with blueshifted absorption components, suggesting outflowing material along the line of sight. The He I $λ$5876 line displays a narrow component likely associated with post-shock accretion regions and a broad, slightly blueshifted component probably arising from MAGNETospheric flows and/or inner disk winds. The [O I] $λ$6300 profile is decomposed into low- and high-velocity components, tracing a slow disk wind and a fast JET. Using the forbidden [O I] line, we estimate for the first time a disk inclination angle of $\approx50^\circ$. The derived mass accretion and JET mass-loss rates imply $\dot{M}_{JET}/\dot{M}_{acc} \sim 0.01$--$0.03$, at the lower end of, but consistent with, the range observed for Class II YSOs. Forbidden-line diagnostics indicate densities $\sim10^{3}$ and $10^{6}$ cm$^{-3}$ with temperatures of $\sim10^{4}$ K, supporting a multi-component outflow scenario. Overall, the results support a picture in which V1180 Cas is an actively accreting, moderately inclined system hosting a multi-component outflow.
[abstract 23 / 39] (score: 3) - Title: ElectroMAGNETic drift-kinetic particle-in-cell model with energy and charge conservation for studying finite-$β$ plasmasAuthors: O. P. Morozov, V. A. Kurshakov, I. V. Timofeev,Comments: 26 pages, 7 figures. Submitted to Journal of Computational PhysicsSubjects: physics.plasm-ph physics.comp-phCreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
The paper proposes a generalization of the fully implicit energy- and charge-conserving electroMAGNETic particle-in-cell method to the case where the lightest type of plasma particle (electrons) is described in the drift-kinetic approximation. This allows us to remove the very strict time step limitation of this method requiring to resolve the gyrorotation of electrons. Since the drift-kinetic model is only applicable to light particles whose contribution to plasma POLARIZATION is small, this model can be further simplified by neglecting the electron POLARIZATION drift and including in Maxwell's equations, in addition to the current of gyrocenters, only the MAGNETization current. In order for such a hybrid model to retain conservative properties in finite-difference form, a method of self-consistent interpolation of $\nabla B$ in the mirror force from grid to particle and the MAGNETization vector from particle to grid is proposed. Unlike existing drift-kinetic models, this model is not limited to considering small perturbations near a given equilibrium, and therefore allows one to study the formation of plasma equilibria in regimes with a finite ratio of plasma to MAGNETic field pressure. Testing of the parallel code implemented in C++ using the PETSc library confirmed the fulfillment of the finite-difference laws of energy and charge conservation, as well as the ability of the model (in the drift-kinetic version for all types of particles) to correctly reproduce the diaMAGNETic effect and longitudinal ion-acoustic wave.
[abstract 24 / 39] (score: 3) - Title: Detection of kilosecond hard lags in the new pulsating ULX candidate NGC 7456 ULX-1Authors: W. Leone, F. Pintore, C. Pinto, N. O. Pinciroli Vago, A. Sanna, A. Wolter, T. Di Salvo, R. Iaria, A. D'Aì, A. Anitra, R. Soria, P. Esposito, F. Barra, E. Ambrosi, S. Caserta, C. Salvaggio, R. Salvaterra, G. L. Israel, S. Banerjee, M. Marelli, G. Rodriguez-Castillo, L. Burderi,Comments: Accepted for publication, A&A, on 29/09/2026Subjects: astro-ph.HE astro-ph.GACreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
Context. Ultraluminous X-ray sources (ULXs) are thought to be powered, in many cases, by super-Eddington accretion onto compact objects. While soft X-ray lags have been detected in several ULXs, hard lags remain rare and poorly understood. Aims. We investigate the temporal and energy dependence of X-ray lags in NGC 7456 ULX-1 to constrain their physical origin and probe the super-Eddington accretion flow. Methods. We analyzed the two deepest XMM-Newton observations, taken in 2018 and 2023. Hard (1-10 keV) and soft (0.3-1 keV) light curves were cross-correlated using adaptive-binning techniques optimized for Poissonian low-count data. We measured lags over consecutive 10 ks intervals and investigated their energy dependence. Spectra were modeled using thermal and Comptonization models. Results. We detect significant hard X-ray lags in both observations, with the hard emission delayed by $\sim 10^3$ s during phases of rapid flux variability. The delays are primarily driven by the lowest-energy photons. Spectral modeling indicates a Comptonization-dominated flow comprising a cooler, extended outer region and a hotter, compact inner flow embedded in an optically thick wind. We interpret the delays as the combined effect of inward propagation of accretion-rate fluctuations and photon diffusion within the dense outflow. Fluctuations first enhance the soft-emitting outer regions and then propagate toward the hotter inner flow, where photons undergo stronger Comptonization before escaping with a kilosecond delay. The small inferred inner emitting radius disfavors an intermediate-mass BLACK HOLE accretor. Conclusions. The sign, amplitude, and energy dependence of the delays disfavor standard reverberation. Propagation-driven variability coupled with radiative transfer in optically thick winds appears to play a major role in shaping the timing properties of super-Eddington accretion flows.
[abstract 25 / 39] (score: 3) - Title: Constraining the density distribution of the cold Circumgalactic Medium of QUASARs at z>2 through Lya, HeII and Ha emissionAuthors: Andrea Travascio, Sebastiano Cantalupo, Titouan Lazeyras, Naveen A. Reddy, Charles C. Steidel, Yongming Liang, Gabriele Pezzulli, Massimo Gaspari, Matteo Fossati, Michele Fumagalli, Chiara Feruglio, Fabrizio Fiore, Huiyang Mao, Marta Galbiati, Weichen Wang, Nicolas Ledos, Bahram Mobasher, Antonio Pensabene, Giada Quadri,Comments: 21 pages, 15 figures, 6 tables in total, including an 8-page appendix with 9 figures and 5 tables. Submitted to A&A on 6 August 2026Subjects: astro-ph.GACreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
Extended Lya emission is routinely detected around high-redshift QUASARs, revealing large reservoirs of cool circumgalactic medium (CGM). Its resonant nature complicates interpretation of gas density, ionization state, and kinematics, making non-resonant tracers such as HeII and Ha essential. Extending previous analytical models, we use CLOUDY photo-ionization simulations to predict HeII/Ha in QUASAR-illuminated gas over a broad parameter range, including log-normal density distributions. The ratio constrains density fluctuations, commonly quantified by the clumping factor C. We compare the models with extended Lya, HeII, and Ha observations around QUASARs at z~2.1-4.5. At z~2.2, we observed 13 QUASARs with Keck/KCWI and targeted the systems with the most prominent extended Lya and HeII emission with Keck/MOSFIRE, providing the first statistical QUASAR-CGM sample with combined Lya, HeII, and Ha measurements. Within matched apertures out to ~35 pkpc, stacked spectra give Lya/Ha=9.1, HeII/Ha=0.54, and HeII/Lya=0.06. Single-density models require very high CGM densities (n>10 cm^-3) or implausibly soft AGN spectra to reproduce the low HeII/Ha ratio. Broad log-normal density distributions instead reproduce it at lower median densities but require a substantial emissivity-weighted high-density tail, corresponding formally to C~10^3-10^4 in our parameterization. We also analyze 26 VLT/MUSE QUASARs at 3.1
[abstract 26 / 39] (score: 2) - Title: Hadronic description of nuclear matter and neutron star propertiesAuthors: Yao Ma, Yong-Liang Ma, Jia-Ying Xiong,Comments: A major revision was made. A more systematic analysis was givenSubjects: nucl-th astro-ph.HECreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
The composition of the neutron star is one of the most fundamental and long-standing problems in nuclear- and astro-physics. The known properties of nuclear matter, together with the astronomical observations, impose the stringent and interconnected constraints on the theoretical descriptions. In this work, by using the most general quantum hadrodynamics model including $σ, ω, ρ$ and $a_0$ in addition to nucleons, and performing a Bayesian joint analysis of experimental nuclear matter data, the heavy-ion flow pressure, and astrophysical observations including the mass-radius inferences of PSR J0740+6620, PSR J0437$-$4715, PSR J0614$-$3329 and HESS J1731$-$347 and the tidal posterior of GW170817, we point out that the nuclear matter made of only hadrons can provide a unified description of nuclear matter properties and astrophysical observations.In addition, we find that the speed of sound in the GQHD develops a non-monotonic, peak-like structure which is absent in the Walecka-type models TM1, NL3 and FSU-$\delta6.7$. This soft-to-stiff transition, accompanied by a pronounced softening of the symmetry energy, results in small size intermediate mass neutron stars, $R_{1.4}\simeq (11.1-11.4)$~km, together with the maximum mass $(2.2-2.3)M_\odot$, and, to our knowledge, has not been found before in the Walecka-type RELATIVISTIC mean-field models. What we find here indicate that the sequential measurement of neutron star mass and radius by the next generation facilities, especially that of the intermediate mass neutron stars, is crucial for distinguishing the pure nucleonic stars from the hybrid ones.
[abstract 27 / 39] (score: 2) - Title: Real-Time Estimation of High-Resolution Flow Fields and Reduced-Order Coordinates from Event-Based Imaging VelocimetryAuthors: L. Franceschelli, E. Amico, C. E. Willert, M. Raiola, G. Cafiero, S. Discetti,Comments:Subjects: physics.flu-dynCreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
We propose a data-driven framework to estimate high-resolution (HR) velocity fields and reduced-order flow coordinates from real-time Event-Based Imaging Velocimetry (rt-EBIV). Fast event analysis first provides low-resolution (LR) velocity snapshots on a coarse grid. Offline, paired LR/HR fields are used to identify the LR-to-HR mapping and a linear dynamical model in a POD-based latent space. Online, each LR snapshot is projected onto the LR basis, the corresponding HR coordinates are estimated and temporally regularized, and the HR field is reconstructed from the retained POD modes. Three estimators are compared: a direct Kalman filter (KF), a linear stochastic estimator followed by Kalman filtering (LSE), and a variance-rescaled variant (LSE+VR). The method is tested on two turbulent flows acquired with pulsed EBIV: a submerged water JET and a channel flow over a square rib. All estimators outperform direct cubic interpolation of the LR fields, yielding more consistent HR reconstructions of instantaneous flow states, turbulent kinetic energy, spectra, reduced-order dynamics, and temporal coherence. LSE gives the lowest overall reconstruction error, while LSE+VR achieves similar errors with improved recovery of fluctuation energy and higher-order content. The direct KF is the most computationally efficient and provides the closest agreement with the HR reference in spectral analyses. Since most of the cost is associated with full-field HR reconstruction, the latent-coordinate estimation is negligible compared with LR processing. The framework allows deliberately coarse rt-EBIV processing to be combined with reduced-order refinement, extending real-time operation toward higher update rates while preserving richer and dynamically consistent HR flow representations for diagnostics and future observer-based flow-control applications.
[abstract 28 / 39] (score: 2) - Title: Quasinormal Modes of Reissner-Nordström Black Holes in Modified GravityAuthors: Xia-Tong Tan, Yu Zhang, Zhi-Hong Nie,Comments: 14 pages, 9 figures, 10 tablesSubjects: gr-qcCreated: 2026-09-30; Updated: 2026-10-02; Datestamp: 2026-10-02
In the framework of Scalar-Tensor-Vector Gravity (STVG), this paper investigates the quasinormal modes and time-domain evolution of Reissner-Nordström Modified Gravity (MOG) BLACK HOLEs under massless scalar, electroMAGNETic, and gravitational perturbations. Quasinormal frequencies are calculated by extending the 3rd- to 6th-order WKB method and combining it with Padé approximation to the 13th order, while complete time-domain waveforms are obtained using a finite-difference method based on light-cone coordinates. The results indicate that increasing the MOG parameter $α$ raises the effective mass of the BLACK HOLEs, leading to a decrease in the damping rate $|ω_I|$ and a slower ringdown decay. An increase in charge $Q$ produces a similar effect, with the damping approaching zero in the near-extremal limit. Regarding the ringdown decay times for the three types of perturbations, the gravitational field has the longest duration, the electroMAGNETic field is intermediate, and the scalar field is the shortest. The oscillations and decay observed in the time-domain waveforms are qualitatively consistent with the frequency-domain results, and the power-law exponent governing the late-time tail aligns with that of asymptotically flat spacetimes. This study provides a systematic theoretical reference for testing modified gravity theories using BLACK HOLE spectroscopy.
[abstract 29 / 39] (score: 2) - Title: NASA ASTRA White Paper : A Chandra Successor in the 2030sAuthors: C. S. Reynolds, E. Hodges-Kluck, E. A. Kara, M. Koss, K. Madsen, E. Miller, B. Williams, S. Allen, M. Bautz, K. Burdge, N. Cappelluti, B. Cenko, L. Corrales, A. Falcone, A. Foord, D. Haggard, L. Lopez, R. Mushotzky, A. Ptak, H. Russell, S. Safi-Harb, K. Stassun,Comments: 7 pages, submitted as a White Paper to NASA's ASTRA InitiativeSubjects: astro-ph.IM astro-ph.HECreated: 2026-09-30; Updated: 2026-10-02; Datestamp: 2026-10-02
Chandra established that soft X-ray spectral imaging with approximately 1 arcsec angular resolution is an essential tool for almost every area of astrophysics, from the early Universe to ice chemistry in protoplanetary disks. While Chandra continues to deliver groundbreaking science, it lacks the sensitivity to be the counterpart to JWST, Roman, Rubin, LISA, ngVLA, ALMA, IceCube, NewAthena, ELT, and other upcoming large facilities. Here we highlight the scientific potential of a Chandra successor with >10x higher sensitivity and >50x survey speed. While the scientific reach of such a mission is very broad, we showcase four high-priority science questions that require these capabilities -- How did supermassive BLACK HOLEs form?, How does stellar and AGN feedback work in galaxies?, How does high-energy stellar activity affect exoplanet atmospheres? and, How do BLACK HOLEs merge? A Chandra successor in the 2030s would also demonstrate the X-ray mirror technology for a future flagship and sustain the US high energy astrophysics workforce until that flagship launches. We outline the science-instrument trade space by sketching three missions based on the NASA Probe concept study report for the Advanced X-ray Imaging Satellite (AXIS): AXIS-Deep, AXIS-Classic, and AXIS-Fast, highlighting a breakthrough science case for each and listing others that drive the design.
[abstract 30 / 39] (score: 2) - Title: A Multi-Wavelength Picture of the Surprisingly Short 2024/25 Outburst from EXO 0748-676Authors: Amy H. Knight, Lauren Rhodes, Noel Castro Segura, Douglas J. K. Buisson, Aru Beri, David M. Russell, Kevin Alabarta, Maria C. Baglio, Jakob van den Eijnden, Matthew J. Middleton, Payaswini Saikia, Chris Done, Rob Fender, Fraser Lewis,Comments: 26 Pages, 9 Figures, Accepted for Publication in MNRASSubjects: astro-ph.HECreated: 2026-09-30; Updated: 2026-10-02; Datestamp: 2026-10-02
After sixteen years in quiescence, EXO 0748-676 unexpectedly returned to outburst in March 2024. However, in stark contrast to its previous outburst (1985 - 2008), EXO 0748-676 returned to quiescence in January 2025, after ~ 10 months in outburst. Here, we collate data from nine observing facilities, covering wavelengths from radio to X-ray, to provide the first multi-wavelength study of the 2024/25 outburst. Unlike the 1985 outburst, both the rise and decay are fully captured at X-ray and optical wavelengths. The light curves do not exhibit the hallmarks of a canonical transient low-mass X-ray binary outburst. Instead, the X-ray and optical fluxes remain reasonably stable during the 2024/25 outburst. The wealth of optical data of EXO 0748-676 reveals a skewed optical phase curve and an irradiation-dominated optical light curve which lasts until the onset of hydrogen recombination in the outer disc at ~11000K, triggering a rapid fade at the end of the outburst. X-ray observations by XMM-Newton and NICER revealed that EXO 0748-676 was heavily obscured early on, with spectra exhibiting a dampened soft X-ray contribution. We find that a spectral model including a clumpy, ionised absorber describes the obscuration, although the exact cause of the early-time obscuration remains uncertain. X-ray colour analysis indicates that EXO 0748-676 spent most of the ~10 month outburst in a faint, hard state. EXO 0748-676 increased marginally in brightness towards the end of the outburst, but never entered a soft spectral state. This behaviour is characteristic of a failed transition outburst.
[abstract 31 / 39] (score: 2) - Title: Teaching a plasma physics and engineering class at a liberal arts college using Course-Based Undergraduate Research Experiences (CUREs)Authors: Bhavesh Ramkorun,Comments:Subjects: physics.ed-ph physics.plasm-phCreated: 2026-09-30; Updated: 2026-10-02; Datestamp: 2026-10-02
Undergraduate research experiences provide students with an opportunity to apply knowledge learned in the classroom to authentic scientific problems. In this work, we describe the development of a special-topics course in Plasma Physics and Engineering (PPE) at a small liberal arts college using a Course-Based Undergraduate Research Experiences (CUREs). During the first half of the semester, students learned fundamental plasma physics and dusty plasma concepts through traditional lectures and homework. During the second half, they applied this knowledge to investigate an unanswered research question: why does the levitation time of growing nanoparticles decrease in the presence of a MAGNETic field? Students learned and used Langmuir probe and optical emission spectroscopy diagnostics to characterize an argon plasma over a range of MAGNETic-field strengths. Their measurements showed a general decrease in electron density with increasing MAGNETic field strength, while optical emission measurements confirmed a reduction in carbonaceous nanoparticle growth-cycle time from acetylene. Using the measured plasma parameters, students estimated the nanoparticle charge and developed the hypothesis that a reduction in electron density leads to a smaller negative dust charge and consequently a weaker electric force available to levitate the particles as a function of increasing MAGNETic field strength between 50 and 330 Gauss. Students subsequently disseminated their results through research poster presentations at conferences. Course evaluations and E-CLASS responses also indicated positive student experiences with the laboratory and research components of the course. This work demonstrates one approach for integrating plasma physics education and authentic research in an undergraduate curriculum at a small liberal arts institution.
[abstract 32 / 39] (score: 2) - Title: Transport Impacts of Resonant Island Chains in Fusion PlasmasAuthors: Sidney D. V. Williams, Kevin Mitchell, Ethan Custodio, Dmitri M. Orlov,Comments:Subjects: physics.plasm-ph nlin.CDCreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
Magnetic field-line transport in MAGNETically confined plasmas is commonly modeled as diffusion through stochastic MAGNETic layers generated by resonant perturbations. However, experimentally relevant MAGNETic configurations frequently exhibit transport rates that are substantially slower than predicted by fully stochastic models, indicating the presence of unresolved dynamical barriers. In this work, we investigate the role of nested resonant island chains and their associated invariant manifolds in regulating transport within the edge MAGNETic topology of DIII-D tokamak discharge #171491 subjected to strong n=3 resonant MAGNETic perturbations. Using field-line tracing, Poincare analysis, and manifold calculations, we identify a hierarchy of homoclinic and heteroclinic tangles associated with both period-one and period-ten hyperbolic points. A systematic construction based on primary intersection points is developed to extract partial transport barriers from the full manifold geometry and divide the chaotic region into dynamically distinct domains. Monte Carlo simulations reveal that field-line escape exhibits a bi-exponential character when only the outermost period-one boundary is considered, reflecting the presence of a long-lived "sticky" region associated with the period-ten island chain. When the inner period-ten boundary is explicitly incorporated into the Monte Carlo, the escape process becomes approximately single exponential and is accurately described by turnstile lobe transport. The measured escape rate agrees with predictions obtained from the turnstile lobe area and the symplectic structure of the field-line map. These results demonstrate that nested tangles provide a quantitative transport skeleton governing MAGNETic-field-line escape and establish a framework for analyzing transport barriers, cantori, and lobe dynamics in realistic fusion-plasma MAGNETic configurations.
[abstract 33 / 39] (score: 2) - Title: 1RXS J174320.1-042953: another polar with a red-shifted absorption component in emission line wingsAuthors: Diego H. González-Buitrago, Ma. T. García-Díaz, Sergey Zharikov, Gagik Tovmassian, A. Castro, E. J. Kotze, Yair Krongold, C. A. Negrete,Comments: 12 pages, 7 figures. Accepted for publication in Revista Mexicana de Astronomía y Astrofísica (RMxAA)Subjects: astro-ph.SR astro-ph.HECreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
We present the results of a spectroscopic and multi-band photometric study of the MAGNETic cataclysmic variable 1RXS J174320.1-042953. Multi-band photometry confirms a periodic modulation with an orbital period of $P_{\rm orb}=0.0864 \pm 0.0001$ days. Using the estimated secondary mass of $\sim0.15\,\mathrm{M_\odot}$ and, the X-ray-based white dwarf mass of $\sim0.75\,\mathrm{M_\odot}$, we obtain values of $q\sim0.2$ and a system inclination of $47^\circ\pm10^\circ$. The optical spectra of 1RXS J174320.1-042953 are dominated by strong, complex, asymmetric, and highly variable single-peaked emission lines of the Balmer series, \ion{He}{i}, and \ion{He}{ii}, which are characteristic of polar-type MAGNETic cataclysmic variables. Doppler tomography reveals no evidence of a Keplerian accretion disc, supporting the classification of the system as a polar. The H$β$ and \ion{He}{ii} emission lines can be decomposed into at least two distinct components. The low-velocity components have semi-amplitudes of approximately 170 km s$^{-1}$ (H$β$) and 147 km s$^{-1}$ (\ion{He}{ii}), while the high-velocity components reach about 317 km s$^{-1}$ and 460 km s$^{-1}$, respectively. The low-velocity component is likely associated with the irradiated side of the secondary star facing the white dwarf and/or the vicinity of the L$_1$ point, whereas the high-velocity component is related to the accretion-stream structure. A redshifted absorption component in the emission-line wings is detected at orbital phases near $ϕ\approx 0.0$, reaching velocities up to $\sim1400$ km s$^{-1}$ and likely produced by accretion-stream material crossing the line of sight.
[abstract 34 / 39] (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: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
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 35 / 39] (score: 2) - Title: Rational linear forms of linearizable ordinary differential equationsAuthors: Dmitry Lyakhov,Comments: 6 pagesSubjects: math.RA cs.SC nlin.SICreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
Every scalar ordinary differential equation of order at least three with rational right-hand side that is locally linearizable by a point transformation admits a linear form with rational coefficients over the same coefficient field. We prove this by restricting the derived symmetry algebra to a coordinate line and recovering a scalar differential operator from rational symmetry-JET data. The construction uses differential elimination and linear algebra; it does not require the symmetry generators or a linearizing transformation to be solved for. A single integer parameter suffices to choose the line.
[abstract 36 / 39] (score: 2) - Title: Solarprop 2.0: Modern charge-sign dependent solar modulation for everyoneAuthors: Henning Gast,Comments: 41 pages, 15 figures, comments welcome, associated source code available at https://github.com/henningrwth/solarprop2Subjects: astro-ph.SR astro-ph.HE astro-ph.IMCreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
I present a greatly improved version of SOLARPROP, an open source framework for building models of charge-sign dependent solar modulation of COSMIC RAYs in the heliosphere. The transport equation of charged particles is solved by converting it to a set of stochastic differential equations (SDEs). The code now includes the full set of SDEs in two spatial dimensions, allowing for MAGNETic fields with latitudinal components, and it has been generalized to accommodate models in three spatial dimensions. Due to code parallelization and optimization, a speedup of up to three orders of magnitude with respect to the original version is achieved. Python bindings have been added for ease of use. The code has been validated against the results of several model calculations found in the literature. While excellent agreement is found in many cases, important differences are observed for two model implementations. Possible root causes for the differences have been investigated.
[abstract 37 / 39] (score: 2) - Title: Resolving the physics of Quasar Ly$α$ Nebulae (RePhyNe): II. The dense and clumpy CGM of Quasars at $z \sim$ 3.5Authors: Titouan Lazeyras, Sebastiano Cantalupo, Andrea Travascio, Nicolas Ledos, Joop Schaye, Gabriele Pezzulli, Federico Baraggioni, Alessandro Lupi, Andrea V. Macciò, Marta Galbiati, Antonio Pensabene, Giada Quadri, Weichen Wang,Comments: 13 pages + 4 appendix pages, 7 + 6 figures, submitted to A&ASubjects: astro-ph.GACreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
The small scale density distribution of the cold circumgalactic medium (CGM) plays a central role in galaxy evolution, yet it is still poorly understood. We provide new constraints on the cold CGM density distribution by comparing the CGM emission from MUSE observations of QUASAR (QSO) nebulae at $z \sim 3.8$ with mock observations generated from the new DaLya simulation suite under the assumption of maximal fluorescence. These are further complemented by mock observations generated from the COLIBRE (m5 and m6 resolutions) and HELLO simulations. We first investigate the distribution of the observed and simulated Ly$α$ surface brightness (SB) values, which directly depend on the cold gas density distribution under our assumption, finding stark differences between observations and upper limits provided by simulations with the exception of the COLIBRE higher-resolution run (m5). The observations generally show a much larger covering fraction of regions with relatively large Ly$α$ SB values and suggest that densities reaching at least 10 cm$^{-3}$ must be present in the CGM of QSOs within a radial distance of 50 to 200 ckpc. To understand the origin of this discrepancy, we study the cold CGM density distribution finding in all cases simulated PDFs consistent with skewed lognormal ones with medians $\sim 10^{-2}$ cm$^{-3}$ and clumping factors between 16 and 102. We compare the broadness of these distributions to the one implied by the observed HeII/Ly$α$ CGM ratio, which is independent on the assumption of maximum fluorescence. Assuming lognormal PDFs with median values similar to the simulations, the observed ratio requires a broader PDF with a clumping factor at least 8 times larger than predicted by simulations. These results suggest that higher resolution and/or additional physical mechanisms are needed to reproduce the observed CGM of QSOs at these redshifts.
[abstract 38 / 39] (score: 2) - Title: Where Chaos Pauses: Sliding-Window Frequency Ratios Reveal Transient Resonances in Relativistic OrbitsAuthors: Wenfu Cao, Ying Wang, Hongsheng Zhang,Comments: 18 pages, 6 figuresSubjects: gr-qcCreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
A long-time Poincaré section flattens a chaotic orbit into one static blur, erasing the order in which the orbit visits its own local structures. We introduce the sliding-window frequency ratio (SWFR), built from nothing but radial and polar turning events, to recover that order along individual RELATIVISTIC orbits. Each window spans a fixed number of radial cycles and simply counts the polar events inside it; because event times are kept, any candidate interval can be sliced out and replotted as its own Poincaré section. No spectrum, no reference center, no basis functions. Integrable Kerr benchmarks recover the known frequency ratios, and for regular motion with uniformly bounded count deviations the counting-error bound falls off as $O(W^{-1})$. The same counts then pay off in chaos. In MAGNETized Kerr spacetime a single charged orbit dwells near $3/5$ and later near $4/7$, and exactly those intervals open into fivefold and sevenfold section structures; a second orbit dwells near $1/2$ with two lobes. In Schwarzschild--Melvin spacetime a photon holds $4/5$ across a fivefold pattern. In every case the section covers exactly the interval SWFR selected: integer counts and phase-space geometry agree that a globally chaotic orbit is paying a temporary visit to a resonance.
[abstract 39 / 39] (score: 2) - Title: From Simulation to Fabrication: Realizing Silicon Crystalline Undulators with Silicon Nitride Stressor Layer PatterningAuthors: L. Malagutti, L. Bandiera, F. Bonafè, N. Canale, D. De Salvador, P. Fedeli, V. Guidi, A. V. Korol, F. Mancarella, R. Negrello, Gianfranco Paternò, M. Romagnoni, F. Sgarbossa, A. V. Solov'yov, A. Sytov, D. Valzani, A. Mazzolari,Comments: 6 pages, 4 figuresSubjects: physics.acc-phCreated: 2026-10-01; Updated: 2026-10-02; Datestamp: 2026-10-02
A crystalline undulator is a crystal exhibiting periodic deformations that cause channeled particles to oscillate, generating coherent electroMAGNETic waves. In this study, stressor layer patterning has been employed to induce the desired deformations on a silicon substrate. Finite element method simulations were performed to optimize the geometric parameters of the undulator. The primary focus was on achieving sinusoidal deformation with sub-millimeter period and amplitude exceeding 1~nm, utilizing the silicon (110) plane for its superior channeling properties. Key parameters, such as substrate thickness and undulator period, were meticulously refined to ensure uniform deformation while minimizing the impact of higher harmonics, which could degrade performance. Based on the simulation results, a crystalline undulator, 160 $μ$m thick and consisting of 10 periods with a period length of 334 $μ$m, has been successfully fabricated. The final device demonstrates structural integrity and a uniform deformation extending up to 20 $μ$m from the surface. Specifically designed for use with 5-30 GeV particle beams, the undulator is capable of generating gamma photons in the 5-15 MeV range. This work effectively integrates advanced simulation techniques with precise fabrication methods, demonstrating the feasibility of crystalline undulators as high-performance devices for generating gamma radiation.
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