Current date: 2026-09-25
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Number of records retrieved: 840
Keyword score statistics
score 10 -- 1 abstracts
score 9 -- 1 abstracts
score 8 -- 2 abstracts
score 7 -- 3 abstracts
score 6 -- 2 abstracts
score 5 -- 7 abstracts
score 4 -- 5 abstracts
score 3 -- 7 abstracts
score 2 -- 27 abstracts
in total -- 55 abstracts
Articles that appeared on 2026-09-25
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[abstract 1 / 55] Wow! (score: 10)
- Title: A Helical Trajectory Interpretation of a Multi-wavelength Event in a Blazar S5 0716+714Authors: Zhihao Ouyang, Jingyu Wu, Hubing Xiao, Zhijian Luo, Zhu Chen, Shaohua Zhang, Liang Chen, Jianzhen Chen, Marina Manganaro, Luis C. Ho, Junhui Fan, Chenggang Shu,Comments: 22 pages, 8 figures,3 tablesSubjects: astro-ph.HECreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Relativistic JETs in BLAZARs exhibit strong variability across multiple timescales, but the connection between temporal variability and the evolution of JET structures remains poorly understood. In this work, we investigate the $γ$-ray variability of the BL Lac object S5 0716+714 from July 2014 to June 2015 and explore its possible connection with the parsec-scale JET evolution. We identify an escalating periodic oscillation (EPO) in the $γ$-ray light curve, characterized by a sequence of successive flux enhancements with progressively increasing temporal separations. Combining \textit{FERMI}-LAT data with contemporaneous 43 GHz Very Long Baseline Array (VLBA) observations, we find a temporal association between the EPO and the downstream propagation of a superluminal knot. A helical trajectory model simultaneously fitting the $γ$-ray variability and the two-dimensional VLBA component positions reproduces the observed flux modulation and component motion. These results suggest that geometric Doppler modulation caused by the changing viewing angle of a moving JET component provides a possible explanation for the observed EPO. This work provides a framework of connecting BLAZAR variability to the knot evolution of RELATIVISTIC JETs.
[abstract 2 / 55] Wow! (score: 9) - Title: Exceptional Gamma-Ray Flaring Activity of the Blazar S4 0954+65 in Early 2025Authors: Zhihao Ouyang, Jingyu Wu, Hubing Xiao, Lili Yang, Shangchun Xie, Shaohua Zhang, Zhijian Luo, Jianzhen Chen, Jianguo Wang, Mingjun Liu, Qinyu Wu, Huaqing Cheng, Wenda Zhang, Junhui Fan,Comments: 24 pages, 12 figures, 7 tables. Accepted by Astronomy & AstrophysicsSubjects: astro-ph.HE astro-ph.GACreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
S4 0954+65 (4FGL J0958.7+6534) is a TeV-detected BLAZAR at a redshift of $z = 0.3694 \pm 0.0011$, classified as an intermediate-SYNCHROTRON-peaked BL Lac object. In early 2025, it entered an exceptional $γ$-ray high state. We aim to investigate the origin and physical properties of the exceptional 2025 flare, and to constrain the emission processes responsible for this flaring activity. We performed a multi-wavelength analysis using $γ$-ray, X-ray, optical/UV, radio, and 43 GHz Very Long Baseline Array (VLBA) observations. We examined multi-band correlations with the z-transformed discrete correlation function (zDCF), analyzed the spectral evolution and parsec-scale JET kinematics, and modeled the broadband spectral energy distributions (SEDs). The $γ$-ray variations lead the optical and radio emission by 3.22 days and possibly 18.26 days, respectively, while no significant correlation is found between the $γ$-ray and X-ray emission. The $γ$-ray spectra show a harder-when-brighter behavior, consistent with enhanced particle acceleration during the active state. A similar spectral trend is also observed in the X-ray band, where the photon index is anti-correlated with flux. During the major $γ$-ray flare, VLBA images reveal the emergence of a new superluminal radio knot from the core, whose extrapolated ejection time is consistent with the peak of the $γ$-ray flare. The temporal and structural evolution during the 2025 flare is consistent with a shock-in-JET scenario, in which a newly emerging disturbance propagates downstream and drives the flare. Broadband SED modeling shows that a leptonic SYNCHROTRON self-Compton plus external Compton model with dusty torus seed photons reproduces the multi-wavelength observations with physically plausible parameters. A lepto-hadronic interpretation remains possible but requires substantially higher JET power.
[abstract 3 / 55] Wow! (score: 8) - Title: Gaussian Process Inference of Stochastic Magneto-Active Dynamics and Viscosity in SWIFT J1727.8-1613Authors: Lijuan Dong, Dahai Yan, Zihan Yang, Haiyun Zhang, lin Xie, Qingcui Bu, Lian Tao,Comments: 13 pages, 8 figures. Accepted for publication in Astronomy & AstrophysicsSubjects: astro-ph.HECreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Linking X-ray variability to the underlying MAGNETohydrodynamic (MHD) dynamics of BLACK HOLE X-ray binaries remains challenging. We systematically investigate the stochastic and oscillatory variability of the BLACK HOLE X-ray binary candidate SWIFT J1727.8$-$1613 during its 2023 outburst using Gaussian process (GP) regression applied to Insight-HXMT multi-band light curves. The variability is modeled with a physically motivated composite kernel comprising one stochastically driven damped simple harmonic oscillator (SHO) and two damped random walk (DRW) components. The SHO term robustly recovers quasi-periodic oscillations (QPOs) with frequencies $ν_0 \sim 0.07$--$5$ Hz, consistent with the fundamental Alfvén mode of a contracting MAGNETically confined disk--coronal cavity. The quality factor rises from $Q \sim 3$ to $Q \sim 10$, suggesting increasing coherence of the MAGNETic cavity. We also find an anti-correlation between QPO frequency and the short DRW damping timescale, supporting our proposed stochastic MAGNETo-active dynamics scenario. Associating the short and long DRW timescales with the local turbulent turnover and thermal adjustment timescales, respectively, we infer an effective viscosity parameter of $α\approx 0.1$, supporting a strongly MAGNETized accretion flow. Strikingly, near the onset of RELATIVISTIC JET ejection around MJD 60206, both relaxation timescales collapse toward the 0.1 s sampling limit, suggesting a rapid reorganization of the disk internal energy balance immediately before JET launching. Our results establish GP inference as a powerful route to connecting X-ray timing observables with the dynamical state of BLACK HOLE accretion flows.
[abstract 4 / 55] Wow! (score: 8) - Title: Anisotropy and energy distribution of leptons and photons in radiative RELATIVISTIC Alfvénic turbulenceAuthors: Peng Liu, Xiaochun Wei, Zheng Gong,Comments: Published in Physical Review DSubjects: physics.plasm-ph astro-ph.HECreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
The anisotropic evolution of RELATIVISTIC particles in MAGNETically dominated Alfvénic turbulence is a fundamental process governing nonthermal emissions in high-energy astrophysical environments. In this work, we develop a theoretical framework by deriving scaling equations that characterize the pitch-angle dynamics of leptons and photons across both weak- and strong-radiative cooling regimes. Our model reveals a universal coupling between particle energy and angular distribution, arising from the interplay of field-aligned accelerations, perpendicular drift motions, and radiation reactions. The model can uniquely identify ``turning-point energies" that exhibit a nonlinear dependence on the local MAGNETic field and the energy-injection scale. The validity of this scaling model is confirmed through radiative particle-in-cell simulations. We show that the electron pitch-angle distribution fundamentally dictates photon emission characteristics, further revealing a pronounced statistical correlation between high-energy photon emission and turbulent vortices in the RECONNECTion regions. By bridging the gap between small-scale kinetic interactions and broad-band spectral characteristics, this work provides a quantitative basis for interpreting the hardening of radiation spectra and complex POLARIZATION signatures in sources such as pulsar wind nebulae and GAMMA-RAY BURSTs.
[abstract 5 / 55] Wow! (score: 7) - Title: The impact of flickering variability and MAGNETisation on the dynamics, stability and morphology of radio-loud AGN JETsAuthors: Emma L. Elley, James H. Matthews, Henry Whitehead, Alex J. Cooper,Comments: AcceptedSubjects: astro-ph.HE astro-ph.GACreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
The physics governing the morphology of radio-loud AGN JETs is not fully understood. We investigate how MAGNETization, flickering JET power and their interplay affects the morphology of RADIO GALAXies. We present a grid of RELATIVISTIC MAGNETohydrodynamic simulations using the PLUTO code covering constant and variable JETs with two levels of MAGNETisation. We find that the constant high MAGNETisation JETs can lead to highly asymmetrical cocoon morphologies, whilst the variable high MAGNETisation JET can exhibit a broken morphology, caused by a discontinuous JET beam. Our work highlights the importance of MAGNETisation and variability on the stability and resulting morphology of radio-loud AGN JETs, suggesting both are significant factors in addition to JET power or environment. Furthermore, we show that the interaction between MAGNETisation and variability can lead to the development of localised kink instabilities along the JET beam. Finally, we discuss the effects of hydrodynamic mixing in low MAGNETisation JETs and the role of viewing angle dependence in comparisons between our simulations and observed sources. To facilitate this comparison we present a library of simulated radio images at different times in the simulations and from various viewing angles, which highlight a diverse set of complex morphologies.
[abstract 6 / 55] Wow! (score: 7) - Title: Probing binary supermassive BLACK HOLE in QUASARs tough spectropolarimetryAuthors: J. Biedermann, F. Marin,Comments: 4 pages, 1 figureSubjects: astro-ph.GACreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Nearly all galaxies are believed to host a supermassive BLACK HOLE at their center. In the context of galaxy mergers, the SMBHs from the progenitor galaxies are expected to form a bound binary system. Given the high frequency of such mergers throughout cosmic time, binary SMBHs should be relatively common in ACTIVE GALACTIC NUCLEi (AGNs). Yet, their direct detection remains a major observational challenge, with most candidates inferred only through indirect signatures. The QUASAR Markarian 231 presents unique ultraviolet-optical properties, including an atypical drop in the total flux around 2500 A and a strong wavelength-dependent POLARIZATION. In this work, we explore the potential of spectropolarimetry as a tool to detect and characterize SMBH binaries in AGNs. We construct a simple analytical model in order to reproduce the spectral energy distribution (SED) of Mrk 231 taking into account a binary SMBHs scenario and we compute the resulting total and polarized flux. Our goal is to test if the presence of two distinct sources can reproduce the unique ultraviolet-optical properties observed in Markarian 231. Such investigations support the case for future high-sensitivity UV spectropolarimeters in order to probe the inner structure of QUASARs. In particular, the next-generation instrument POLLUX, proposed for the Habitable Worlds Observatory, would be particularly suited to provide new insights into AGNs physics and supermassive BLACK HOLE binaries in QUASARs.
[abstract 7 / 55] Wow! (score: 7) - Title: Potential binary supermassive BLACK HOLEs in Markarian 231 as a scientific case for the spectropolarimeter POLLUXAuthors: Biedermann. J, Marin. F, Neiner. C, Bouret. Jean-Claude,Comments: 4 pages, 1 figureSubjects: astro-ph.GACreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
It is now widely accepted that a supermassive BLACK HOLE (SMBH) resides in the core of nearly every galaxy. Within the context of mergers of galaxies, the central SMBHs from each system should form a gravitationally bound binary system. Given the frequency of galaxy mergers throughout cosmic time, the existence of such binary SMBHs is likely to occur within ACTIVE GALACTIC NUCLEi. However, identifying them observationally remains highly challenging. The majority of reported candidates rely on indirect evidence rather than unambiguous detection. The QUASAR Markarian 231 (Mrk 231) stands out because of its distinctive ultraviolet to optical properties, which includes a strong wavelength dependent POLARIZATION and an unusual flux decrease at 2500A. In this work, we investigate the potential of spectropolarimetry as a powerful tool for identifying and characterizing SMBH binaries in AGNs. We have developed a simplified analytical model to reproduce the spectral energy distribution of the QUASAR Mrk 231 assuming a binary SMBH geometry, and we compute both its total and polarized emission. The main aim is to test whether two separate emitting sources could explain the unique UV to optical signatures of Mrk 231. Such investigations highlight the importance of a future high-sensitivity UV spectropolarimetric instrument. For instance, the proposed Pollux spectropolarimeter for the Habitable Worlds Observatory (HWO) has the potential to significantly contribute to our understanding of AGNs structure and the role of SMBH binaries in QUASARs.
[abstract 8 / 55] Yes (score: 6) - Title: The first IXPE view of the eclipsing ADC source 4U 1822-37Authors: A. Anitra, A. Gnarini, T. Di Salvo, R. Iaria, A. Marino, F. Barra, L. Burderi, A. Sanna, L. Marra, S. Bianchi, G. Matt, F. Ursini, C. Miceli, A. Miraval Zanon, W. Leone., F. Capitanio, S. Fabiani, P. Kaaret, A. Tarana,Comments: 12 pages, 8 figures. Accepted for publication in Astronomy & AstrophysicsSubjects: astro-ph.HECreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Accretion-disc corona sources are high-inclination low-mass X-ray binaries in which the innermost regions are hidden and the observed X-ray emission is dominated by radiation scattered above the disc. 4U 1822-37 is a key binary system of this class, but its geometry is still debated. X-ray polarimetry offers a direct probe of the scattering structure. We present the first X-ray spectro-polarimetric study of 4U 1822-37 and test whether its spectrum and polarisation can be explained within the accretion-disc-corona scenario. We analysed a coordinated campaign with IXPE, XMM-Newton, NUSTAR, and SWIFT. We performed broadband spectral modelling and model-independent, energy-resolved, and orbital-phase-resolved polarimetric analyses. The broadband spectrum requires a soft thermal component, a Comptonised continuum, a hard power-law tail, and RELATIVISTICally blurred reflection. The observed 0.1-100 keV luminosity, $L_{\rm obs}\simeq6.1\times10^{36}\ {\rm erg\,s^{-1}}$, is far below the intrinsic luminosity expected from the orbital evolution, supporting a geometry in which only a small fraction of the intrinsic emission is scattered into the line of sight by an extended, optically thin corona. In the 2-8 keV band, IXPE measures ${\rm PD}=7.9\pm0.6\%$ and ${\rm PA}=-24^\circ\pm2^\circ$. The PD increases with energy, while the PA remains approximately constant. During eclipse, the PD decreases to ${\rm PD}=5.5\pm1.7\%$, with no significant PA variation. This behaviour is consistent with the companion occulting the most polarimetrically efficient part of the extended corona. The high PD, stable PA, energy-dependent polarisation, and eclipse behaviour support a picture in which 4U 1822-37 is observed in an extreme high-inclination, scattering-dominated regime. The extended corona is the main structure shaping both the observed X-ray emission and its polarisation.
[abstract 9 / 55] Yes (score: 6) - Title: Composition-dependent acceleration of UHE Cosmic Rays in AGN electric fieldsAuthors: E. Koutsoumpou, I. Contopoulos, A. Nathanail, A. Loules, D. Kazanas,Comments:Subjects: astro-ph.HECreated: 2026-09-23; Updated: 2026-09-25; Datestamp: 2026-09-25
The origin of ultra-high-energy COSMIC RAYs (UHECRs) remains elusive, as proposed acceleration mechanisms are rarely connected directly to composition-sensitive air-shower observables. We establish such a connection for voltage-drop acceleration in near-horizon current sheets of MAGNETically arrested disks around supermassive BLACK HOLEs. Fragmentation is represented by a log-normal distribution of effective potential-sampling factors $η$, with $μ_η=\langle\lnη\rangle$, $σ_η=[\mathrm{Var}(\lnη)]^{1/2}$, and median $\widetildeη=e^{μ_η}$, while the energy gain scales with nuclear charge $Z$ and maximum potential $\mathcal{V}_{\max}$. We propagate the accelerated particles through Bethe--Heitler and adiabatic losses, proton photopion attenuation, and a mass-evolving photodisintegration cascade, and predict $\langle X_{\max}\rangle$ and $σ(X_{\max})$. We perform Bayesian fits to the Pierre Auger Observatory 2025 DNN measurements for two fixed injection templates and propagation distances of 10, 30, and 100 Mpc. An Auger-inspired, proton-poor injection reproduces both shower moments at 10 and 30 Mpc, with $χ^2/ν=0.33$ and $0.47$. At 30 Mpc, $σ_η=0.59^{+0.13}_{-0.10}$, corresponding to a multiplicative dispersion of approximately 1.8. The median sampling factor and maximum potential remain strongly degenerate, with $\widetildeη\mathcal{V}_{\max}$ more directly constrained. A metal-enriched injection containing $\sim53\%$ hydrogen gives $χ^2$ larger by 17.9 and 25.9 at 10 and 30 Mpc. Both templates remain viable at 10 and 30 Mpc but fit poorly at 100 Mpc. Within the scenarios tested, the results favour a relatively proton-poor accelerated population and show that the shower-width evolution can constrain the stochastic structure of electric-field acceleration in nearby AGN.
[abstract 10 / 55] Yes (score: 5) - Title: Event Horizon Telescope Pattern Speeds in the Visibility DomainAuthors: Nicholas S. Conroy, Michi Bauböck, Vedant Dhruv, Daeyoung Lee, Chi-kwan Chan, Abhishek V. Joshi, Cora Prather, Charles F. Gammie,Comments: Published in ApJ 2026 June 25 (16 pages, 10 figures)Subjects: astro-ph.HECreated: 2026-09-23; Updated: 2026-09-25; Datestamp: 2026-09-25
The Event Horizon Telescope is preparing to produce time sequences of BLACK HOLE images, or movies. In anticipation, we developed an autocorrelation technique to measure apparent rotational motion using the image-domain pattern speed $Ω_p$. Here, we extend this technique to the visibility domain and introduce the visibility amplitude pattern speed $Ω_{\mathrm{VA}}$. We show that in the Illinois v3 library of EHT source models, $Ω_{\mathrm{VA}}$ depends on the source inclination, BLACK HOLE mass, BLACK HOLE spin, accretion state (MAD or SANE), and baseline length, and then provide approximate fits for this dependence. We show that $Ω_{\mathrm{VA}}$ is particularly sensitive to baseline length for MAD (strongly MAGNETized) models, and that the slope of this dependence can be used to constrain BLACK HOLE spin. As with $Ω_p$, models predict that $Ω_{\mathrm{VA}}$ is well below the Keplerian frequency in the emission region for all model parameters. This is consistent with the idea that $Ω_{\mathrm{VA}}$ measures an angular phase speed for waves propagating through the emission region. Finally, we identify the information that would be provided by space-based millimeter VLBI such as the proposed BHEX mission.
[abstract 11 / 55] Yes (score: 5) - Title: Probing Extragalactic Ultralight Axion Dark Matter with Decade-long Blazar Optical Polarimetry of 1ES 1959+650Authors: Qiu-Ju Huang, Bao Wang, Jun-Jie Wei, Xue-Feng Wu,Comments: 12 pages, 8 figures. Accepted for Publication in Physical Review LettersSubjects: astro-ph.HE astro-ph.CO hep-phCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Axions or axion-like particles (ALPs) are well-motivated DARK MATTER (DM) candidates whose coupling to photons induces periodic oscillations in the POLARIZATION angle of astrophysical light. This work reports the first search for such a signature using ten years of optical polarimetric monitoring of the BLAZAR 1ES~1959+650. No statistically significant periodicity is detected, determined by a Lomb-Scargle periodogram combined with Monte Carlo analysis. Assuming a central DM density in the host galaxy, this null result places tight upper limits on the ALP-photon coupling constant at $g_{aγ}<(5.8 \times 10^{-14}-1.8\times 10^{-10})\,\mathrm{GeV}^{-1}$ across a broad ALP mass range of $m_a \sim (1.4\times10^{-23}-5.2\times10^{-20})\,\mathrm{eV}$. Our constraints surpass those from Very Long Baseline Array polarimetry of active galactic JETs and from polarimetric data of the European Pulsar Timing Array, and are competitive with those from long-term Galactic pulsar timing of PSR J0437-4715 over the same ALP mass window. These results establish long-term BLAZAR polarimetry as a competitive and complementary approach for probing axion-like DM on extragalactic scales.
[abstract 12 / 55] Yes (score: 5) - Title: Profile Analysis of the Multiwavelength 2.1-year Oscillations of PG 1553+113Authors: P. Peñil, N. Torres-Albà, A. Rico, L. Marcotulli, A. Domínguez, M. Ajello, S. Buson, S. Adhikari,Comments: 21 pages, 10 figues, 5 tables. Published in the Open Journal of AstrophysicsSubjects: astro-ph.GACreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
We investigate the morphology of the oscillation profiles of the BLAZAR PG~1553+113 in relation to its well-known $\sim$2.1 yr periodicity. We identify individual cycles in the $γ$-ray, X-ray, UV, and optical light curves and characterize their temporal profiles using analytical models for single- and multi-peaked events. We find that the oscillations are generally described by a broad activity envelope with shorter-timescale substructure, showing that the $\sim$2.1 yr signal is not a strictly sinusoidal or self-similar modulation. The internal morphology varies across cycles and energy bands. This is particularly evident in X-rays, where all analyzed cycles show a strong formal preference for multi-component profiles, unlike the $γ$-ray band, where several cycles admit statistically comparable empirical descriptions. The contemporaneous MWL oscillations show broadly aligned activity episodes, but the timing and relative amplitudes of secondary components are not systematically repeated. This suggests that a common long-term modulation affects the broadband emission, while additional local or energy-dependent processes shape individual cycles. Such a picture is compatible with a geometric, JET-related contribution to the broad recurrent envelope, with intrinsic variability superimposed on it. We also identify new cycles with a dominant peak accompanied by weaker twin-peak-like features, similar to structures previously discussed in a supermassive BLACK HOLE binary scenario for PG~1553+113. Although our results do not provide definitive evidence for this interpretation, the recurrence of comparable morphologies in newly analyzed cycles keeps this scenario viable.
[abstract 13 / 55] Yes (score: 5) - Title: Recurrent double-peaked $γ$-ray sub-flares in PKS 1424-418Authors: Na Wang, Tong Liu, Jingran Xu,Comments: 12 pages, 6 figures, 3 tables, accepted for publication in MNRASSubjects: astro-ph.HE astro-ph.GACreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
We report a hint of recurrent double-peaked $γ$-ray sub-flares in PKS~1424--418 during two similar major active epochs, MJD 56117--56498 and MJD 59669--59978. The candidate double-peaked sub-flares show a characteristic intra-subflare peak separation of $\sim 11.8$ d and a neighbouring-subflare spacing of $\sim 67$ d. Red-noise Monte Carlo tests indicate that the candidate recurrent double-peaked morphology is not easily reproduced by stochastic variability alone, with false-alarm probabilities of $p_{\rm a}=0.0216$ and $p_{\rm b}=0.0006$ for the two active epochs, respectively. In the simulations of the entire \textit{FERMI} Large Area Telescope (LAT) light curve, no red-noise realisation reproduces both epoch-like structures. The spectral energy distribution (SED) modelling shows similar radiative properties for the two peaks of one double-peaked candidate, while changes in the Doppler factor appear to play an important role in the flaring activity. Together with the previously reported near-zero lag between the millimetre and $γ$-ray emission, these results suggest that the recurrent activity may be associated with the compact mm/sub-mm core region. We discuss a possible structured-JET scenario in which a single disturbance propagates through a chain of quasi-stationary recollimation shocks. In this picture, repeated interactions between the disturbance and the shock structure may qualitatively account for both the double-peaked sub-flare profiles and the observed $\sim 11.8$ d and $\sim 67$ d time-scales. Further active epochs are required to determine whether this similarity represents a recurrent long-term behaviour.
[abstract 14 / 55] Yes (score: 5) - Title: AGN winds and outflows: from accretion-disc scales to the host galaxyAuthors: Delphine Porquet,Comments: 6 pages, 1 figure (two panels). Proceedings contribution based on an invited review presented in Session 20 at the 2026 Annual Meeting of the French Society of Astronomy and Astrophysics (SF2A), held in June 2026; limited to six pagesSubjects: astro-ph.HE astro-ph.GACreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Ultra-fast outflows (UFOs), launched from the inner accretion disc in ACTIVE GALACTIC NUCLEi (AGN), are among the prime candidates for driving AGN feedback in their host galaxies. Determining their physical properties and energetics is therefore essential for assessing their impact on galaxy evolution. This review highlights recent observational progress, with particular emphasis on the groundbreaking insights enabled by high-resolution X-ray spectroscopy. The first X-Ray Imaging and Spectroscopy Mission (XRISM)/Resolve observations of AGN winds have revealed that the innermost UFOs are kinematically structured and inhomogeneous. In the archetypal QUASAR PDS 456, these observations have led to a substantial upward revision of the inferred mass outflow rate, momentum flux and kinetic power. Complementary UV, optical, IR and mm observations trace the ionised, atomic and molecular phases of AGN-driven outflows from parsec to galactic scales. However, the physical coupling between the accretion-disc wind and the galactic outflows remains one of the major unresolved questions in AGN feedback. Building on the pioneering XRISM results, NewAthena's X-ray Integral Field Unit (X-IFU) will characterise the physical properties and energetics of accretion-disc winds with unprecedented precision from the local Universe up to cosmic noon, while complementary multi-wavelength observations with facilities such as the Extremely Large Telescope (ELT), James Webb Space Telescope (JWST), Atacama Large Millimeter/submillimeter Array (ALMA), and Square Kilometre Array (SKA) will determine whether and how their energy and momentum are transferred to the host galaxy.
[abstract 15 / 55] Yes (score: 5) - Title: A Multiwavelength View of $ρ$ Oph II: Disentangling the Variability of the Multi-Star Component CAuthors: Sean J. Gunderson, Walter W. Golay, Jackson Codd, David P. Huenemoerder, Felipe Navarete, Christiana Erba, Alexandrea Moreno, John M. Cannon, Richard Ignace, Pragati Pradhan, the MACRO consortium,Comments: 27 pages, 8 figures, 6 tables, accepted for publication in ApJ, full list of contributing MACRO consortium members is provided in the Author Contribution section at the end of the manuscriptSubjects: astro-ph.SR astro-ph.HECreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
We present a multiwavelength analysis of the star $ρ$ Oph C, covering X-ray, optical, near-infrared, and radio observations to test for the presence of interferometrically-detected cool star companions. The X-ray observations from Chandra, XMM-Newton, and NUSTAR show flare-like events lasting minutes or days in time and spectral properties consistent with those of cooler stars instead of the primary MAGNETic B star. The near-infrared data is also consistent with the proposed trinary system properties due to the presence of CO-band heads. After removing the primary B star's rotation, the optical data from TESS shows a residual signal at the level of 0.8 mmags, matching the variations expected from cool stars in orbit around a bright B star. Finally, multi-epoch radio data reveals that $ρ$ Oph C exhibits significant large scale flux variations that are atypical for a MAGNETic massive star. Taken as a whole, the multi-epoch and -wavelength data presents a consistent picture of $ρ$\,Oph\,C as a rare trinary system composed of a hot star and two cool stars.
[abstract 16 / 55] Yes (score: 5) - Title: Study of low-frequency core-edge coupling in a tokamak: III. Core-localized MHD continuum pulsations \& distant forced RECONNECTionAuthors: Andreas Bierwage, Panith Adulsiriswad, Gyungjin Choi, Young-chul Ghim, Masatoshi Yagi,Comments: 29 pages, 18 figuresSubjects: physics.plasm-phCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Slow MAGNEToacoustic pulsations (SMAPs) are found in MHD simulations of a tokamak plasma whose safety factor $q$ near the center is flat and slightly above unity ($q \gtrsim 1$). SMAPs are located on the central plateau of the slow MAGNEToacoustic continuum $ω_{\rm S} = k_\parallel c_{\rm S}$, where $c_{\rm S}$ is the speed of sound and $k_\parallel$ the wavenumber parallel to the MAGNETic field. In our model, SMAPs exist when the ion viscosity and thermal diffusivity are sufficiently low. They can be driven unstable by a pressure gradient in the $q \sim 1$ region when the electric resistivity is sufficiently high. Exponentially growing SMAPs consist of standing slow waves on MAGNETic surfaces that are radially synchronized into a quasi-interchange structure with poloidal/toroidal mode numbers $m/n=1/1$. After free energy depletion, saturated quasi-linear pulsations (alternating $n=1$ and $0$) in the central $q\sim 1$ region couple to distant $q\geq 2$ rational surfaces that undergo "reversible" MAGNETic RECONNECTion: as the MAGNETic islands wax and wane with period $2π/ω_{\rm S}$, their X- and O-points alternate. These results show how the MHD model facilitates non-local coupling of slow waves, pressure-driven resistive interchange and tearing. This motivates further study in kinetic models, where collisionless mechanisms for fast reversible RECONNECTion exist and proper treatment of parallel dynamics will allow to assess the role of Landau damping as well as the question whether the ${\mathbf B}$ field's weak ergodicity in the $q\sim 1$ region allows the waves to outpace the ion's parallel streaming to maintain the thermal misbalance underlying SMAPs. Also of interest are pulsations closer to the Alfvénic branch, satisfying $ω\approx k_\parallel v_{\rm A}$ with Alfvén speed $v_{\rm A}$, which require no resistivity and are less dependent on thermal misbalance.
[abstract 17 / 55] Yes (score: 4) - Title: Magnetic Field Configurations in Binary Neutron Star Mergers I: Post-merger Remnant and DiskAuthors: Eduardo M. Gutiérrez, William Cook, David Radice, Sebastiano Bernuzzi, Jacob Fields, Peter Hammond, Boris Daszuta, Harshraj Bandyopadhyay, Maximilian Jacobi,Comments: 21 pages, 17 figures, 1 tableSubjects: astro-ph.HE gr-qcCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
We present a suite of general RELATIVISTIC MAGNETohydrodynamic (GRMHD) simulations of binary neutron star (BNS) mergers performed with the code GR-Athena++. We investigate how a different initial MAGNETic field configuration, nuclear equation of state, or binary mass ratio affects the MAGNETic and thermodynamic evolution of the post-merger remnant and disk. We also analyze the impact of the commonly-assumed reflection (bitant) symmetry across the equatorial plane. Magnetic field amplification occurs shortly after the merger due to the Kelvin-Helmholtz instability; later, the field keeps evolving with a predominantly toroidal configuration due to winding and turbulence. The initial MAGNETic field topology leaves an imprint on the field structure and affects MAGNETic field amplification for the initial MAGNETic field values commonly assumed in the literature and the limited resolution of the simulations. Enforcing equatorial reflection symmetry partially suppresses the development of turbulence near the equatorial plane and impacts the post-merger MAGNETic field evolution. Stiffer EOSs produce larger, less compact remnants that may retain memory of the pre-merger strong poloidal field.
[abstract 18 / 55] Yes (score: 4) - Title: Wind-confined JET collimation revealed by the acceleration-phase photosphere of GRB 220426AAuthors: Felix Ryde, Asaf Pe'er,Comments: Submitted. 18 pages + appendicesSubjects: astro-ph.HECreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
We analyze the prompt emission of the exceptionally bright GRB 220426A observed by {\it FERMI}/GBM, whose time-resolved spectra are among the narrowest measured in any GRB. Here we show that observations during the first $\sim 5$~s are consistent with the signal being emitted while the JET was still in the initial radiation-dominated acceleration phase. The time-resolved spectra allow the effective launch radius, $r_0$, to be inferred with unusual precision. We find $r_0 \sim \mathrm{few} \times 10^{10}\,\mathrm{cm}$, increasing linearly with time. These findings match the theoretical expectation for the recollimation shock, implying that this GRB shows the first clear evidence for the existence and evolution of a recollimation shock. Using this interpretation, the linear increase observed is sustained over a period longer than expected from a pure JET breakout. Therefore, the JET collimation must have persisted even after breakout. We suggest that the collimation was maintained by a finite, dense, wind-like circumburst medium, which would reproduce the observed behavior of the prompt emission. We conclude that late-stage progenitor mass-loss can shape the earliest prompt emission and that the photospheric emission provides a way to probe both the JET collimation and the innermost region of the circumburst medium (CBM) surrounding the progenitor, independently of the constraints from interacting SUPERNOVAe.
[abstract 19 / 55] Yes (score: 4) - Title: Supermassive BLACK HOLE binaries in the multi-messenger context of ground and spaceborne VLBIAuthors: B. Hudson, L. I. Gurvits, D. J. D'Orazio, C. Tiede, T. M. Eubanks, E. Mooij,Comments: Published in the BHEX focus issue by Publications of the Astronomical Society of the Pacific (PASP). 22 pages, 10 figures. Comments are welcomeSubjects: astro-ph.HE astro-ph.IMCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Evidence of a gravitational wave background suggests the existence of a population of sub-parsec supermassive BLACK HOLE binaries (SMBHBs), with characteristic angular separations on the order of 1-10 $μ$as. Spaceborne extensions of Very Long Baseline Interferometry (VLBI) and the next generation ground arrays introduce the possibility of directly imaging these SMBHBs. In this work, a binary spectral energy distribution model is used to predict the detectability of SMBHBs with ground and spaceborne VLBI. We consider the Black Hole Explorer (BHEX), a proposed spaceborne VLBI mission, as our primary case study. We explore the detectable SMBHB parameter space and identify distinguishable binary signatures in the visibility domain. We find that for a flux-density-limited sample, ground array observations are more effective at detecting a wider region of the binary parameter space, with $M_\mathrm{tot} \gtrsim 10^9$ solar mass systems detectable out to redshift $z=0.075$ and beyond, depending on mass ratio. Conversely, inclusion of a spaceborne element such as BHEX, offering finer angular resolution ($\sim6\,μ$as) and sampling of the (u,v) plane not limited by Earth rotation synthesis, will provide significant benefits in constraining binary properties. An illustrative Fisher analysis shows improvements in characterisation of the separation and position angle of SMBHBs by a factor of $\sim4$. Near-future ground and/or spaceborne VLBI may achieve the first direct observation of a SMBHB, contributing significantly to multi-messenger studies of such systems with pulsar timing arrays and observations across the electroMAGNETic spectrum.
[abstract 20 / 55] Yes (score: 4) - Title: Dynamically Stable Magnetic Fields in Relativistic Neutron Stars: A Diverse Landscape of GRMHD EquilibriaAuthors: Mai Li, Vasileios Paschalidis, Antonios Tsokaros, Maria Mutz, Koji Uryu,Comments:Subjects: astro-ph.HECreated: 2026-09-23; Updated: 2026-09-25; Datestamp: 2026-09-25
Neutron stars endowed with purely poloidal or purely toroidal MAGNETic fields are known to be unstable, and settle into mixed poloidal-toroidal configurations. The end state of these instabilities is still poorly understood. It is unclear whether this state is unique or whether the dynamically stable configuration has memory of the initial conditions. In this work, we perform long-term, fully general RELATIVISTIC MAGNETohydrodynamic simulations of equilibrium configurations of slowly rotating neutron stars endowed with self-consistent mixed poloidal and toroidal MAGNETic fields. Our initial configurations differ in their initial MAGNETization and MAGNETic field geometry. We evolve the initial equilibria for tens of Alfvén timescales until well after any instabilities have saturated. Employing an array of diagnostic tools from visualizations to the structure of the plasma four-current and a vector spherical harmonic decomposition of the settled MAGNETic fields, we characterize the structure of the dynamically stable, settled MAGNETic equilibria. We find that the settled configurations are not unique. Instead, they exhibit diverse multipolar structures, with higher-order modes contributing substantially. Our findings demonstrate that there is memory of the MAGNETic-field initial conditions, and that there is no unique dynamically stable MAGNETic-field geometry for neutron stars. Nevertheless, we find that the angle-averaged radial profile of the MAGNETic field toroidal to poloidal amplitude in the bulk of the settled configurations exhibits some degree of universality with typical values of order \(20\)--\(40\%\).
[abstract 21 / 55] Yes (score: 4) - Title: Spatial segregation as the origin of anisotropic satellite quenching in haloes and beyondAuthors: Zhuoming Zhang, Weiguang Cui, Yun Chen, Romeel Davé,Comments: 22 pages, 7 figures, 1 tableSubjects: astro-ph.GA astro-ph.COCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Satellite galaxies in massive halos are seen to be preferentially quenched along the major axes of their central galaxies. In contrast, the AGN JET tends to point along the minor axis, which imposes interesting constraints on the role of AGN feedback in satellite galaxy quenching. Here we use the SIMBA, TNG100, EAGLE, and feedback-free SIMBA cosmological simulations at $z=0$ to show that this satellite anisotropy primarily originates from spatial segregation between quenched and unquenched populations. Quenched satellites are more centrally concentrated and more strongly aligned with the central galaxy's major axis, whereas unquenched satellites occupy larger radii and are more nearly isotropic. The persistence of this behaviour without stellar or ACTIVE GALACTIC NUCLEus feedback suggests that feedback is not important for satellite quenching. Beyond the halo boundary, the signal varies strongly among simulations and correlates with the excess number of galaxies along the major axis. This links large-scale anisotropic quenching to the direction-dependent distribution of groups, clusters and filamentary environments. Our results provide a unified geometrical interpretation of anisotropic satellite quenching across halo and extra-halo scales.
[abstract 22 / 55] (score: 3) - Title: Simulating the convection in red super-giant stars: wobbling JETs in common envelope evolutionAuthors: Shlomi Hillel, Ron Schreier, Noam Soker,Comments: Accepted in Publications of the Astronomical Society of the PacificSubjects: astro-ph.SRCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
We use our newly constructed three-dimensional red supergiant (RSG) stellar model, which also mimics nuclear energy production and photospheric emission, to calculate the stochastic component of the angular momentum of the mass that a companion spiraling within the RSG's envelope accretes during common envelope evolution (CEE). The accreted mass has a fixed-direction angular-momentum component arising from the density gradient in the RSG envelope and orbital motion. The angular momentum component with a stochastically varying direction results from vigorous envelope convection. We do not include the companion's influence on the RSG envelope during the CEE and consider an undisturbed, non-rotating RSG stellar model. We find that the fluctuating angular momentum amplitude can be several times the fixed-axis angular momentum. The total specific angular momentum of the accreted mass easily forms intermittent accretion disks around neutron stars and BLACK HOLEs, but it is only marginally sufficient, or not at all, to form accretion disks around main-sequence stellar companions. The intermittent accretion disks we expect to form will launch wobbling JETs with varying axes. We discuss aspects of wobbling JETs in the CEE and the grazing envelope evolution (GEE), which might precede the CEE or replace it altogether. Studies have claimed that JETs are a crucial ingredient in many cases of CEE, and the standard CEE should include JETs that the companion launches, before (like the GEE), during, and/or at the exit from the CEE. Our study supports this claim and emphasizes the importance of wobbling JETs.
[abstract 23 / 55] (score: 3) - Title: Probing the Metallicity Dependence of Fast Radio Burst Progenitors with CHIME/FRB Outrigger Dwarf Host GalaxiesAuthors: Y. Dong, W. Fong, K. Nimmo, N. Loudas, B. C. Andersen, S. Andrew, A. Cai, S. Chatterjee, A. M. Cook, A. P. Curtin, T. Eftekhari, B. M. Gaensler, J. Hessels, V. M. Kaspi, A. Khan, C. Leung, L. Mas-Ribas, K. Masui, A. Moroianu, A. B. Pearlman, J. X. Prochaska, M. W. Sammons, P. Scholz, K. Shin, S. Simha, M. Woodland, Z. Zhuang,Comments: Submitted to ApJ. 32 pages, 10 figures, and 6 tablesSubjects: astro-ph.HE astro-ph.GACreated: 2026-09-23; Updated: 2026-09-25; Datestamp: 2026-09-25
Using the fast radio bursts (FRBs) localized with the CHIME/FRB Outriggers between February and October 2025, we conduct a systematic search for dwarf host galaxies. We identify and characterize eight host galaxies for one repeating and seven apparently non-repeating FRBs, newly classifying five hosts as dwarfs with stellar masses of $\log(M_\ast/M_\odot) \approx 8.1-9.1$. We measure their gas-phase metallicities and, when combined with hosts from the literature, finding that repeating and non-repeating FRBs have statistically distinct metallicity distributions. Non-repeating FRBs inhabit relatively metal-rich environments ($12 + \rm log( O/H) \gtrsim 8.35$) across the full observed mass range, while repeating FRBs have significant preference for dwarf galaxies with $12 + \rm log( O/H) \lesssim 8.35$. Almost all repeaters associated with persistent radio sources (PRSs) are in dwarfs with $12 + \rm log( O/H) \lesssim 8.15$, suggesting a connection between repeaters in metal-poor dwarf environments and PRS formation. We also calculate the host dispersion measure ($\mathrm{DM}_{\rm host}$), Faraday rotation measure ($\mathrm{RM}_{\rm host}$), and scattering timescale ($τ_{\rm host,1~GHz}$) for 54, 37, and 24 FRBs, respectively, including both our sample and FRBs in the literature. We find no significant ($>3σ$) correlation between host metallicity and $\mathrm{DM}_{\rm host}$, $\mathrm{RM}_{\rm host}$, or $τ_{\rm host,1~GHz}$. The distinct host metallicities of apparently non-repeating and repeating FRBs may reflect metallicity-dependent massive-star evolution, with repeating FRBs and PRSs requiring more extreme MAGNETar birth spins than the predominantly non-repeating FRB population.
[abstract 24 / 55] (score: 3) - Title: Turning-Point Count Discrepancy as a Diagnostic of Relativistic Orbital ChaosAuthors: Wenfu Cao, Ying Wang, Hongsheng Zhang,Comments: 17 pages, 3 figuresSubjects: gr-qcCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
We propose the turning-point count-discrepancy indicator (TPCD) for diagnosing orbital chaos from a single trajectory in RELATIVISTIC Hamiltonian systems with two oscillatory degrees of freedom. TPCD measures the largest cumulative departure of one turning-event count from its mean rate per reference cycle, requiring neither a neighboring orbit nor a phase-space partition and applying to both massive particles and photons. We establish its long-time behavior under explicit event--phase assumptions. Rigid phases with an exact event--phase correspondence obey a strict discrepancy bound of unity, and linearizable regular tori with bounded degree-one phase deformations obey a finite, orbit-dependent bound; both imply that the normalized indicator decays to zero as the record grows. A diffusive fluctuation mechanism instead yields a Brownian-bridge scaling and a finite statistical scale. Integrable Kerr motion validates the construction, recovering prescribed frequency ratios from event counts to within $2.6\times10^{-5}$ for six targets, including an irrational ratio. In charged-particle scans around a Kerr BLACK HOLE in an external test MAGNETic field, TPCD and the fast Lyapunov indicator agree for all 80 sampled trajectories. In the Schwarzschild--Melvin photon model, a trajectory with elevated finite-time TPCD but low fast-Lyapunov values is identified as regular once its indicator trends downward over an extended integration, showing that finite-time values must be read together with their long-time trend.
[abstract 25 / 55] (score: 3) - Title: Impact of soft QCD effects over intraJET azimuthal anisotropiesAuthors: Jesus Alberto V. Corral, A. Cota Rodriguez, J. A. Murillo Quijada,Comments: 13 pages, 6 figuresSubjects: hep-ph hep-exCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Observations of collective signatures within JETs of particles have been recently reported by measurements at the Large Hadron Collider at CERN laboratory, providing insights on the minimum conditions required for forming a Quark Gluon Plasma state. A quantitative comparison with data measurements on intraJET azimuthal anisotropies and predictions from PYTHIA event generator soft QCD model parameter tunes: Monash, CP5, and QCD-scheme CR is presented. Energetic JETs with transverse momentum over 550 GeV from proton-proton collisions at 13 TeV are reconstructed. Results from predictions using the standard E-scheme (ES) and JET axis choice are compared with those from the Winner-Take-All (WTA) frame. Significant differences are present between predictions from WTA and ES frames at the lowest and highest intraJET charged particles multiplicities ($N_{\mathrm{ch}}$), with the QCD-scheme CR tune showing the smallest variation between frames. Predictions for $v_2$ at the highest $N_{\mathrm{ch}}$ are consistent with the data measurements at a 2.3$σ$ uncertainty level. These results set new guidance towards the search for intraJET collective effects and understanding of nonperturbative QCD dynamics originated from a single parton.
[abstract 26 / 55] (score: 3) - Title: Optical spectropolarimetry of extreme H$α$ line profiles in seven ACTIVE GALACTIC NUCLEiAuthors: J. Biedermann, F. Marin, D. Hutsemékers, C. M. Gaskell,Comments: 20 pages, 12 figures, 2 tablesSubjects: astro-ph.GACreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Some ACTIVE GALACTIC NUCLEi (AGNs) are known to show extremely asymmetric broad Balmer lines, with their main peak redshifted or blueshifted by thousands of km s$^{-1}$, severely challenging our understanding of the standard AGN paradigm. We wanted to explore the causes of such asymmetric features by carrying out a spectropolarimetric study of a sample of bright AGNs with known extreme Balmer line profiles. We present optical spectropolarimetry of seven bright (V $<$ 17.5) Seyfert-1 galaxies obtained with the Very Large Telescope (VLT) FOcal Reducer/low dispersion Spectrograph 2 (FORS2) instrument from March 2012 to January 2013. The main broad Balmer lines (H$α$ and H$β$, and H$γ$ occasionally) were sampled with a resolving power ranging from 350 to 500. We performed a detailed spectral decomposition of each H$α$ profile to isolate kinematic substructures within the broad line region (BLR) and measured the POLARIZATION degree and angle of each component, providing constraints on the inner geometry and scattering properties. The broad H$α$ components exhibit various scattering geometries. Their POLARIZATION as a function of full width at half maximum (FWHM) reveals two distinct behaviors, corresponding to either a BLR of roughly constant scale height or a stratified structure with decreasing height at higher velocities. This supports a disk-wind geometry linking equatorial and polar regions.
[abstract 27 / 55] (score: 3) - Title: Coronal Green-Line Emission During a Solar Prominence Eruption: Spectroscopic Evidence of Its Correspondence with the EUV Late PhaseAuthors: P. Vemareddy, R. Ramesh, V. Muttu Priyal,Comments: Accepted to publish in ApJ, 12 pages, 7 figuresSubjects: astro-ph.SRCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
We report spectroscopic observations during a prominence eruption on 9 October 2025 from the Sun's west limb, associated with an M2.0 flare that commenced at 12:11 UT. The event was captured in sit-and-stare mode by the Visible Emission Line Coronagraph (VELC) onboard Aditya-L1, providing continuous observations of the Fe XIV 5303 Åcoronal greenline. The spatially averaged green-line emission exhibits a clear correspondence with the EUV late-phase (ELP) emission observed in multiple SDO/AIA channels. In particular, an enhanced 5303 Åemission peak at 15:24 UT coincides with secondary peaks in the AIA 211, 171, 193, and 335 Åpassbands, occurring $\sim173$ minutes after the X-ray peak. The 5303 Åline-width information provides important constraints on the mechanism responsible for the ELP. The line-width decreases progressively by about 28\% toward the ELP peak, broadly consistent with the cooling of post-flare coronal loops. This behavior suggests that the ELP is predominantly associated with plasma cooling, with relatively weak additional energy input from MAGNETic RECONNECTion, which does not produce a significant enhancement in line-widths. The estimated non-thermal velocity decreases from $\sim$36 km s$^{-1}$ during the impulsive phase to $\sim$21 km s$^{-1}$ during the gradual phase, indicating a reduction in turbulent plasma motions. And doppler velocities evolve from predominantly positive values during the eruptive rise phase to negative values during the later gradual phase, implying upward and subsequent downward plasma motions. To our knowledge, this study provides the first space-based spectroscopic evidence linking coronal green-line emission with the ELP and its origin during a solar flare.
[abstract 28 / 55] (score: 3) - Title: The third law of BLACK HOLE thermodynamics and the mass-to-charge ratio of scalar fieldsAuthors: Shahar Hod, Tsvi Piran,Comments: 4 pagesSubjects: gr-qc astro-ph.HE hep-thCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Kehle and Unger have recently shown that self-gravitating charged classical scalar fields can collapse to form extremal Reissner-Nordström (eRN) BLACK HOLEs in finite time, thus violating the third law of thermodynamics (TLT). Reall has subsequently proved that the formation of an eRN BLACK HOLE in gravitational collapse is impossible if the mass-to-charge ratio of the field exceeds unity, $m/e\geq1$. In the present compact paper we conjecture, using quantum considerations, that the Reall bound is {\it not} sharp. In particular, we point out that the electric field of a charged system with charge $Q$ will spontaneously polarize the vacuum in the regime $(eQ/\hbar)^2>(mQ/\hbar)^2+1/4$, thereby creating pairs of charged particles that discharge the BLACK HOLE and ensure the quantum validity of the TLT in this regime. Motivated by the TLT, we conjecture that the classical Reall bound can be strengthened such that classical considerations would prevent eRN BLACK HOLEs from forming dynamically in the regime $m/e\geq\sqrt{1-\big({{\hbar}/{2eQ}}\big)^2}$, where quantum POLARIZATION effects are unable to protect the TLT.
[abstract 29 / 55] (score: 2) - Title: Detecting Extragalactic Axion-like Dark Matter with Polarization Measurements of Fast Radio BurstsAuthors: Bao Wang, Xuan Yang, Jun-Jie Wei, Song-Bo Zhang, Xue-Feng Wu,Comments: 27 pages, 7 figures. Published in Communications PhysicsSubjects: astro-ph.HE astro-ph.CO hep-phCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Axions or axion-like particles (ALPs) are one of the promising DARK MATTER (DM) candidates. A prevalent method to detect axion-like DM is to seek periodic oscillation in the POLARIZATION angles (PAs) of linearly polarized light emitted from astrophysical sources. In this work, we use the time-resolved POLARIZATION measurements of the hyperactive repeating fast radio burst, FRB 20220912A, detected by the Five-hundred-meter Aperture Spherical radio Telescope (FAST) to search for extragalactic axion-like DM. Given a DM density profile of FRB 20220912A's host, we obtain upper limits on the ALP-photon coupling constant of $g_{a γ}<(3.4 \times 10^{-11}-1.9\times 10^{-9})\,\mathrm{GeV}^{-1}$ for the ALP masses $m_a \sim (1.4\times10^{-21}-5.2\times10^{-20})\,\mathrm{eV}$. Persistent polarimetric observations with FAST would extend the constraints to lower masses. Although the $g_{a γ}$ constraints derived from FRBs are less competitive than those from other methods, FRBs offer an alternative way to detect axion-like DM on extragalactic distance scales, complementary to galactic DM probes.
[abstract 30 / 55] (score: 2) - Title: Medium-induced modification of azimuthal correlations of electrons from heavy-flavor hadron decays with charged particles in Pb--Pb collisions at $\sqrt{s_{\rm{NN}} = 5.02}$ TeVAuthors: ALICE Collaboration,Comments: 35 pages, 10 captioned figures, 2 tables, authors from page 29, published version, figures at http://alice-publications.web.cern.ch/node/12665Subjects: nucl-ex hep-exCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
The azimuthal-correlation distributions between electrons from the decays of heavy-flavor hadrons and associated charged particles in Pb$-$Pb collisions at $\sqrt{s_{\mathrm{NN}}} = 5.02$ TeV are reported for the 0$-$10% and 30$-$50% centrality classes. This measurement provides access to the JET-like correlation observables in the heavy-flavor sector in Pb$-$Pb collisions. The analysis is performed for trigger electrons from heavy-flavor hadron decays with transverse momentum $4 < p_\mathrm{T}^\mathrm{e} < 16~{\rm GeV}/c$, considering associated particles within the transverse-momentum range $1 < p_\mathrm{T}^\mathrm{assoc} < 7$ ${\rm GeV}/c$, and a pseudorapidity difference of $|Δη|<1$ between the trigger electron and associated particles. The per-trigger nuclear modification factor ($I_\mathrm{AA}$) is calculated to compare the near- and away-side peak yields to those in pp collisions at $\sqrt{s} = 5.02$ TeV. In 0$-$10% central collisions, the $I_\mathrm{AA}$ indicates a hint of enhancement of associated-particle yields with $p_\mathrm{T}<3$ GeV/$c$ on the near side, and a suppression of yields with $p_\mathrm{T}>4$ GeV/$c$ on the away side. The $I_\mathrm{AA}$ for electron triggers from heavy-flavor hadron decays is compared with that for light-flavor and strange-particle triggers to investigate the dependence on different fragmentation processes and parton-medium dynamics, and is found to be the same within uncertainties.
[abstract 31 / 55] (score: 2) - Title: Detection of a puzzling dual-superorbital hard X-ray modulation in the X-ray binary GX 301-2Authors: Haoyang Zhang, Li Zhang,Comments: This paper is withdrawn because reanalysis shows that the reported 115- and 65-day signals are sampling aliases of the orbital modulation and its second harmonic in the monthly-binned Swift/BAT data. The claimed detection of two independent superorbital modulations and the associated physical interpretation are therefore not supportedSubjects: astro-ph.HECreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
The superorbital modulations (SMs) observed in wind-fed X-ray binaries remain a puzzling phenomenon in astrophysics. To investigate this behavior observationally, we analyzed the long-term hard X-ray light curve from the SWIFT/BAT 157-Month Hard X-ray Survey in X-ray binary GX 301-2. Using three timing analysis methods--the Lomb-Scargle periodogram, the weighted wavelet Ztransform, and Gaussian processes--we identify a rare dual-SM behavior in this source: the 115-day modulation exceeds the 5$σ$ global significance level, whereas the 65-day signal only marginally reaches the 4$σ$ level. Because the 115-day period is more consistent with the previously reported linear relation between orbital and superorbital periods, we interpret 115 days as the actual superorbital period, while the weaker and less stable 65-day period is its beat modulation with the orbital period.By assessing the applicability of different physical scenarios to our results, we suggest that this dual-SM behavior is most plausibly associated with corotating interaction regions (CIRs) in the stellar wind. This framework can also account for the observed linear orbital-superorbital relation, despite the unclear physical mechanism that sets the apparent ratio between the CIR and orbital periods across sources. Further long-term monitoring of this system, together with continued theoretical development of the CIR scenario, will be essential for clarifying the origin of wind-fed SMs.
[abstract 32 / 55] (score: 2) - Title: Dispersion Measure Distribution of Unlocalized Fast Radio Bursts as a Probe of the Hubble ConstantAuthors: Yang Liu, Jun-Jie Wei, Puxun Wu, Xue-Feng Wu,Comments: 12 pages, 4 figures, 2 tablesSubjects: astro-ph.CO astro-ph.HE gr-qcCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
We present constraints on the Hubble constant ($H_0$) derived from the observed dispersion measure (DM) distribution of unlocalized fast radio bursts (FRBs). While localized FRBs with redshift measurements have been used to investigate the Hubble tension, their sample remains limited. Here we demonstrate that unlocalized FRBs---which are far more numerous---can independently constrain $H_0$ without requiring redshift information, as cosmic expansion imprints itself on their DM distribution. Analyzing a selected sample of 2124 unlocalized FRBs from the CHIME Catalog II, we obtain $H_0 = 69^{+17}_{-15}~\mathrm{km\,s^{-1}\,Mpc^{-1}}$ at the $1σ$ confidence level, corresponding to an uncertainty of about 22\%. Disentangling the parametric degeneracy among $H_0$, the FRB spectral index $α$, and the characteristic cutoff energy $E_*$ of the FRB energy distribution would reduce the fractional uncertainty in $H_0$ to 9\%. This work constitutes the first $H_0$ measurement derived solely from the DM distribution of unlocalized FRBs, highlighting their potential as a new cosmological probe. Future joint analyses with localized FRBs promise even tighter constraints.
[abstract 33 / 55] (score: 2) - Title: Accretion Disks in Schwarzschild-MOG and Kerr-MOG Backgrounds: MOG Parameter in terms of Observational QuantitiesAuthors: José Miguel Rojas, Mehrab Momennia,Comments: Published version; 28 pages with 3 captioned figuresSubjects: gr-qc astro-ph.GACreated: 2026-09-23; Updated: 2026-09-25; Datestamp: 2026-09-25
We apply a general RELATIVISTIC framework to static and rotating BLACK HOLE solutions in Scalar-Tensor-Vector Gravity or modified gravity (MOG). Our results yield exact analytic, closed-form relations expressing the mass $M$, the MOG coupling parameter $α$, and the distance $D$ of a Schwarzschild-MOG BLACK HOLE in terms of a minimal set of directly measurable elements of the accretion disk: the total frequency shift, the telescope aperture angle, and the redshift rapidity. The resulting expressions are derived for particles close to the midline and line of sight, where the redshift rapidity is treated as a RELATIVISTIC invariant encoding the evolution of the frequency shift with respect to the emitter's proper time in MOG spacetime. We further extend the formalism to the rotating Kerr-MOG geometry and obtain corresponding relations that determine the rotation parameter $a$ jointly with $M$, $α$, and $D$ on the midline. In the rotating background, we introduced the redshift acceleration (general-RELATIVISTIC version of jerk) to disentangle the spacetime parameters. Crucially, the explicit appearance of $α$ in these formulas enables direct empirical estimation of this parameter, thereby providing a means to test for departures from standard general relativity. The present study focuses on the geodesic motion of massive test particles revolving around Schwarzschild and Kerr-MOG BLACK HOLEs, and the previous results obtained in the standard Schwarzschild and Kerr backgrounds are recovered in the limit $α\to 0$. The derived expressions are concise and suitable for incorporation into BLACK HOLE parameter-estimation pipelines.
[abstract 34 / 55] (score: 2) - Title: Search for quantum BLACK HOLEs in lepton+JET final states using proton-proton collisions at $\sqrt{s}=13.6$ TeV with the ATLAS detectorAuthors: ATLAS Collaboration,Comments: 37 pages in total, author list starting page 20, 4 figures, 2 tables, published in PLB. All figures including auxiliary figures are available at https://atlas.web.cern.ch/Atlas/GROUPS/PHYSICS/PAPERS/EXOT-2024-32Subjects: hep-exCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
A search for quantum BLACK HOLEs in electron+JET or muon+JET final states with high invariant mass is performed. The analysis uses data from $\sqrt{s}=13.6~\textrm{TeV}$ $pp$ collisions recorded by the ATLAS detector between 2022 and 2024 during Run~3 of the Large Hadron Collider, corresponding to an integrated luminosity of $164~\mathrm{fb}^{-1}$. This search is strongly motivated by a dramatic increase of the production cross-section by up to an order of magnitude for the highest masses considered, thanks to the small increase of $0.6~\textrm{TeV}$ in centre-of-mass energy between Run~2 and Run~3. No significant excess above the Standard Model background is observed, and 95\% CL upper limits are set on the production cross-section times branching ratio in several benchmark models, reaching a mass scale of $9.4~\textrm{TeV}$. These represent the strongest exclusion limits to date on quantum BLACK HOLE production.
[abstract 35 / 55] (score: 2) - Title: Lattice Boltzmann Methods for Navier-Stokes Equations in General Orthogonal Coordinates for Efficient Flow Simulations using Nonuniform Clustered GridsAuthors: Eman Yahia, Kannan Premnath, William Schupbach,Comments: 92 pages, 24 figuresSubjects: physics.flu-dyn physics.comp-phCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Resolving multiscale fluid flows or boundary layers effectively requires the use of nonuniform meshes with local grid clustering. The standard lattice Boltzmann method (LBM), a kinetic theory-based approach for computational fluid dynamics, however, is restricted to the use of uniform Cartesian grids. We present new and improved formulations of the LBM that accommodate continuously varying spatial grids via coordinate transformations to simulate the Navier-Stokes equations (NSE) in the general orthogonal coordinates (GOC). They are constructed using a Chapman-Enskog analysis to specify the equilibrium moments of the distribution functions and the geometric force terms used in the collision step to be dependent on the local metric factors and their spatial derivatives, along with the density, momentum and their fluxes, and some correction terms related to the normal velocity gradients so as to accurately represent the NSE in the GOC. The resulting GOC-LBM importantly maintains the simplicity of the collide-and-stream approach and is Galilean invariant that is free of the cubic velocity artifacts. Our GOC-LBM is general and modular in that it can be used with any collision model with appropriate modifications to the equilibria and forcing terms. We present its implementation details for a variety of collision models while the central moments-based model using multiple relaxation times was found to be the most robust in practical implementations. We validate the GOC-LBM through numerical simulations for various benchmark flow problems. Moreover, we demonstrate significant computational advantages of our approach for a case study on simulating boundary layer flows efficiently that involves coupling the GOC-LBM for the NSE with a new GOC-LB scheme for solving the MAGNETic induction equation for MAGNETohydrodynamics (MHD), and for another case study involving orthogonal curvilinear grids.
[abstract 36 / 55] (score: 2) - Title: Klein Tunneling of Dirac FERMIons through ElectroMAGNETic BarriersAuthors: Lingang Zhang, Hua Chen,Comments: 6 pages, 3 figuresSubjects: quant-phCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
The Lorentz covariance of RELATIVISTIC Dirac equations serves as a fundamental principle underlying the laws of electroMAGNETism across different inertial frames. Exploiting the covariance, we obtain the general solutions for Dirac fermions under both the in-plane electric $\boldsymbol{E}$ and perpendicular MAGNETic $\boldsymbol{B}$ fields, which reduce to either a MAGNETic or electric field in the inertial frame with drift velocity along the $\boldsymbol{E}\times\boldsymbol{B}$ direction. This dichotomy defines the MAGNETic and electric regimes, separated by the critical field ratio $E/B=v_\text{F}$ with $v_\text{F}$ denoting the FERMI velocity of Dirac fermions. Using these solutions, we revisit Klein tunneling through a heterojunction with generalized electroMAGNETic potentials. In the MAGNETic regime, the transmission exhibits oscillations governed by the Fabry-Pérot interference. In the electric regime, perfect transmission occurs at normal incidence in the drifted frame. The interference phase is further analyzed in terms of the solid angles on the Bloch sphere, providing a geometric interpretation of Klein tunneling. Finally, we briefly discuss the relation between the tilting of Dirac cones and the in-plane electric field, establishing the correspondence of the undertilted and overtilted cases to the MAGNETic and electric regimes, respectively. Our findings reveal the manipulation of Klein tunneling by electroMAGNETic fields, offering a theoretical basis for designing novel electronic devices.
[abstract 37 / 55] (score: 2) - Title: AstroGenesis: A Domain-Specific Multi-Agent AI for Astrophysical ResearchAuthors: N. Sahakyan, M. Khachatryan, A. Mahabal, D. Pasham, A. Khachatryan, V. Markosyan, N. Unkovskii, V. Vardanyan, D. Bégué, P. Giommi, G. Harutyunyan, D. Israyelyan, A. Tramacere, A. Casotto, Y. Wang, D. Li,Comments: Submitted to ApJ; AstroGenesis demo: https://youtube.com/shorts/vsfZ_D_XcJUSubjects: astro-ph.IM astro-ph.GA astro-ph.HECreated: 2026-09-23; Updated: 2026-09-25; Datestamp: 2026-09-25
Modern astrophysical research requires the integration of rapidly expanding scientific literature, heterogeneous observational data, and increasingly complex physical models. We introduce AstroGenesis (https://astrogenai.com), a domain-specific multi-agent AI framework that integrates literature retrieval, multiwavelength data access and analysis, theoretical modeling, and research ideation within a unified research environment.The current implementation focuses on BLAZAR research, with specialized agents coordinated by a Supervisor Agent and Planner/Replanner architecture. These agents provide capabilities for retrieving and synthesizing literature, accessing and analyzing multiwavelength observations, performing physical modeling, and identifying research directions. A central component is the Theoretical Modeling Agent, which uses pretrained neural-network surrogate models to enable efficient broadband and multimessenger modeling through natural-language interaction. The framework provides natural-language access to science-ready multiwavelength observational data and retrieval-grounded literature through a multi-stage retrieval and ranking pipeline. The literature-retrieval system was evaluated using two benchmarks: a single-paper benchmark, in which each question targets one publication, and a multi-paper benchmark, in which questions may require evidence from several publications. At least one relevant publication was retrieved among the top five results for 76.6% of the single-paper questions and 79.2% of the multi-paper questions. Representative workflows demonstrate how literature, observational data, physical modeling, and hypothesis generation can be combined within traceable analyses. The framework is extensible to additional astrophysical domains, with the goal of streamlining research workflows and enabling efficient, connected, and reproducible scientific investigations.
[abstract 38 / 55] (score: 2) - Title: Plasma instability splits axion-photon conversion linesAuthors: Elizabeth A. Tolman,Comments: Accepted for publication in Physical Review D; 12 pages, 4 figuresSubjects: hep-ph astro-ph.HE physics.plasm-phCreated: 2026-09-23; Updated: 2026-09-25; Datestamp: 2026-09-25
The axion coupling to electroMAGNETism may leave signatures of uncertain nature in astrophysical spectra; one is thought to be a single line centered at the axion frequency $ω= \sqrt{\left(m_a c^2/\hbar\right)^2 + c^2 k_a^2}$, with $m_a c^2/\hbar$ the axion Compton frequency and $\hbar k_a$ its momentum. If a parametric plasma instability is excited, this signature is transformed into a set of lines, which may be proportionally spaced and linearly polarized. A Crab pulsar signal at a frequency near recent cosmological predictions for the axion Compton frequency has some qualitative similarity to this signature, though this similarity is not evidence that the signal is caused by axions.
[abstract 39 / 55] (score: 2) - Title: A comprehensive multi-wavelength study of two X-ray emitting Be starsAuthors: Hema Anilkumar, Blesson Mathew, Savithri H. Ezhikode, Sreeja S. Kartha, Suman Bhattacharyya, Sneha Nedhath, Ajith N,Comments: 23 pages, 15 figures, This paper is accepted for publication in RAASubjects: astro-ph.SR astro-ph.HECreated: 2026-09-23; Updated: 2026-09-25; Datestamp: 2026-09-25
We present a multi-wavelength study of two X-ray-emitting Be stars, CXOU J052218.4+332820 (Star 1) and CXOU J052304.2+332846 (Star 2), identified from the LAMOST DR5 Hot emission-line stars catalog. Our spectroscopic and photometric analyses indicate that Star 1 is a main-sequence B5e star, whereas Star 2 is a pre-main-sequence B7e star. The LAMOST spectrum of Star 1 exhibits shell-type Feii, Paschen, and Oi emission from circumstellar regions extending to ~ 3 - 5Rstar. TESS period analysis reveals a rapid rotational period of ~ 0.355 d and an inclination angle of ~ 68 deg, confirming the Classical Be nature of Star 1. In contrast, Star 2 shows strong accretion signatures, including inverse P-Cygni Feii and redshifted Hei absorption features. Its ZTF light curves display irregular dimming events of up to ~ 3 mag and quasi-periodic variability on timescales of ~ 50 - 110 d, consistent with circumstellar obscuration in an accreting Herbig Be star. To further investigate the high-energy properties of the two systems, we analyzed their Chandra X-ray spectra. Chandra spectroscopy yields moderate plasma temperatures (kT ~ 1.7-1.8 keV) and X-ray luminosities of logL_X ~ 30.4-30.6 erg/s, comparable to those observed in MAGNETically active coronae. Furthermore, the positional agreement between the Chandra and Gaia coordinates indicates that the X-ray emission is spatially associated with the optical systems rather than a nearby resolved companion. These results suggest that the observed X-ray emission originates from MAGNETically influenced circumstellar activity, consistent with MAGNETically confined wind-shock (MCWS) or MAGNETically torqued disk scenarios.
[abstract 40 / 55] (score: 2) - Title: AI-Accelerated Gyrokinetic Predictions of Turbulent Transport for Stellarator Design Optimization and Experimental PlanningAuthors: R. Michael Churchill, Matt Landreman, Jong Youl Choi, Byoungchan Jang, Rory Conlin, Noah Mandell, Anima Anandkumar, Valentin Duruisseaux, Jeffrey Larson, Dario Panici, Yigit Gunsur Elmacioglu, Jai Sachdev, Tony Qian,Comments:Subjects: physics.plasm-phCreated: 2026-09-23; Updated: 2026-09-25; Datestamp: 2026-09-25
Previous work built AI-based surrogates for a nonlinear gyrokinetic simulation code with the goal of using them for fast, direct calculations of turbulent ion heat flux in stellarator design optimizations and scenario planning for experiments. These AI surrogates were trained on data from >200k nonlinear, adiabatic electron gyrokinetic simulations with the gyrokinetic flux-tube code GX, using a wide range of stellarator MAGNETic configurations ($\sim$23k), positions in the plasma, and gradient scale lengths. In this paper, we demonstrate the use of the AI-based turbulence surrogate in the optimization of stellarator MAGNETic equilibrium and to speed up stellarator transport solvers. Due to its speed ($\sim$ms), the AI-based surrogate enables previously unattainable optimization objectives, such as full radial profiles of ion turbulent heat flux, or directly optimizing to maximize the turbulent critical gradient at multiple locations across the plasma. These direct calculations provide a potentially more accurate optimization target and reduce reliance on ad-hoc heuristics that may not accurately capture the variation of turbulent transport with MAGNETic configuration. By including the AI-based surrogate for turbulent heat flux in a transport solver, we can quickly postprocess and confirm the improved ion temperature resulting from the optimized equilibrium. Finally, we demonstrate the use of AI agents with strong reasoning AI models to automate the outer loop, exploring many objective and hyperparameter configurations with this AI-based turbulence surrogate to discover improved turbulence optimized MAGNETic equilibria.
[abstract 41 / 55] (score: 2) - Title: Development and Testing of Tools for ORM Measurements and Quadrupole CenteringAuthors: A. Pathak, E. Chen, A. Shemyakin,Comments:Subjects: physics.acc-phCreated: 2026-09-23; Updated: 2026-09-25; Datestamp: 2026-09-25
In preparation for the commissioning of Linac2 (formerly referred to as the {PIP-II} linac) at FERMIlab, we are developing high-level applications that automate Orbit Response Matrix (ORM) measurement and beam-based localization of quadrupole MAGNETic centers. Both procedures are designed to run in a low-amplitude mode compatible with otherwise regular operation. The ORM is measured by exciting multiple dipole correctors simultaneously at low amplitude, each at a distinct frequency, and applying a Discrete Fourier Transform to the recorded BPM signals to extract per-element transfer function with quantified noise. One application of the measured ORM is to predict the corrector coefficients that form local orbit perturbations (bumps). To center the trajectory in a quadrupole, such a bump is created around it, the quadrupole current is oscillated, and the responses of the downstream BPMs are recorded and analyzed. Repeating this at several beam positions inside the quadrupole -- each set by the bump -- the dependence of the BPM signal on beam position provides information about the quadrupole center. The applications are being tested at the FERMIlab 400\,MeV Linac during regular production runs, and the lessons learned are fed back into their improvement.
[abstract 42 / 55] (score: 2) - Title: Simulation of ultracold plasma expansion in homogeneous MAGNETic fieldAuthors: E. V. Vikhrov, B. B. Zelener, B. V. Zelener,Comments: 6 pages, 10 figuresSubjects: physics.plasm-phCreated: 2026-09-23; Updated: 2026-09-25; Datestamp: 2026-09-25
We present molecular dynamics simulation results for an ultracold $^{40}$Ca plasma in a constant, homogeneous MAGNETic field. The MAGNETic field induces a significant spatial separation of charges. Furthermore, a significant fraction of the electrons escapes from the region bounded by the ions, in contrast to the case of plasma expansion into a vacuum. This leads to the formation of a quasineutral plasma core containing the remaining electrons and surrounded by an outer, thick ion shell, where the ion density drops sharply. Anisotropy in the ion kinetic energy is also observed, depending on the direction of ion motion relative to the MAGNETic field lines. The simulation results are in agreement with experimental data on ion dynamics.
[abstract 43 / 55] (score: 2) - Title: Quasinormal modes of type II-perturbation for dilaton-Euler-Heisenberg BLACK HOLEsAuthors: Sheng-Yuan Li, Yun Soo Myung, De-Cheng Zou, Yu-Xuan Wang,Comments: 44 Pages, 14 FiguresSubjects: gr-qcCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
We study the quasinormal modes (QNMs) of Type II perturbations for dilaton-Euler-Heisenberg (dEH) BLACK HOLEs. These perturbations consist of coupled even-parity gravitational and dilaton perturbations together with odd-parity electroMAGNETic perturbations. The background is described by mass $M$, MAGNETic charge $Q_m$, and dilaton coupling difference $ζ=α-β$ to the Euler-Heisenberg term. To find the QNM frequencies, we need to find the parameter space of $(ζ, Q_m/M)$ that is free from vector ghosts. For the $\ell=1$ mode, the radiative block couples the dilaton and axial electroMAGNETic amplitudes, whereas the $\ell=2$ mode also contains metric amplitudes, so the frequencies are obtained from matrix-valued boundary-value problems. We calculate QNM frequencies for the fundamental ($n=0$) branch with direct integration and the Chebyshev pseudospectral method, and compare the two computations wherever their charge intervals overlap. We find that the $\ell=1,2$ modes in the $n=0$ branch remain damped over the ghost-free parameter domain, supporting the stability of dEH BLACK HOLEs against Type II perturbations. The Type I sector will be presented elsewhere; no claim is made here about that sector, higher multipoles, or overtones.
[abstract 44 / 55] (score: 2) - Title: Constraining the Quadratic-mode Amplitude Coupling in GW250114Authors: Yuxin Yang, Changfu Shi, Yi-Ming Hu,Comments: 10 pages, 5 figuresSubjects: gr-qc astro-ph.HECreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Detecting quadratic quasi-normal modes in BLACK HOLE ringdowns would provide evidence for nonlinear gravitational dynamics, while measuring their properties would enable tests of the corresponding predictions of general relativity. Specifically, second-order BLACK HOLE perturbation theory predicts that their amplitudes scale with the product of the amplitudes of their parent linear modes, with a coupling coefficient that depends on the spin of the remnant BLACK HOLE. This mode-specific coupling coefficient has not yet been directly measured from gravitational wave data. Here, we use Bayesian inference on the GW250114 ringdown, modeled with the $220$, $221$, and $220\times220$ modes, to infer the amplitude-coupling coefficient of the $220\times220$ mode. The inferred coefficient is consistent with predictions from numerical relativity fits and second-order perturbation theory; no comparison shows a deviation exceeding $1.3 σ$. Although the current data cannot distinguish among these spin-dependent predictions, this measurement establishes a basis for more stringent observational tests of nonlinear gravitational dynamics in black-hole ringdowns.
[abstract 45 / 55] (score: 2) - Title: Ringdown and greybody signatures of rational regular BLACK HOLEs in non-polynomial gravityAuthors: Shohzod Jumaniyozov, Javlon Rayimbaev, Azam Payzullaev, Bahodir Ahmedov, Ilkhomjon Makhmudov, Farhod Nuraliev,Comments: 15 pages, 9 figures, 7 tablesSubjects: gr-qcCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
We study the quasinormal mode spectrum and wave-scattering properties of the four-dimensional rational regular BLACK HOLE recently obtained in non-polynomial (quasi-topological) gravity. Using third-order WKB together with two independent cross-checks a Frobenius--Riccati shooting method and a time-domain evolution we compute the fundamental scalar, electroMAGNETic, and axial gravitational-type quasinormal frequencies, validating our approach against known Schwarzschild results. We find that as the geometry approaches extremality, its dimensionless ringing frequency is systematically suppressed relative to the Schwarzschild value, a direct and quantifiable imprint of the non-polynomial regularization that we trace, via the photon-sphere correspondence, to the response of the effective potential near the horizon. A Fisher-matrix estimate indicates that this suppression could in principle be resolved by a space-based detector such as LISA for a sufficiently massive and nearby source. We further compute, for the first time, the axial gravitational-type ringdown spectrum of this geometry using the Regge--Wheeler master equation, while noting that a full stability analysis of the underlying gravity theory remains an open problem requiring the linearized field equations of the modified action. Finally, we examine the greybody transmission factors across spins $s=0,1,2$ and show that they follow the same systematic ordering and near-extremal enhancement as the ringing-frequency suppression, pointing to a common physical origin. Together, these results give one of the first quantitative characterizations of the observational signatures and the remaining open theoretical questions of a regular BLACK HOLE in modified gravity.
[abstract 46 / 55] (score: 2) - Title: Mixed-Valent Magnetism in CeFe$_2$ from Multi-Impurity DFT+DMFTAuthors: Basile Herzog, Vladislav Borisov, Olle Eriksson,Comments:Subjects: cond-mat.str-elCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
The microscopic origin of MAGNETism in CeFe$_2$ has remained unresolved for almost forty years, where polarized-neutron diffraction and x-ray MAGNETic circular dichroism infer markedly different Ce $4f$ spin and orbital moments, that also are in disagreement with theory. We show here that within a RELATIVISTIC multi-impurity DFT+DMFT framework, where the Fe $3d$ states are treated by spin-polarized T-matrix fluctuation exchange and Ce $4f$ orbitals by a bath-coupled configuration-interaction solver, this long standing problem is resolved. This level of theory is exclusive in reproducing MAGNETic moments (spin and orbital) for both the Ce and Fe atoms, yielding a total moment in agreement with the measured saturation moment. The theory put forth here is much closer to the atom specific moments reported from XMCD, compared to values from polarized-neutron diffraction. The occupation $\langle n_f\rangle=0.85$ and charge variance $δn_f^2=0.27$ establish substantial valence fluctuations, while the spectral function simultaneously recovers significant weight at the FERMI level together with separate incoherent structures. These results identify bath-mediated POLARIZATION and configuration mixing as the essential ingredients governing the electronic structure and MAGNETism of CeFe$_2$.
[abstract 47 / 55] (score: 2) - Title: Monte Carlo sampling of first-order QED processes in LASER and pulsar plasmasAuthors: Verneri Sarjomaa, Joonas Nättilä,Comments: 19 pages, 16 figuresSubjects: physics.comp-ph astro-ph.HE hep-ph physics.plasm-phCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Monte Carlo sampling of strong-field quantum electrodynamics processes underpins simulations of high-intensity LASER experiments and of astrophysical compact-object MAGNETospheres. Sampling an event requires the total rate of the process together with the cumulative probability that determines how energy is partitioned between the produced particles. Simulations typically tabulate both in advance and invert the tabulated probability numerically. Here we replace this procedure with elementary-function approximations for SYNCHROTRON radiation and the nonlinear Breit--Wheeler process. For each process, we approximate the auxiliary function that sets the total rate, as well as the cumulative probability, with Padé approximants chosen so that the inversion reduces to a quartic equation. This yields the sampled quantum parameter---electron $χ_e$ or photon $χ_γ$---in closed form. The approximations and the particle spectra sampled from them agree with the exact results to within $1\%$. The procedure requires no lookup tables, no interpolation, and no numerical root finding, and can be inserted directly into radiative particle-in-cell codes.
[abstract 48 / 55] (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: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
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 49 / 55] (score: 2) - Title: Estimates of MAGNETic field strength in the solar corona using observations of thermal radio emission at low frequenciesAuthors: Shaik Sayuf, Kathiravan C, Ramesh C,Comments: Accepted in The Astrophysical JournalSubjects: astro-ph.SRCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Measurements of the MAGNETic field strength in the solar corona at heliocentric distances $r\,{\gtrsim}\,1.1\,R_{\odot}$, using observations other than transient radio bursts, are rare. Circular POLARIZATION observations of thermal bremsstrahlung radio emission at frequencies $<$ 100 MHz, which typically originate at $r\,{>}\,1.1R_{\odot}$ in the solar corona, can be effectively used for this purpose. The thermal bremsstrahlung emission is randomly polarized, but in the presence of a MAGNETic field it propagates in two oppositely polarized circular modes whose differential absorption in the medium results in an observable circular POLARIZATION. We report a case study of two-dimensional imaging observations of the above mentioned circular POLARIZATION in the solar corona at 51\,MHz using the Gauribidanur RAdioheliograPH (GRAPH), and estimates of the associated coronal MAGNETic field strength. The peak degree of circular POLARIZATION ($dcp$), calculated from the observed total and circularly polarized intensity images with the GRAPH, is ${\approx}$2.7%. Using ray-tracing simulations we find that the observed peak $dcp$ corresponds to a radio source located at $r\,{\approx}\,1.65\,{\pm}\,0.15\,R_{\odot}$ at 51 MHz, and its field strength is ${\approx}\,1.55\,{\pm}\,0.3\,$Gauss.
[abstract 50 / 55] (score: 2) - Title: Environmental Imprints of Dark Matter and Accretion Disks on Eccentric EMRIs around Kerr Black HolesAuthors: Hai-Chao Yuan, Yong Tang,Comments: 30 pages, 11 figuresSubjects: gr-qc astro-ph.GACreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Extreme-mass-ratio inspirals (EMRIs), systems in which a stellar-mass compact object spirals into a supermassive BLACK HOLE ($M_1$), are prime targets for the space-based gravitational-wave interferometers and are acutely sensitive to their astrophysical environment. We quantify the joint imprint of a DARK MATTER (DM) spike and an accretion disk on the waveforms of eccentric, equatorial Kerr EMRIs, integrating four modular effects---DM dynamical friction, DM self-gravity, Newtonian accretion-disk torques, and disk self-gravity---into a fifth post-Newtonian (5PN) augmented analytic kludge (AAK) waveform model, and assess their measurability via a Fisher-matrix analysis. The DM dynamical-friction dephasing peaks at $M_1\sim 10^6\,M_\odot$, reaching $\sim 10^2$--$10^3\,\mathrm{rad}$; there the DM spike slope is measurable to sub-percent precision and both DM channels are unambiguously detectable, while omitting DM biases the intrinsic parameters significantly. At $M_1\gtrsim 10^8\,M_\odot$ the DM and disk self-gravity channels dominate their dissipative counterparts. The disk parameters remain degenerate across the explored parameter space, since the supersonic regime dominates the inspiral and the subsonic-to-supersonic transition only mildly weakens this degeneracy without lifting it; a combined DM$+$disk analysis further reveals a cross-sector degeneracy between the DM slope and the disk parameters. This physical degeneracy, reflected in the near-singular Fisher matrix, implies that independently measuring the disk parameters requires a RELATIVISTIC torque model or an electroMAGNETic counterpart.
[abstract 51 / 55] (score: 2) - Title: How Magnetic Fields Regulate Cooling and Mixing in Turbulent Radiative Mixing LayersAuthors: Rajsekhar Mohapatra, Lachlan Lancaster, Drummond Fielding, Eliot Quataert, Greg L. Bryan,Comments: 20+6 pages, 10+6 figures, to be submitted to MNRAS, simulation movies available at this playlist: https://www.youtube.com/playlist?list=PLcOrV9QAo3yUSubjects: astro-ph.GACreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Turbulent radiative mixing layers (TRMLs) are expected wherever hot and cold gas move past one another, including in the solar corona, galactic winds, and cold filaments in galaxy clusters. These environments are often MAGNETized, but MAGNETic effects on mixing and cooling remain less well understood than in the hydrodynamic (HD) case. We present MAGNETohydrodynamic (MHD) simulations of TRMLs at resolutions up to $1024 \times 2048^2$, spanning fields aligned with and transverse to the shear, and polarity-reversing configurations in which oppositely directed fields form current sheets at the interface. Even initially weak hot-phase fields, with $\mathcal{M}_{\rm A,shear}\equiv v_{\rm shear}/v_{\rm A}\sim14$, reduce the mass and enthalpy flux and radiative cooling rate by up to an order of magnitude relative to HD. Magnetic tension weakens turbulent motions, reducing both the diffusion of hot gas into the layer and the folding of the cooling surface. Transverse fields suppress cooling somewhat more strongly than shear-aligned ones, although a transverse field exerts no tension against the initial linear instability. Polarity reversal changes the morphology of the cooling gas without restoring HD-like mixing. The dependence on the Damköhler number is similar to the HD case, but the degree of suppression is dependent on the initial field orientation. The net cooling rate appears resolution-independent in HD but declines with resolution in MHD, and has not converged, so our suppression factors are lower limits. Magnetic fields therefore strongly regulate cooling and mixing in multiphase gas, and quantitative predictions require careful treatment of transport processes.
[abstract 52 / 55] (score: 2) - Title: Observational signatures of warped accretion flows in tidal disruption eventsAuthors: Andrew Mummery, Eliot Quataert,Comments: 42 pages, 24 figures. Submitted to ApJSubjects: astro-ph.HECreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
We analyze the possible observational signatures and evolution of global warps in the accretion flows produced in tidal disruption events. These warps are driven by Lense-Thirring torques resulting from the misalignment of the disk's rotation axis and the BLACK HOLE's spin axis. In a previous paper we argued that these global warps should be generically present in TDE accretion flows as they enter a late-time thin disk phase of evolution. We isolate three possible observational signatures of warps: (i) anomalous (reddened) late time optical colors, resulting from irradiative heating of the warped outer disk by the inner flow, (ii) delayed X-ray rises, resulting from the inner disk being slowly revealed to a distant observer as the warped flow gradually aligns with the spin axis, and (iii) reverberation of turbulent X-ray flares into optical/UV frequencies as the inner disk heats the outer disk during a flaring state. We present preliminary observational evidence that all three effects may have already been observed in TDE systems. Observations of TDEs may well offer the cleanest astronomical signatures of the strong-gravity effects which cause disk warping, and provide unique constraints on the poorly understood evolution of warped accretion disks.
[abstract 53 / 55] (score: 2) - Title: Quasi-symmetric error field correction and applications to ITERAuthors: Gwang-Geun Seo, Jong-Kyu Park, S. J. Han, M. Dubrov,Comments: 16 pages, 19 figuresSubjects: physics.plasm-phCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Reliable correction of nonaxisymmetric error fields (EFs) is essential to the safety and performance of tokamak operation. Although resonant error field correction (EFC) is well established, supported by an improved understanding of 3D plasma response, the residual fields left after resonant EFC remain an open question: they are expected to be predominantly nonresonant, yet can still degrade both confinement and stability. Here we introduce a systematic EFC scheme that minimizes resonant and nonresonant EF effects simultaneously, based on neoclassical torque response computed from self-consistent perturbed equilibria. The scheme extends the method developed for designing quasi-symmetric MAGNETic perturbations to the case where actual error fields are present. Application to standard ITER target plasmas with a range of intrinsic EF scenarios demonstrates the advantages of this quasi-symmetric (QS) EFC scheme for controlling residual EFs. QS EFC consistently yields low-torque solutions while strongly suppressing resonant response, outperforming single-mode resonant overlap EFC in most cases and approaching the performance of multimodal resonant EFC. We also show that the QS EFC solution varies only tolerably between half- and full-$I_p$ ITER scenarios, despite the greater sensitivity expected from its higher-order nature.
[abstract 54 / 55] (score: 2) - Title: DKIST unveils MHD-predicted sub-50 km photospheric vorticesAuthors: S. Vargas Dominguez, O. A. Calvo Rebellon, J. S. Castellanos Duran, M. van Noort, F. Wöger, D. A. Rodriguez Torres, C. G. Bernal,Comments: 12 pages, 3 figures, 2 tables. Submitted to Solar PhysicsSubjects: astro-ph.SRCreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Solar vortices are rotating plasma structures that play a key role in the transport of energy and MAGNETic helicity from the photosphere to the chromosphere and corona. While numerical simulations predict the existence of small-scale photospheric vortices with diameters of $50$--$100$ km, no direct observational evidence has been reported to date, primarily because of the limited spatial resolution of previous instrumentation. Here, we analyze high-resolution observations obtained with the 4-meter Daniel K. Inouye Solar Telescope (DKIST) at 416 nm, with a spatial resolution of 12.3 km. Using Fourier local correlation tracking and the swirling strength criterion ($λ_{\rm ci}$), we identify 201 vortex detections across a sequence of 143 reconstructed frames, spanning approximately 3.2 minutes, within a field of view of $4.92 \times 4.13$ Mm. The observations cover a photospheric plage region containing pore-like MAGNETic concentrations. The detected vortices have a median equivalent diameter of 38.6 km and a mean diameter of $39.5 \pm 3.3$ km. Virtually all detections are smaller than 50 km and therefore fall within the subgranular regime predicted by MAGNETohydrodynamic simulations but never previously observed. The median swirling period, $τ_{\rm ci}=37.3$ s, satisfies the $τ_{\rm ci}<100$ s criterion established by MURaM simulations. No statistically significant preference is found for prograde rotation (53.7\%) over retrograde rotation (46.3\%), consistent with the negligible influence of the Coriolis force at subgranular scales. These results demonstrate the unique capability of DKIST to resolve the population of photospheric convective vortices predicted by state-of-the-art MAGNEToconvection simulations, opening a new observational window into small-scale solar convective dynamics.
[abstract 55 / 55] (score: 2) - Title: Breaking the Blend: A multi-tracer kinematic decomposition method for IFS data applied to disentangling the AGN outflow and circumnuclear ring in NGC 5728 with JWSTAuthors: Oscar Veenema, Niranjan Thatte, Dimitra Rigopoulou, Richard I. Davies, Miguel Pereira-Santaella, Ismael García-Bernete, Almudena Alonso-Herrero, Anelise Audibert, Enrica Bellocchi, Andrew J. Bunker, Françoise Combes, Tanio Díaz Santos, Fergus R. Donnan, Donaji Esparza-Arredondo, Federico Esposito, Santiago García-Burillo, Begoña García-Lorenzo, Omaira Gonzalez Martin, Laura Hermosa Muñoz, Erin K. S. Hicks, Sebastian F. Hönig, Masatoshi Imanishi, Alvaro Labiano, Nancy A. Levenson, Enrique Lopez-Rodriguez, Cristina Ramos Almeida, Claudio Ricci, Rogemar A. Riffel, Marko Stalevski,Comments: 7 pages, 2 figures, MNRAS Letters submitted, Supplementary material available as an ancillary fileSubjects: astro-ph.GACreated: 2026-09-24; Updated: 2026-09-25; Datestamp: 2026-09-25
Integral field spectroscopy (IFS) of the central kiloparsecs of ACTIVE GALACTIC NUCLEi (AGN) reveals a mixture of spatially coincident emission from star-formation and AGN feedback exciting the interstellar medium. Disentangling these components remains a challenge, as most spectral tracers are affected by both processes, limiting robust interpretation of kinematics and energetics. We present a new framework for decomposing IFS data into distinct components on a spaxel-by-spaxel basis using a multi-tracer, stacked kinematics approach. This method combines kinematic modelling with imposed flux decomposition per spaxel, quantifying the contribution of each component across the field of view. We apply this method to JWST IFS observations of the Seyfert galaxy NGC 5728 from the Galaxy Activity, Torus, and Outflow Survey (GATOS), analysing twelve mid-infrared fine-structure lines (4.49 < $λ$ < 25.89 $μ$m, 7.9 < IP < 126.2 eV). We find that the circumnuclear emission can be decomposed into two dominant components: a star-forming ring and an AGN-driven biconical outflow. Our method separates these structures and recovers their detailed spatial morphology. This framework provides a general and scalable method for physically motivated component separation in IFS data, applicable across many wavelength ranges and targets, enabling reliable interpretation of complex emission line structures (or morphologies) in active galaxies and beyond.
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