Current date: 2026-10-07
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Scoring abstracts
Number of records retrieved: 561
Keyword score statistics
score 10 -- 1 abstracts
score 6 -- 2 abstracts
score 5 -- 2 abstracts
score 4 -- 2 abstracts
score 3 -- 9 abstracts
score 2 -- 12 abstracts
in total -- 28 abstracts
Articles that appeared on 2026-10-07
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[abstract 1 / 28] Wow! (score: 10)
- Title: Extreme superluminal expansion traces an ultra-narrow GRB JET across RELATIVISTIC regimesAuthors: Jin-Jun Geng, Ying-Kang Zhang, Hao-Xuan Gao, Jie Hu, Fan Xu, Bing Li, Tian-Rui Sun, Ai-Ling Wang, Zhi-Jun Xu, Yuan-Qi Liu, Jun Yang, Chen-Ran Hu, Lauren Rhodes, Liang Li, Yu Wang, Ye Li, Di Xiao, Jia Ren, Bing Zhang, Tao An, Xue-Feng Wu, Yong-Feng Huang, Zi-Gao Dai,Comments: 36 pages, 21 figures, updated version submittedSubjects: astro-ph.HECreated: 2026-10-06; Updated: 2026-10-07; Datestamp: 2026-10-07
The long-term evolution of GAMMA-RAY BURST (GRB) JETs from ultra-RELATIVISTIC launch to a slowly expanding radio source remains a fundamental problem in high-energy astrophysics, rarely resolved directly by imaging. We use very long baseline interferometry (VLBI) to trace the radio angular scale of GRB 221009A, the brightest GRB ever detected, from 5 to 299 days after the burst, and constrain the JET's geometry and dynamics. The Very Long Baseline Array data at 8.4 and 15.2 GHz are calibrated and imaged with AIPS and Difmap, and the source size is characterized by a circular-Gaussian model fitted to the complex visibilities. The JET dynamics, multi-wavelength emission, and source size are modeled within a two-shell collision scenario. A hydrodynamic simulation confirms that such an ultra-narrow JET undergoes lateral spreading. The observations reveal apparent superluminal expansion, with the expansion speed declining from about 90c at 5 days to about 6c at 300 days, tracing the JET's deceleration from the ultra-RELATIVISTIC to the mildly RELATIVISTIC regime and placing GRB 221009A far beyond the luminosity--velocity envelope of ACTIVE GALACTIC NUCLEi and microQUASAR JETs. Combined with the multi-wavelength afterglow, they establish an ultra-narrow RELATIVISTIC JET with a half-opening angle of about 0.01--0.03 radians, propagating through a wind-like medium at small radii before entering an interstellar-medium-like profile at larger radii. Joint modeling favors a two-phase size evolution with tentative evidence for lateral spreading. These results provide a direct geometric view of a GRB outflow and establish GRB 221009A as a benchmark for RELATIVISTIC JET physics.
[abstract 2 / 28] Yes (score: 6) - Title: Power-Law Injection Spectrum from an Ensemble of Reconnecting Current SheetsAuthors: Omar French,Comments: 9 pages, 3 figuresSubjects: astro-ph.HE physics.plasm-phCreated: 2026-10-05; Updated: 2026-10-07; Datestamp: 2026-10-07
A collisionless, low-$β$ plasma undergoing strong sub-Alfvénic turbulence is expected to form a broad hierarchy of RECONNECTing current sheets immersed in a strong guide MAGNETic field. If the RECONNECTing field strength of a sheet scales with its length as a power law of index $κ$, and the number of sheets per unit interval of sheet length decreases as a power law of index $x$, the current-sheet ensemble injects nonthermal particles with a power-law energy spectrum $\propto γ^{-s}$, where $s = 1 + (x-2)/(1 + κ)$. The spectrum is hard ($s < 2$) when the longest sheets deliver most of the injected energy, which requires $x < 3 + κ$. Past numerical studies have measured $2 \lesssim x \lesssim 3.3$, and the scalings of intense current sheets support $κ\gtrsim 0$, resulting in $1 \lesssim s \lesssim 2.3$. This injection may yield flat or mildly steep radio spectra in optically thin sources and hard ion spectra in the coronae of ACTIVE GALACTIC NUCLEi.
[abstract 3 / 28] Yes (score: 6) - Title: Investigating X-ray Emission from Radio-detected Broad- and Narrow-line Seyfert 1 GalaxiesAuthors: Minhua Zhou, Minfeng Gu, Lei Xu, Mai Liao, ZhengXue Chang,Comments: 13 pages, 13 figures, 2 Tables, Accepted for publication in Astronomy and Astrophysics (A&A)Subjects: astro-ph.HECreated: 2026-10-05; Updated: 2026-10-07; Datestamp: 2026-10-07
Context: This paper presents a study of the X-ray emission for a sample of radio-detected (RD-) broad- and narrow-line Seyfert 1 galaxies (NLS1s and BLS1s). Aims: To investigate the X-ray emission properties of early-stage accretion activity or early JETs in NLS1s. Methods: By fitting XMM-Newton X-ray spectra and combining with multi-band data from SDSS and FIRST, we conducted a statistical comparative study on the X-ray emission and multi-band correlations of NLS1s and BLS1s. Results: NLS1s and BLS1s show no significant difference in their soft X-ray blackbody temperatures, but NLS1s exhibit steeper hard X-ray photon indices and optical-to-X-ray slopes ($α_{\rm ox}$). Moreover, correlation analyses of various parameters reveal intrinsic differences in the X-ray emission between the two samples. For instance, at comparable optical luminosities, NLS1s exhibit a higher $ α_{\rm ox} $ (i.e., weaker X-ray emission), marginally distinct dependencies between radio luminosity and BLACK HOLE mass in the fundamental plane, and different correlations between $α_{\rm ox} $ and radio loudness. Based on the relationship between UV luminosity and $α_{\rm ox} $ in RQ-AGN, the estimated X-ray excess ($Δα_{\rm ox} $) in both samples is positively correlated with radio loudness. RQ-BLS1s generally display the X-ray excess, whereas RQ-NLS1s tend to show an X-ray deficiency. The Eddington ratio of RQ-NLS1s derived from X-ray luminosity is lower than that inferred from optical luminosity, further supporting their intrinsically weaker X-ray emission. Conclusions: These differences in X-ray emission between NLS1s and BLS1s may ultimately stem from the earlier evolutionary stage of NLS1s. Multivariate linear fits among radio luminosity, X-ray luminosity, and radio loudness for NLS1s and BLS1s support a multi-wavelength radiative connection associated with JETs.
[abstract 4 / 28] Yes (score: 5) - Title: Unraveling the mysteries of Jets in peculiar NLSy1 galaxies through multi-wavelength variabilityAuthors: Vineet Ojha, Xue-Bing Wu, Luis C. Ho, Raj Prince, Joysankar Majumdar, Hum Chand, Chi-Zhuo Wang,Comments: Accepted for publication in the A&A Journal. The main text includes 10 figures and 5 tables, and the appendix includes 3 figures and 1 table. A reduced abstract is presented here due to the arXiv limitSubjects: astro-ph.GA astro-ph.HECreated: 2026-10-06; Updated: 2026-10-07; Datestamp: 2026-10-07
Radio-quiet narrow-line Seyfert 1 galaxies (RQ-NLSy1s) are generally considered to be dominated by thermal emission from the accretion disk. However, recurring 37 GHz radio flares detected from seven RQ-NLSy1s by the Metsahovi Radio Observatory suggest that non-thermal processes may also contribute to their emission. We present a systematic optical and mid-infrared (MIR) variability study combined with broadband SED modeling to investigate the origin of their flux variations and assess the relative contributions of accretion disk and possible JET-related components. High-cadence optical light curves in the g, r, and i bands were obtained from ZTF, while long-term MIR light curves in the W1 and W2 bands were taken from WISE. Optical variability was quantified using the FAGN-test, peak-to-peak variability amplitude, and fractional variability, while MIR variability was characterized using redshift-corrected intrinsic variability amplitudes. Optical variability was examined from intra-night to long-term timescales, and MIR variability on long-term timescales. All RQ-NLSy1s show statistically significant long-term optical variability, with amplitudes increasing toward shorter wavelengths. Three sources exhibit bluer-when-brighter trends and increasing variability amplitudes across the optical bands, indicating a non-thermal contribution. Intrinsic MIR variability is detected in three of the four sources. Significant optical-MIR and MIR intra-band lags are observed, while optical intra-band lags are insignificant. Optical variability amplitudes are anti-correlated with the Eddington ratio and positively correlated with BLACK HOLE mass. These results suggest that a subset of RQ-NLSy1s hosts weak or intermittent JETs contributing to their optical and MIR emission, supported by SED modeling. Coordinated multi-wavelength monitoring is required to better constrain the origin of these variations.
[abstract 5 / 28] Yes (score: 5) - Title: Deriving the Continuous $β$-FPUT Model for Decayless Solar Coronal Oscillations Directly from Resistive MHDAuthors: D. Tsiklauri,Comments: Code, interactive simulation engine, and supplementary video available at https://doi.org/10.5281/zenodo.23120908 , submitted for publicationSubjects: astro-ph.SR physics.plasm-ph physics.space-phCreated: 2026-10-03; Updated: 2026-10-07; Datestamp: 2026-10-07
We present an analytical framework deriving the fluid-continuum $β$-FERMI-Pasta-Ulam-Tsingou ($β$-FPUT) system directly from a third-order resistive MAGNETohydrodynamics (MHD) expansion to explain persistent, decayless transverse oscillations observed in solar coronal loops. For a continuous wave field propagating along a longitudinal MAGNETic field with cross-field density variations, a multi-scale expansion demonstrates that quadratic $\mathcal{O}(2)$ advective and Maxwell tension terms vanish identically due to out-of-plane POLARIZATION symmetry. Instead, the quadratic longitudinal ponderomotive force drives field-aligned density modulations that back-react on the primary transverse wave, yielding a cubic $\mathcal{O}(3)$ restoring force. In the long-wavelength limit, the governing equations reduce to a fluid-continuum Modified Korteweg-de Vries (mKdV) system where cross-field profile variation provides the non-linear dispersive mechanism. We prove that this internal fluid mechanism establishes stable, amplitude-dependent frequency self-focusing, which phase-locks adjacent elements and prevents phase-mixing wave attenuation without requiring external steady driving parameterizations. This framework enables macro-scale coronal seismology, providing closed-form expressions to invert observed decayless wave-packet durations to compute the unresolved cross-field density gradient scale length ($L_x$) and the internal volumetric filling factor ($f_V$) without relying on traditional emission measure or spectroscopic line-ratio diagnostics. Much like famous Enrico FERMI's historic use of macro-scale displacements to estimate complex atomic explosion yields, this framework establishes a paradigm where monitoring macroscopic oscillation durations empowers observers to extract fine-scale, otherwise unresolvable waveguide properties.
[abstract 6 / 28] Yes (score: 4) - Title: Exploring a Cosmic-Ray Inverse-Compton Origin to the SZ-to-X-Ray Pressure Deficit in the Cool Core Cluster ZwCl 3146Authors: Emily M. Silich, Jack Sayers, Philip F. Hopkins, Charles Romero, Brian Mason, John Orlowski-Scherer, Craig L. Sarazin,Comments: updated to ApJ-accepted versionSubjects: astro-ph.HE astro-ph.COCreated: 2026-10-05; Updated: 2026-10-07; Datestamp: 2026-10-07
We explore the possibility that inverse-Compton (IC) scattering of cosmic microwave background photons by $\sim$GeV COSMIC RAYs (CRs) injected by the central ACTIVE GALACTIC NUCLEus (AGN) in cool core (CC) clusters produces a non-negligible continuum-like X-ray signal that is easily misinterpreted as intracluster medium (ICM) thermal bremsstrahlung continuum. This is particularly relevant to the cooling flow problem--the lack of STAR FORMATION relative to X-ray-inferred ICM cooling rates. Using ZwCl 3146, a relaxed CC system at $z=0.291$, we compare pressure profiles derived via X-rays and the thermal Sunyaev-Zel'dovich (SZ) effect. While SZ measurements probe only thermal ICM electrons, additional CR-IC emission would appear to boost the X-ray-inferred pressure. Relative to unity, we measure a $25\%$ decrement in $P_{SZ}/P_X$ within $100$ kpc of the ZwCl 3146 center at a statistical significance $\simeq3σ$, consistent with predicted deficits from CR-IC contamination in reasonable models of central AGN-driven CR injection. X-ray spectral fits of a two-component model with thermal ICM and CR-IC emission are consistent with CR-IC as the cause of this deficit. We test alternative explanations and systematics that could drive such a decrement, with leading-order systematics associated with halo triaxiality and AGN-driven cavities. On average, these systematics could bias $P_{SZ}/P_X$ low by $\simeq5\%$, a factor of two lower than our measurement uncertainty, with an object-to-object variation $\simeq5\%$. While our results establish that non-negligible CR-IC emission is plausible in ZwCl 3146, we stress that detailed studies of larger cluster samples are required to robustly assess whether CR-IC is relevant to the cooling flow problem.
[abstract 7 / 28] Yes (score: 4) - Title: Implementation and verification of the avalanche source in a 3D full-f particle-in-cell model of RELATIVISTIC electrons for studies of tokamak disruptionsAuthors: Fiona Wouters, Hannes Bergström, Matthias Hoelzl, Guido T. A. Huijsmans, Jan van Dijk, the JOREK team,Comments: 19 pages, 12 figures, first revisionSubjects: physics.plasm-phCreated: 2026-10-06; Updated: 2026-10-07; Datestamp: 2026-10-07
Tokamak disruptions may lead to the acceleration of some electrons to RELATIVISTIC energies. These so-called runaway electrons (REs) can multiply exponentially via knock-on collisions with thermal electrons. As the resulting RE avalanche is exponentially sensitive to the pre-disruption plasma current, multi-MA RE beams may form in large future devices, risking severe localized wall damage. In this work, an energy and momentum conserving knock-on collision operator is implemented in the 3D nonlinear MHD code JOREK for the full-f RELATIVISTIC hybrid fluid-kinetic model that describes the REs using the particle-in-cell (PiC) approach both for full-orbit and drift-kinetic markers, which will enable accurate modeling of the RE phase-space dynamics in realistic 3D electroMAGNETic fields. Such a self-consistent treatment of the RE avalanche and competing losses in the stochastic fields of MHD-active plasmas is required to further the understanding of RE transport and phase-space dynamics in self-consistent interaction with the 3D plasma evolution, which is needed for developing reliable predictions as well as reliable mitigation methods. To make such novel high-fidelity simulations computationally viable, a resampling technique was also implemented to restrict the number of markers. The avalanche model is verified using analytical expressions from literature and applied to a JET-like termination scenario, demonstrating its applicability to realistic 3D MHD active scenarios. Future work on porting to accelerated high-performance computing systems will be needed to cross the long time scales involved, e.g., in periodic termination and re-avalanching that could occur in large devices like ITER.
[abstract 8 / 28] (score: 3) - Title: Einstein ring fingerprint around supermassive BLACK HOLEs illuminated by broad line region spectral linesAuthors: Konstantinos Kostaros, George Pappas, Padelis Papadopoulos, Wing-Fai Thi,Comments: 7 pages, 4 figuresSubjects: gr-qc astro-ph.HECreated: 2026-10-05; Updated: 2026-10-07; Datestamp: 2026-10-07
The continuum emission from the hot and ionized inner regions of accretion disks around supermassive BLACK HOLEs (SMBHs), which is strongly lensed by the light ring (i.e., the unstable photon orbit) is always superimposed on that from the locally emitting plasma near the innermost stable circular orbit, masking strong-gravity effects and making their study difficult. Cleaner images of (strong-lensing)-generated brightness distributions set against a nonluminous background would thus be preferable. An SMBH illumination source that allows for this could be the more distant, cooler, neutral gas reservoir, underlying the so-called broad line region. Such a far-field illumination is ideal for producing the aforementioned images, and thus better suited for strong gravity tests. In such an illumination scenario, however, two prominent first-order effects stand out, which will be the focus of this Letter: an hourglass-like brightness distribution around the SMBH, and an associated double-peaked inner feature imprinted on the disk's global double-horned line profile, for lines of sight near the accretion disk plane. The latter effect can be discerned even in unresolved sources where only the total line profile is accessible. Interferometers operating in spectral line mode can reveal this hourglass image {\it and} the inner double peak spectral feature it imprints on the global line profile, and yield SMBH mass estimates for edge-on systems.
[abstract 9 / 28] (score: 3) - Title: Polarization Analysis of Ringdown SignalsAuthors: Nicole Khusid, Will Farr, Maximiliano Isi,Comments: 22 pages, 14 figuresSubjects: gr-qc astro-ph.HECreated: 2026-10-05; Updated: 2026-10-07; Datestamp: 2026-10-07
Merging binary BLACK HOLEs exhibit a ringdown phase in which they primarily emit gravitational waves in the shape of damped sinusoids corresponding to quasi-normal modes of the Kerr remnant. In general, each mode carries four degrees of freedom encoding amplitude and phase information. When the modes are excited with equatorial reflection symmetry, as is the case for BLACK HOLE mergers with spins (anti)aligned to the orbital angular momentum, the symmetry constrains two degrees of freedom. As a result, the relationship between POLARIZATION amplitudes and phases in each mode is fixed by the viewing (inclination) angle to the equatorial plane. We use such a constrained model to fit the ringdown signals of both non-precessing and precessing systems such as GW150914 and GW190521, respectively. We show that we can measure the degree of circular POLARIZATION and handedness of ringdown signals like those of GW150914, even if only the two LIGO detectors are available; such a POLARIZATION measurement can be translated into an inferred source inclination assuming the reflection symmetry above, again using the ringdown signal alone. On the other hand, the constrained POLARIZATION model is insufficient to capture the POLARIZATION structure of signals from precessing systems, leading to biases in the inferred mode frequencies and amplitudes. We explore the magnitude of this effect by fitting GW190521-like injections with the restricted model, finding weaker predictive accuracy relative to the arbitrary-POLARIZATION model and potentially significant systematic biases. As our detectors continue to improve, using the correct POLARIZATION model is increasingly important to avoid biased ringdown measurements.
[abstract 10 / 28] (score: 3) - Title: Granular mass perturbations on the pulsar - supermassive BLACK HOLE systemAuthors: Zexin Hu, Lijing Shao,Comments: 6 pages, 3 figures; accepted by PRLSubjects: astro-ph.HE gr-qcCreated: 2026-10-05; Updated: 2026-10-07; Datestamp: 2026-10-07
Discovery and timing observations of a radio pulsar orbiting around Sagittarius A*, the supermassive BLACK HOLE (SMBH) in our Galactic Centre (GC), will provide unprecedented opportunities of studying the SMBH spacetime, testing gravity theories, and probing the astrophysical environment in the GC. However, unknown mass distributions might cause timing residuals that are much larger than the timing precision. With extensive numerical simulations, for the first time we find that the perturbations caused by a granular cusp of stellar-mass BLACK HOLEs in the GC lead to post-fit timing residuals of 10-100 s--contrary to traditional wisdom--even for a pulsar in a tight orbit with an orbital period $P_b=0.5\,{\rm yr}$. Such a large timing residual can lead to significant measurement bias or even prevent construction of a phase-connected timing solution for the full orbit. We revisit the idea of extracting SMBH parameters only with data around periastron where the perturbation is small. Under the realistic phase-disconnected assumption, we point out that it is vital to consider the frame-dragging effect in the light propagation, which breaks parameter degeneracy and leads to an order of magnitude improvement for the measurement precision of the SMBH spin.
[abstract 11 / 28] (score: 3) - Title: Probing Direct Contributions of Galaxies and AGN to Cosmic Reionization in a Quasar Field J0226+0302 with JWST NIRCam and NIRSpecAuthors: Xiangyu Jin, Jinyi Yang, Feige Wang, Koki Kakiichi, Xiaohui Fan, Enrico Garaldi, Jaclyn B. Champagne, George D. Becker, Yongda Zhu, Yunjing Wu, Marianne Vestergaard, Huanqing Chen, Valentina D'Odorico, Anna-Christina Eilers, Jiamu Huang, Hyunsung D. Jun, Mingyu Li, Maria Pudoka, Wei Leong Tee, Minghao Yue, Huanian Zhang, Siwei Zou,Comments: 22 pages, 13 figures, 1 table, accepted for publication in ApJSubjects: astro-ph.GA astro-ph.COCreated: 2026-10-06; Updated: 2026-10-07; Datestamp: 2026-10-07
We present JWST Cycle 2 NIRCam and NIRSpec observations in a QUASAR field J0226+0302 at z=6.5412 to probe the direct connections between the intergalactic medium (IGM), galaxies, and AGN during reionization. This field was previously observed by the JWST ASPIRE program, detecting eight [OIII]-emitting galaxies at 5.3
[abstract 12 / 28] (score: 3) - Title: Pulsations and constraints on time lags in two distinct ULXs: NGC 5204 X-1 and NGC 55 ULX-1Authors: Rajath Sathyaprakash, Matthew J. Middleton, Chris Done,Comments: 25 pages and 24 Figures; comments welcomeSubjects: astro-ph.HECreated: 2026-10-06; Updated: 2026-10-07; Datestamp: 2026-10-07
The nature of ultra-luminous X-ray sources (ULXs) is shrouded in mystery as they're believed to be point sources with luminosities above the classical Eddington limit for a 10$M_{\odot}$ BLACK HOLE (BH), but generally fit into the classification tree of super-Eddington X-ray binaries. Studies of reverberation lags and lag-energy spectra provide some insight into the nature of viscous turbulence in optically thick, super-Eddington discs, and are useful in conjunction with modelling multi-wavelength spectra and covariance spectra. In this study, we focus on the timing properties of two classically distinct ULXs: NGC 5204 X-1 and NGC 55 ULX-1, both of which are known to emit RELATIVISTIC winds, as observed by modelling emission line spectra with photo-ionisation models such as SPEX, but are thought to be viewed at slightly different inclinations due to differences in the hardness-ratio of their X-ray continuum. Here, we perform an extensive timing study of the two ULXs to reveal new constraints on the accretion disc size scale and structure. We also perform an accelerated search for pulsations (including the correction for an orbital modulation of the signal) to discover significant spin-periodicities in both NGC 5204 X-1 and NGC 55 ULX-1 (at $> 3σ$ significance).
[abstract 13 / 28] (score: 3) - Title: Analytic non-axisymmetric 3D MHD equilibria without stellarator symmetryAuthors: Opal Issan, Jonathan Citrin, Matt Landreman, Brendan Tracey,Comments:Subjects: physics.plasm-phCreated: 2026-10-05; Updated: 2026-10-07; Datestamp: 2026-10-07
Analytical solutions to the three-dimensional ideal MAGNETohydrodynamic equilibrium equations $(\nabla \times \vec{B}) \times \vec{B} = \nabla p$ and $\nabla \cdot \vec{B} = 0$ provide benchmarks for stellarator equilibrium codes. Two families of non-axisymmetric solutions were recently discovered by Landreman [arXiv:2609.26742] as counterexamples to Grad's conjecture, but both satisfy stellarator symmetry. Here, we generalize both families by introducing a symmetry-breaking parameter into each of the solutions, resulting in new non-axisymmetric solutions that break stellarator symmetry and reduce to the stellarator symmetric solutions when the newly introduced parameter is set to zero.
[abstract 14 / 28] (score: 3) - Title: A spatially resolved view of Fast Radio Burst host metallicities with Integral-field SpectroscopyAuthors: Sunil Simha, Hsiao-Wen Chen, Wen-fai Fong, Sarah Hughes, Yuxin Dong, J. Xavier Prochaska, Nicolas Tejos, Tarraneh Eftekhari, Alexa C. Gordon, Stuart D. Ryder, Mawson W. Sammons, Alice P. Curtin, Victoria M. Kaspi, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Aaron B. Pearlman, Ryan M. Shannon,Comments: 14 pages, 4 figures. 4 tablesSubjects: astro-ph.HE astro-ph.GACreated: 2026-10-05; Updated: 2026-10-07; Datestamp: 2026-10-07
Magnetar sources are the leading theory for Fast Radio Burst (FRB) progenitors. If MAGNETars are indeed the dominant sources, we may thus expect any metallicity preference for MAGNETar formation to be reflected in the FRB site in host galaxies. Here, we leverage Integral Field Unit (IFU) spectroscopy to spatially resolve gas-phase metallicity distribution in five FRB host galaxies: FRB 20240210A, FRB 20240312D, FRB 20250227A, FRB 20211127I, and FRB 20250316A, at $z < 0.05$, including the FRB site, with the O3N2 index. We observed the first four sources with the newly commissioned Large Lenslet Array Magellan Spectrograph (LLAMAS) IFU on the Magellan Telescopes and used archival Keck/KCWI data for FRB 20250316A. We find ISM metallicity variations of at least 0.3 dex within individual hosts for the majority of the sample, with median values spanning $12 + log(O/H) \approx$ 8.5--8.7. At the burst sites, four have metallicities of $12 + \log(O/H) \approx 8.5$--8.9, while the fifth has a metallicity below 8.5. These findings reveal substantial metallicity variations both among FRB host galaxies and within the local environments of the bursts. Consequently, our study shows that longslit-based global estimates of host galaxy metallicity do not always represent the true burst-site distributions. We therefore advocate for IFU follow-up of larger host samples to ultimately provide FRB-site-relevant observational constraints on metallicity preferences for FRB occurrence.
[abstract 15 / 28] (score: 3) - Title: Does Diffusive Shock Acceleration Reach Steady State? Insights from a Near-Sun Shock Observed by Parker Solar ProbeAuthors: Immanuel Christopher Jebaraj, Mikhail Malkov, Nicolas Wijsen, Oleksiy Agapitov, Athanasios Kouloumvakos, Alexandr Afanasiev, Federico Fraschetti, Edin Husidic, Christina Cohen, Rami Vainio,Comments: 10 pages, 5 figures, ApJ LettersSubjects: astro-ph.SR astro-ph.HE physics.plasm-ph physics.space-phCreated: 2026-10-06; Updated: 2026-10-07; Datestamp: 2026-10-07
Collisionless shocks accelerate particles at a rate set by the diffusion coefficient of those particles in waves they themselves generate. Theory fixes that coefficient only in steady state, and no measurement has tested whether an evolving shock ever reaches that state. We report Parker Solar Probe observations of a fast, near-parallel interplanetary shock at 0.24 au, encountered four hours after eruption, with the upstream waves and the protons they scatter recorded on the same MAGNETic field line. From the wave spectra alone we derive the parallel mean free path of 0.05-30 MeV protons, resolved in energy and in distance from the shock. The mirror force of the measured compressive fluctuations supplies the scattering through the pitch angles that gyroresonance cannot reach. The mean free path grows with distance nearly as the steady self-generated solution requires, yet the steady balance holds at one energy only, near 1.3 MeV. The intensity profiles are a factor of two shallower than the measured coefficient predicts, because the waves are still growing. Confinement fails between 2.3 and 6 MeV, beginning a factor of two below what the age of the shock allows. The growth of the waves its own particles drive, rather than its age or its size, limits the energy an evolving shock confines.
[abstract 16 / 28] (score: 3) - Title: Exploring an X1.8 flare and associated quasi-periodic pulsations using SDO and Aditya-L1 observations, alongside NFFF extrapolationAuthors: Pawan Kumar, Sanjay Kumar, Sadashiv, Sachin Rajkapoor Kanaujiya, Yogesh Kumar Maurya,Comments: 21 pages, 9 figures accepted for publication in Solar PhysicsSubjects: astro-ph.SRCreated: 2026-10-06; Updated: 2026-10-07; Datestamp: 2026-10-07
The paper seeks to explore the initiation of an X1.8 class solar flare (SOL2024-10-09T0124) and the related quasi-periodic pulsations (QPPs), which are situated within NOAA active region 13848. To achieve this, we perform a multi-wavelength analysis of the event utilizing data from the Solar Dynamic Observatory (SDO) and Aditya-L1. Importantly, the observations indicate the emergence of a sigmoidal brightening at the onset of the flare, alongside the evolution of a complex morphology of flare brightenings and ribbons around the peak time of the flare. Furthermore, QPPs are detected during the impulsive phase of the flare, exhibiting a dominant period of approximately 4 minutes in the hard X-ray light curve. In order to comprehend the initiation of the flare, we construct the coronal MAGNETic field at a pre-flare stage by employing the non-force-free-field (NFFF) extrapolation model. The extrapolated MAGNETic field illustrates the existence of various significant MAGNETic features, including a MAGNETic flux rope, a three-dimensional (3D) null, sheared arcade, and quasi- separatrix layers (QSLs) within the flaring region. The recurrent RECONNECTion occurring at these features is proposed to play a role in the initiation of the flare as well as the associated QPPs.
[abstract 17 / 28] (score: 2) - Title: Simulating the jittering-JETs explosion mechanism: circum-JET rings account for observed core-collapse SUPERNOVA remnant morphologiesAuthors: Muhammad Akashi, Noam Soker,Comments: Published in the Open Journal of AstrophysicsSubjects: astro-ph.HECreated: 2026-10-06; Updated: 2026-10-07; Datestamp: 2026-10-07
We conduct three-dimensional hydrodynamical simulations of core-collapse SUPERNOVA (CCSN) explosion driven by JETs in the framework of the jittering JETs explosion mechanism (JJEM), and obtain a pair of opposite circum-JET rings similar to those observed in some CCSN remnants (CCSNRs). We launch two pairs of JETs along the same axis, the first of two opposite wide JETs, and the second of narrow JETs. The wide JETs compress the core of a stripped-envelope stellar model to form a dense, fast-expanding shell. The narrow JETs catch up with the dense shell, penetrate it, and compress the gas to the sides, forming the two opposite rings. At high inclination angles of the JETs' axis to the line of sight, the projection of each ring on the plane of the sky forms two bright zones, where the rings cross the plane of the sky. This morphology explains that of SNR G46.8-0.3. At intermediate inclination angles, the rings are fully visible as two opposite bright elliptical rims. Our simulations explain the two prominent rings on the outer shell of CCSNR G11.2-0.3. Our results strengthen the claim that the JJEM is the primary explosion mechanism of CCSNe.
[abstract 18 / 28] (score: 2) - Title: Schrödinger equations and fluctuation theorems for collisionless plasma systemsAuthors: Hideo Sugama,Comments: 25 pages , 1 figureSubjects: physics.plasm-phCreated: 2026-10-06; Updated: 2026-10-07; Datestamp: 2026-10-07
The fluctuation theorem and detailed fluctuation theorem are formulated for classical systems whose governing equations can be written in Schrödinger-type equations and which possess either a unitary or an antiunitary time-reversal operator. The initial state vector is treated as a random variable drawn from a time-reversal-symmetric probability distribution, and a stochastic relative entropy defined from its probability density is used to formulate these theorems. The framework is applied to two collisionless plasma systems: the linear Vlasov-Poisson and linear gyrokinetic systems. For the linear Vlasov-Poisson system, the governing equations are recast into Schrödinger form, and Hamiltonian eigenvectors corresponding to Case-Van Kampen modes are derived to construct explicit solutions. The stochastic relative entropy is interpreted as entropy generation associated with Landau damping, in which electric-field energy is transferred from the lowest Hermite state to higher-order Hermite states acting as thermal reservoirs. For a specific class of initial distributions, a new analytical expression for the probability density function of the stochastic relative entropy is derived and validated numerically. For the linear gyrokinetic system in a uniform MAGNETic field, the governing equations are likewise transformed into Schrödinger form, and the corresponding time-reversal operators are identified. The state-vector space is constructed as a tensor product of species, perpendicular-velocity, and parallel-velocity spaces. The resulting state vectors decompose into two orthogonal components: one coupled to electroMAGNETic fluctuations and the other corresponding to ballistic modes. These results establish a nonequilibrium statistical-mechanical framework for collisionless plasma dynamics and provide useful examples for future quantum-computing applications to plasma simulations.
[abstract 19 / 28] (score: 2) - Title: Detection of RELATIVISTIC orbital deformation from improved timing of PSR J1757$-$1854Authors: Jaikhomba Singha, Vivek Venkatraman Krishnan, Marisa Geyer, Victoria Blackmon, Paulo Freire, Norbert Wex, Maura McLaughlin, Michael Kramer, Amanda Weltman, David Champion, Matthew Bailes, Sarah Buchner, Fernando Camilo, Andrea Possenti, Maciej Serylak,Comments: 10 figures, 5 tables. Accepted for publication in MNRASSubjects: astro-ph.HECreated: 2026-10-06; Updated: 2026-10-07; Datestamp: 2026-10-07
PSR~J1757$-$1854, a 21.5\,ms pulsar, is a highly RELATIVISTIC double neutron star (DNS) system in a tight eccentric ($e = 0.61$) 4.4\,hr orbit. With extremely large gravitational wave luminosity and one of the fastest orbital decay rates of any known DNS system, it is ideal for testing general relativity (GR) in the strong-field regime. Here we present results from a high-precision timing campaign combining archival data from the Murriyang telescope and Green Bank Telescope (GBT) with new high-sensitivity observations from the MeerKAT radio telescope and additional observations from the GBT. The extended baseline and superior sensitivity of MeerKAT have yielded substantial improvements to previously measured post-Keplerian parameters by a factor of around $\sim2$ or more. We report the first detection of the RELATIVISTIC angular deformation, $δ_θ$ in this system, making PSR~J1757$-$1854 only the third DNS system for which $δ_θ$ has been measured, achieved here in just 9 yrs compared to the decades of timing required for both the double pulsar and the Hulse-Taylor binary. We demonstrate how $δ_θ$ can be used to constrain the spin-orbit geometry of the system, ruling out two of the four geometric solutions previously identified, while remaining consistent with GR. We also evaluate higher-order contributions to the periastron advance $\dotω$, including the second post-Newtonian correction and the Lense-Thirring term, and show that these have a measurable systematic effect on the inferred total system mass. The observed orbital period derivative, $\dot{P}_\mathrm{b}$ remains consistent with the GR prediction for gravitational-wave damping across a wide range of plausible distances.
[abstract 20 / 28] (score: 2) - Title: Classification of X-ray Binaries in NGC 6946 with the use of Multiwavelength DataAuthors: Senay Avdan, Hasan Avdan, Eda Sonbas, Kalvir S. Dhuga,Comments: Accepted for publication in Astrophysical Journal (ApJ)Subjects: astro-ph.HECreated: 2026-10-02; Updated: 2026-10-07; Datestamp: 2026-10-07
We identified X-ray binary (XRB) candidates in the galaxy NGC 6946 using archival {\it Chandra} data. A total of 98 XRB candidates were detected within the 0.3$-$8 keV energy range, with luminosities between 10$^{36}$ and 10$^{40}$ erg~s$^{-1}$. X-ray color-color diagrams were constructed for these sources, classifying 57 as high-mass X-ray binaries (HMXBs) and 8 as low-mass X-ray binaries (LMXBs). The X-ray temporal variability of the sources was analyzed, revealing that 40 sources exhibit variability and 26 are classified as transient sources. Possible optical counterparts for 57 sources were identified using {\it Hubble Space Telescope} ({\it HST}) images. Based on the color-magnitude diagrams (CMDs), 40 sources were found to have masses greater than 8M$_{\odot}$ and were classified as HMXBs. Seventeen sources with masses between 5 and 8M$_{\odot}$ were classified as intermediate-mass X-ray binaries (IMXBs). The remaining sources, for which optical counterparts could not be identified, were assumed to be LMXBs. The X-ray luminosity functions (XLFs) derived for HMXBs and LMXBs, identified through both X-ray and optical classification, were best described by a single power-law model ($α\sim$ 1.3$-$1.6). We supplemented traditional classification methods with a machine learning (ML) approach based on multiwavelength photometry. While traditional methods identified no AGN candidates, the ML approach detected a significant AGN population. The spatial resolution of the observing instruments and the limits of the training database hinder the reliability of the ML classifications, thus highlighting a key challenge in combining these methods for extragalactic X-ray source
[abstract 21 / 28] (score: 2) - Title: EMIR confirmation of the high-z Lyα blob SHARDS20018464Authors: S. Zarattini, F. Garzón, C. Muñoz-Tuñón,Comments: Letter accepted for publications on A&A. Four pages, four figures and one tableSubjects: astro-ph.GA astro-ph.COCreated: 2026-10-05; Updated: 2026-10-07; Datestamp: 2026-10-07
A spectroscopic follow-up of the Ly$α$ blob SHARDS20018464 was performed using the infrared spectrograph EMIR (Espectrógrafo MultiobJETo Infra-Rojo) at the 10.4 m GTC telescope, equipped with its newly upgraded H2RG focal plane array detector. We observed the blob in the Ks band, which corresponds, at the photometric redshift of $z=3.49$ presented in the literature, to the rest-frame visible part of the spectrum. Thanks to the sensitivity of EMIR, we were able to identify the [OIII] emission doublet at the position of the blob and the companion galaxy. The flux of the detected lines is of the order of $10^{-17}$ erg s$^{-1}$ cm$^{-2}$, obtained with 4-hour exposure. The mean redshift derived by analysing the two lines individually is $z=3.59\pm0.01$, slightly higher than the photometric one, although in agreement within the uncertainties. We also estimated the flux of the two lines and their ratio, which was found to be $R = 2.92$, very close to the theoretical prediction of 2.98. This is a strong analytical confirmation that the observed emissions correspond to the [OIII] doublet. Within uncertainties, the redshift of the blob confirms the photometric one reported in the literature, as well as the physical properties inferred for it. Its remarkably small size (5-8 kpc vs. $\sim 100$ kpc for typical samples) and its position aside the companion galaxy also confirm the previously-proposed idea that this object could be the first of a new class of compact Ly$α$ emitters. Moreover, the data support the scenario of photo-ionisation due to a cluster of young and massive stars.
[abstract 22 / 28] (score: 2) - Title: Uncovering the Physical Origins of Black Holes in the Milky Way for Astronomical SurveysAuthors: Ilia Kiato, Pierson Lipschultz, Vicky Kalogera, Jeff J. Andrews, Max M. Briel, Abhishek Chattaraj, Seth Gossage, Philipp M. Srivastava,Comments: Submitted to ApJSubjects: astro-ph.HE astro-ph.GA astro-ph.SRCreated: 2026-10-05; Updated: 2026-10-07; Datestamp: 2026-10-07
The observational landscape of stellar-mass BLACK HOLEs (BHs) in the Milky Way is expanding beyond X-ray binaries, with Gaia DR4 and Roman expected to open new windows onto BH populations. We use the binary population synthesis framework POSYDON to predict the present-day Galactic BH population and connect it to its evolutionary origins. We test the robustness of these predictions to uncertainties in binary evolution and BH formation, including core-collapse mechanisms, natal kicks, common-envelope efficiency, metallicity, and initial binary distributions. Across our models, we find that most Galactic BHs are isolated, with stellar mergers providing the largest contribution and binary disruptions the second largest. Among surviving binaries, detached BH-BH systems dominate. We identify a distinct, narrow feature at higher BH masses ($\simeq13\,\mathrm{M}_{\odot}$ in the fiducial model) produced by wind-driven evolution of massive Wolf-Rayet progenitors. This feature is particularly prominent among detached BH-BH binaries and persists across variations in binary-evolution and BH-formation physics, but depends strongly on metallicity. At lower masses, these BH-BH systems predominantly originate from progenitors that undergo stable mass transfer before BH formation. Finally, for more direct observational applications, we embed the synthetic populations in a Galactic model, evolve their kinematics, perform first-order microlensing calculations for BH-BH lenses, and examine BH systems with luminous companions in the context of the Gaia BHs. In the latter, we uncover a robust stable-mass-transfer population largely absent in rapid population-synthesis predictions. These results provide an evolutionary framework for interpreting the emerging Galactic BH population across complementary observational channels.
[abstract 23 / 28] (score: 2) - Title: Hierarchical Black Hole Mergers at High Redshift: Predictions for LISA and LGWA from SEEDZAuthors: Daxal H. Mehta, Lewis R. Prole, John A. Regan, Rüdiger Pakmor, Sophie Koudmani, Ricarda S. Beckmann, Michael Tremmel, John H. Wise, Martin A. Bourne, Ralf S. Klessen, Simon C. O. Glover, Martin G. Haehnelt, John Brennan, Pelle Van De Bor, Debora Sijacki, Paul C. Clark,Comments: 17 pages, 9 figures, submitted for peer review in the Open Journal of AstrophysicsSubjects: astro-ph.GA astro-ph.COCreated: 2026-10-05; Updated: 2026-10-07; Datestamp: 2026-10-07
We investigate the hierarchical assembly of BLACK HOLEs (BHs) in the early Universe using the next-generation SEEDZ cosmological zoom-in simulations. Our suite follows two independent regions (\textsc{Rarepeak} and \textsc{Normal1}) evolved with three BH feedback prescriptions: no feedback (NoFB), weak feedback (WeakFB), and standard thermal isotropic feedback (FidBH). Focusing on BH mergers at $z \geq 10$, we explore merger-driven BH growth and detectability with next-generation gravitational-wave observatories. We find that stronger AGN feedback models dramatically suppress hierarchical BH assembly compared to weaker feedback implementations. In the NoFB simulations, BHs frequently undergo repeated mergers, with some experiencing more than 50 merger events within a few hundred Myr and gaining over $10^8,\mathrm{M_{\odot}}$ through mergers alone. In contrast, BHs in the FidBH simulations rarely undergo more than three mergers. NoFB therefore represents an upper limit to BH merger-driven growth beyond what is expected in the Universe. The suppression of BH mergers in the FidBH case is not driven by differences in galaxy assembly, BH occupation fractions, or BH seed abundances, which remain broadly similar across the simulation suites. Instead, feedback disrupts the dense gas surrounding newly formed BH seeds, suppressing their early accretion-driven growth and preventing them from entering runaway hierarchical merger pathways. Our results demonstrate that early-Universe feedback prescriptions strongly influence hierarchical BH growth through both mergers and accretion, producing distinct high-redshift merger populations. Coupled with seeding choices and other BH subgrid prescriptions, this introduces multiple degeneracies that will need to be broken in advance of LISA and other next-generation GW facilities.
[abstract 24 / 28] (score: 2) - Title: An Implicit, Moment-Conserving Low-Rank Tensor Method for the Hybrid Kinetic-Ion Fluid-Electron Plasma ModelAuthors: Stephen R. White, Adam J. Stanier, Luis Chacón, Will T. Taitano, Isaac A. Castro,Comments: 32 Pages, 10 Figures, 4 Tables, 2 AlgorithmsSubjects: physics.plasm-phCreated: 2026-10-05; Updated: 2026-10-07; Datestamp: 2026-10-07
Quasi-neutral hybrid models for simulating plasmas, with kinetic ions and fluid electrons, have shown great promise for approaching the multi-scale nature of plasmas. In this paper we present a novel hybrid scheme for electroMAGNETic settings that conserves mass, momentum, and energy, employing a low-rank tensor method utilizing the Tensor Train decomposition to avoid the \enquote{curse of dimensionality.} Electrons are simulated as a continuous fluid, while the kinetic ions are modeled as a distribution function governed by the Vlasov equation. The Vlasov equation is updated with the implicit midpoint method. We use a modified version of a conservative truncation method to guarantee conservation of mass, momentum, and energy throughout the method, which corrects the truncated distribution function without needing to advance a separate set of fluid-moment equations. A series of electrostatic and electroMAGNETic test problems is used to demonstrate the correctness of the method and its conservation properties.
[abstract 25 / 28] (score: 2) - Title: Chana: A GPU-Accelerated AMR GRRMHD CodeAuthors: Tianshu Wang,Comments: 16 pages, 10 figures. Submitted to ApJSSubjects: astro-ph.HE astro-ph.IMCreated: 2026-10-05; Updated: 2026-10-07; Datestamp: 2026-10-07
This paper presents Chana, a GPU-accelerated, block-structured adaptive-mesh code for general RELATIVISTIC MAGNETohydrodynamics, multigroup M1 neutrino transport, and dynamical spacetime evolution using the Z4c formulation. Each physical module uses independently selected spatial discretizations and ghost-zone widths to balance accuracy and computational cost. Stiff radiation-matter interactions are treated implicitly, with Jacobians calculated analytically from the chain-rules. The code is written in C++20 and it uses MPI and Kokkos 5 for distributed-memory and performance-portable parallelism. The code is validated through a number of GRMHD, radiation transport, and dynamic spacetime tests. For a representative core-collapse SUPERNOVA configuration with three neutrino species and 12 energy groups per species, the code achieves approximately $1.1 \times 10^6$ cell updates per GPU second on NVIDIA A100 GPUs using four-stage RK4 integration. Weak-scaling efficiency remains above 85\% up to 256 GPUs on Perlmutter.
[abstract 26 / 28] (score: 2) - Title: Multiple H I 21-cm absorbers towards BLAZAR PKS 1158+007Authors: Abhisek Mohapatra, R. Srianand, R. Dutta,Comments: 12 pages, 5 figures, 3 tables. Accepted for publication in ApJSubjects: astro-ph.GACreated: 2026-10-05; Updated: 2026-10-07; Datestamp: 2026-10-07
We report an interesting line of sight towards the BLAZAR PKS 1158+007 (J1201+0028) ($z_{\rm em}$ = 1.369), revealing the rare detection of two intervening HI 21-cm absorption systems within a narrow redshift interval ($Δz \sim 0.04$) using the MeerKAT radio telescope. The stronger absorber at $z_{\rm abs}$ $=0.5653$ ($\intτdv = 1.31\pm0.04$ \kms) is associated with a strong MgII $\lambda2796$ system seen in the Sloan Digital Sky Survey (SDSS) and Dark Energy Spectroscopic Instrument (DESI) spectra, with rest-frame equivalent widths of $W_{2796} = 1.40\pm0.07$~Å and $1.21\pm0.11$~Å, respectively. In stark contrast, the second detection at $z_{\rm abs}$ $= 0.5305$ reveals a distinct HI 21-cm absorption feature ($\intτdv = 0.31 \pm 0.04$ \kms) with no associated metal absorption detectable in the optical spectra. This system represents a prime example of a "metal-poor'' HI 21-cm absorber. Using photometric redshifts from Hyper Suprime-Cam (HSC) PDR3 and DESI Legacy Surveys DR10, we identify a broad galaxy overdensity (at $z \sim0.53\pm0.06$) coincident with these absorbers, suggesting the sightline pierces a complex large-scale structure or filament, which would be interesting to confirm with follow-up observations. These results underscore the power of blind HI 21-cm surveys to uncover the "invisible'' cold gas phase of the Universe that optical/UV metal-line selection may systematically miss.
[abstract 27 / 28] (score: 2) - Title: Adiabatic confinement and escape in an open billiardAuthors: Matheus Rolim Sales, Leonardo Costa de Souza, Ricardo Luiz Viana, Edson Denis Leonel, Iberê Luiz Caldas,Comments:Subjects: nlin.CD physics.plasm-phCreated: 2026-10-05; Updated: 2026-10-07; Datestamp: 2026-10-07
We introduce a stationary, field-free billiard that reproduces the adiabatic confinement mechanism of a MAGNETic mirror through boundary geometry alone. Rapid transverse reflections generate an approximately conserved action that plays the role of the MAGNETic moment, producing an effective longitudinal barrier and a nominal loss cone for escape. For the half-width profile considered here, confinement is controlled by a competition between mirror strength and adiabaticity: shortening the profile increases the mirror ratio but also reduces the accuracy of the adiabatic approximation. As a result, the escaping fraction is nonmonotonic and confinement is strongest at an intermediate profile length. We characterize the associated phase-space structure, escape-time statistics, and escape basins, revealing long-lived transient motion and a strong sensitivity of the final escape direction to the initial condition that persists as the uncertainty in the initial condition is reduced.
[abstract 28 / 28] (score: 2) - Title: Radiation pressure powers QUASAR broad absorption line winds but fails to drive galaxy feedbackAuthors: Braden Seefeldt-Gail, Lluís Mas-Ribas, Norman Murray,Comments: 21 pages, 5 figures; supplementary material: 31 pages, 17 figures, 2 tables. Submitted to Science AdvancesSubjects: astro-ph.GACreated: 2026-10-06; Updated: 2026-10-07; Datestamp: 2026-10-07
Most cosmological simulations invoke QUASAR-driven winds as the primary mechanism quenching STAR FORMATION in massive galaxies, assuming wind momentum flux approaches the radiation-pressure maximum, $L/c$. Using 81,388 broad absorption line troughs from the SDSS-IV DR16 QUASAR catalog and detailed mock trough spectra, we detect line locking, a spectral signature of radiation-pressure-driven outflows, in 60 to 70 percent of troughs, demonstrating that radiative line driving dominates wind acceleration and ruling out alternative mechanisms. Direct measurement of the wind energy budget yields a median kinetic luminosity of only 0.01 percent of bolometric luminosity, 50 times below the level required for effective feedback. Line-driven QUASAR winds are therefore insufficiently powerful to quench STAR FORMATION, challenging the primary physical mechanism invoked for BLACK HOLE feedback in galaxy formation models.
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