Current date: 2026-06-05
Setting default datestamp limit: 0
Datestamp limit: 2026-06-05 (0 days ago)
Created/updated limit: 2026-05-29 (7 days ago)
Found keywords_cs.datFound keywords_cis.dat
Suggested sets: physics, physics:astro-ph, physics:gr-qc, physics:physics
Setting default set: physics
OAI-PMH request: http://export.arxiv.org/oai2?verb=ListRecords&from=2026-06-05&until=2026-06-05&set=physics&metadataPrefix=arXiv
Scoring abstracts
Number of records retrieved: 692
Keyword score statistics
score 8 -- 1 abstracts
score 7 -- 1 abstracts
score 6 -- 6 abstracts
score 5 -- 4 abstracts
score 4 -- 4 abstracts
score 3 -- 11 abstracts
score 2 -- 15 abstracts
in total -- 42 abstracts
Articles that appeared on 2026-06-05
-
[abstract 1 / 42] Wow! (score: 8)
- Title: Constraining Orbital Eccentricity of a Supermassive Black Hole Binary Candidate PKS 2131-0211Authors: Avinash Kumar Paladi, A. Gopakumar, Sushmita Agarwal, Fazal Kareem,Comments:Subjects: astro-ph.HE astro-ph.GACreated: 2026-06-03; Updated: 2026-06-05; Datestamp: 2026-06-05
A detailed analysis of the decades-long radio light curve of BLAZAR PKS 2131-021 showed epochs of sinusoidal variations in the radio flux density time-series as detailed in O'Neill et al. (2022). The observed sinusoidal flux modulation arises naturally from RELATIVISTIC Doppler boosting of the JET when the JET-emitting supermassive BLACK HOLE (SMBH) orbits its companion. For SMBHs in circular orbits, this scenario yields sinusoidal light curves, offering a simple kinematic explanation for the observed variability in PKS 2131-021. We present an approach that incorporates the effects of orbital eccentricity into the Kinematic Orbital model for PKS 2131-021, using the Keplerian parametric solution to describe the SMBH binary orbit. Using the available radio light curve data, we demonstrate that the proposed SMBH binary likely possesses a residual orbital eccentricity, which we constrain through detailed Bayesian parameter estimation studies to be 0.053 \pm 0.015 with a Bayes factor of 3.15 over the circular model. However, when the analysis accounts for the presence of red noise in the data using a Damped Random Walk (DRW) process, the circular model is preferred, giving an eccentricity upper limit of e < 0.15. Nevertheless, our efforts reveal that the Circular+DRW model is strongly favored. This model consistently recovers a coherent periodic signal across all datasets, with the orbital period remaining well-defined even when accounting for broader uncertainties. This analysis incorporated archival observations from the Haystack Observatory, the University of Michigan Radio Astronomy Observatory (UMRAO), and the Owens Valley Radio Observatory (OVRO), spanning the period from 1975 to 2021, compiled by O'Neill et al. (2022).
[abstract 2 / 42] Wow! (score: 7) - Title: The WISSHFUL program: the highest redshift UFO discovered in a non-lensed QSOAuthors: G. Lanzuisi, L. Borrelli, E. Piconcelli, G. Chartas, A. Luminari, J. Reeves, V. Braito, E. Bertola, S. Bianchi, A. Comastri, M. Brusa, C. Vignali, F. Vito, S. Marchesi, M. Cappi, M. Dadina, L. Zappacosta, A. Tortosa, M. Bischetti, G. Vietri, F. Salvestrini, G. Bruni, M. Fanelli, E. Kammoun, X. Zhao, G. Matzeu, F. Tombesi, A. Marinucci, M. Gaspari, T. Misawa, D. Stern,Comments: Under minor revision in A&ASubjects: astro-ph.HE astro-ph.GACreated: 2026-06-03; Updated: 2026-06-05; Datestamp: 2026-06-05
We present the first results from the WISSHFUL program, an XMM-Newton heritage program targeting luminous QSOs at Cosmic Noon. We report on recent simultaneous XMM-Newton and NUSTAR observations of the Super-Eddington accreting QUASAR WISSH13 at z=3.294, which provide the highest quality broadband X-ray spectrum to date for a non-lensed QSO at this redshift. Physical modeling of the continuum reveals a soft photon index ($Γ\sim2$) and strong reflection ($R\sim1.4-1.8$), despite the weak narrow Fe emission, and a low high-energy cut-off ($E_{cut}\sim60-80$ keV, $kTe = 15-20$ keV, depending on the model adopted). Most notably, we detect two significant (at $96.7\%$ and $98.9\%$ confidence level, respectively) absorption features at $\sim7.5$ and $\sim10$ keV rest-frame, interpreted as a blueshifted blend of Fe XXV He$α$ and Fe XXVI Ly$α$. These features indicate the presence of two kinematic components of a highly ionized, high column Ultra-Fast Outflow (UFO) with a velocity of $v_{out}\sim0.1c$ and $v_{out}\sim0.3c$, respectively. The slower wind is consistently detected in an archival 2017 XMM-Newton observation, whereas the faster wind is detected only in 2024. This stratified and variable wind exhibits extreme energetics, with a mass outflow rate of $\dot{M}_{out}\sim20M_{\odot}/yr$ (corresponding to $15\% \dot{M}_{acc}$) for each component, and a kinetic power of the order of $\sim1$ and $\sim10\%$ of the bolometric luminosity, respectively. While this represents one of the most powerful UFOs ever detected, its kinetic power is a similar fraction of the QSO's bolometric luminosity compared to lower-redshift AGN. We present several theoretical frameworks to explain the peculiar accretion and ejection properties of this remarkable QSO at Cosmic Noon.
[abstract 3 / 42] Yes (score: 6) - Title: Prospects for optical detections from binary neutron star mergers with the next-generation multi-messenger observatoriesAuthors: E. Loffredo, N. Hazra, U. Dupletsa, M. Branchesi, S. Ronchini, F. Santoliquido, A. Perego, B. Banerjee, S. Bisero, G. Ricigliano, S. Vergani, I. Andreoni, M. Cantiello, J. Harms, M. Mapelli, G. Oganesyan,Comments: Corrected typo in coefficient b of equation (11). Main paper: 24 pages, 17 figures, 5 tables. Total with appendices: 35 pagesSubjects: astro-ph.HECreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
Next-generation gravitational wave (GW) observatories, such as the Einstein Telescope (ET) and Cosmic Explorer, will observe binary neutron star (BNS) mergers across cosmic history, providing precise parameter estimates for the closest ones. Innovative wide-field observatories, such as the Vera Rubin Observatory, will quickly cover large portions of the sky with unprecedented sensitivity to detect faint transients. This study aims to assess the prospects for detecting optical emissions from BNS mergers with next-generation detectors, considering how uncertainties in neutron star (NS) population properties and microphysics may affect detection rates. Starting from BNS merger populations exploiting different NS mass distributions and equations of state (EOSs), we model the GW and kilonova (KN) signals based on source properties. We model KN ejecta through numerical-relativity informed fits, considering the effect of prompt collapse of the remnant to BLACK HOLE and new fitting formulas appropriate for more massive BNS systems, like GW190425. We include optical afterglow emission from RELATIVISTIC JETs consistent with observed short GAMMA-RAY BURSTs. We evaluate the detected mergers and the source parameter estimations for different geometries of ET, operating alone or in a network of current or next-generation GW detectors. Finally, we estimate the number of detected optical signals simulating realistic observational strategies by the Rubin Observatory. ET as a single observatory will enable the detection of about ten to a hundred KNe per year by the Rubin Observatory. This improves by a factor of about 10 already when operating in the network with current GW detectors. Detection rate uncertainties are dominated by the poorly constrained local BNS merger rate, and depend to a lesser extent on the NS mass distribution and EOS.
[abstract 4 / 42] Yes (score: 6) - Title: Discovery of a Featureless Tidal Disruption Event at z~1 with the Wide Field Survey TelescopeAuthors: Jiazheng Zhu, Zelin Xu, Ning Jiang, Ji-an Jiang, Tinggui Wang, Yuhan Yao, Ryan Chornock, Erica Hammerstein, Yibo Wang, Min-Xuan Cai, Shifeng Huang, Wenkai Li, Mingxin Wu, Chichuan Jin, Jie Lin, Jianwei Lyu, Dezheng Meng, Weiyu Wu, Zhengyan Liu, Junhan Zhao, Ziqing Jia, Chengyi Wang, Lulu Fan, Xu Kong, Feng Li, Ming Liang, Jinling Tang, Hairen Wang, Jian Wang, Yongquan Xue, Ji Yang, Hongfei Zhang, Wen Zhao, Qingfeng Zhu,Comments: 12 pages, 6 figures, published for ApJLSubjects: astro-ph.HECreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
We report the discovery of tidal disruption event (TDE) WFST250820mmsw/AT2025wet by the 2.5-meter Wide Field Survey Telescope (WFST). It exhibits a blue nuclear flare throughout the observed evolution with a g-band peak magnitude ~22, which is about 3 magnitudes brighter than its host galaxy. A Keck/LRIS spectrum taken near the optical peak reveals a featureless blue continuum, with no discernible emission lines. However, its redshift can be accurately determined to be 1.037 by its host galaxy absorption lines. Blackbody fits to the multiband spectral energy distribution (SED) of AT2025wet yield a constant temperature of ~19,000K and a peak luminosity of (8.27 +0.92 -0.71)*10^44 erg s^-1 while actually the SED likely peaks at a much shorter wavelength than a 19,000K blackbody. The SED modeling of the host galaxy implies a stellar mass of ~10^11.2 M_odot and an estimated central BLACK HOLE mass of ~10^8 M_odot, with no evidence of significant ACTIVE GALACTIC NUCLEus activity prior to the flare. All of these observations are well consistent with a featureless TDE scenario, making it the highest-redshift non-JETted TDE known to date. TDEs at such high redshift provide us a unique opportunity to explore the intrinsic SEDs of TDEs, particularly to test whether they peak in the extreme-UV regime, thereby addressing the missing energy puzzle and the origin of optical emission in TDEs. Ongoing surveys represented by WFST and the Legacy Survey of Space and Time (LSST) are expected to discover an increasing number of TDEs at higher redshifts, which will extend our census of SMBHs across redshift space and help unravel the mysteries of optical TDEs through direct probes of their UV emission.
[abstract 5 / 42] Yes (score: 6) - Title: Radiation-induced electron spin POLARIZATION in ultraRELATIVISTIC kinetic turbulenceAuthors: Peng Liu, Karen Z. Hatsagortsyan, Christoph H. Keitel, Zheng Gong,Comments: Comments are welcomeSubjects: physics.plasm-ph astro-ph.HECreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
Electron spin POLARIZATION in radiative plasmas with ultraRELATIVISTIC kinetic turbulence under highly MAGNETized conditions is investigated using particle-in-cell simulations. We observe that a significant spin POLARIZATION can be sustained when the leptons undergo energetic photon emission accompanied by spin flips during the nonequilibrium turbulent evolution. By analyzing the time evolution of spatially dependent spin POLARIZATION, we identify an electroMAGNETic (EM) regime of kinetic turbulence, distinct from the well-known density-dominated regime characterized by vortex currents and MAGNETic islands. While in the latter regime the spin POLARIZATION exists only transiently, in the EM regime significant anisotropic net POLARIZATION emerges and persists in non-dissipative scenarios. The correlation between spin signals and turbulence features is leveraged to introduce the characteristic parameter delimiting the EM regime via the ratio of electric and MAGNETic energy densities and to gain insight into complex plasma turbulence. This study demonstrates the versatility of a spin-resolved study of the plasma turbulence in extreme environments, such as BLACK HOLEs and MAGNETar MAGNETospheres.
[abstract 6 / 42] Yes (score: 6) - Title: Joint Multi-Period FERMI-LAT and LHAASO Constraints on Axion-Like Particles from Mrk 421 Using Profile Likelihood with Gaussian Copula CorrelationAuthors: Longhua Qin, Jiancheng Wang, Chuyuan Yang, Huaizhen Li, Ao Wang, Weiwei Na, Hushan Xu, Xiaogu Zhong, Zunli Yuan, Yubin Li, Guangbo Long,Comments: Ready to submit; comments are welcomeSubjects: astro-ph.HECreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
We construct a multi-epoch joint profile-likelihood framework to constrain axion-like particles (ALPs), employing a Gaussian copula ($ρ=0.03$) to account for weak correlations among distinct observational periods. Different from traditional independent likelihood addition, our scheme globally optimizes nuisance parameters under the no-ALP hypothesis prior to profiling ALP mass $m_a$ and coupling $g_{aγ}$, enhancing numerical stability and statistical consistency. Using five sets of simultaneous FERMI-LAT and LHAASO data of Mrk 421, we implement both two-zone hybrid and single-zone hadronic JET models. In the CAST-sensitive low-mass regime $m_a\lesssim1$ neV, the 95\% CL upper limit of $g_{aγ}$ is $8.33\times10^{-14}\,\mathrm{GeV}^{-1}$. Over $0.1$-$500$ neV, conservative bounds read $g_{aγ}<6.50\times10^{-12}\,\mathrm{GeV}^{-1}$ (two-zone) and $g_{aγ}<7.30\times10^{-12}\,\mathrm{GeV}^{-1}$ (single-zone). These results benefit from LHAASO's broadband very high energy coverage and long term monitoring of Mrk 421; the developed framework provides a robust and scalable pipeline suitable for future multi-messenger ALP searches with next-generation gamma-ray observatories.
[abstract 7 / 42] Yes (score: 6) - Title: Modeling Gamma-Ray Burst Spectra with Convolutional Neural Networks: Fast-Cooling Synchrotron Emission in a Decaying Magnetic FieldAuthors: Jia-Ming Chen, Ke-Rui Zhu, Shan Chang, Zhao-Yang Peng, Yong-Gang Zheng, Li Zhang,Comments: 20 pages, 9 figures,accepted for publication in ApJSubjects: astro-ph.HECreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
The radiation mechanism of GAMMA-RAY BURST (GRB) prompt emission remains uncertain. Although the fast-cooling SYNCHROTRON model in a decaying MAGNETic field can account for the characteristic nonthermal spectral shape, its computational cost has limited its use in systematic observational fitting and statistical model comparison. We develop a convolutional neural network (CNN)-based spectral emulator for this physical model and train it on a large synthetic data set generated over a physically motivated parameter space. The trained network reproduces the numerical spectra with high fidelity while reducing the cost of spectral evaluation to the millisecond level. We then incorporate the emulator into a Bayesian spectral-analysis framework and apply it to the time-resolved spectra of GRB 231020A observed by FERMI/GBM. In most time intervals, the decaying-field fast-cooling SYNCHROTRON model provides better fits and smaller Bayesian information criterion values than the standard fast-cooling SYNCHROTRON model. These results suggest that a radially decaying MAGNETic field provides a plausible and more physically motivated interpretation of the prompt-emission spectrum of this burst, while also indicating that the emulator offers a practical route for large-sample Bayesian inference and systematic comparisons of GRB prompt-emission models.
[abstract 8 / 42] Yes (score: 6) - Title: Probing a new subclass of llGRB-SN transients: Insights from EP250304a and its associated SUPERNOVAAuthors: L. Cotter, A. Martin-Carrillo, R. A. J. Eyles-Ferris, L. Izzo, D. B. Malesani, Y. Julakanti, G. Corcoran, A. Saccardi, P. G. Jonker, A. J. Levan, F. Carotenuto, P. T. O'Brien, J. H. Gillanders, J. N. D. van Dalen, M. E. Ravasio, S. Schulze, N. Sarin, F. E. Bauer, M. Fraser, J. Quirola-Vasquez, A. P. C. van Hoof, S. J. Smartt, C. Gall, A. Rest, C. T. Murphey, N. Tanvir, T. -W. Chen, S. Campana, C. Ashall, J. P. Anderson, J. A. Chacon, F. J. Cowie, V. D'Elia, L. Galbany, C. P. Gutierrez, D. H. Hartmann, P. Jakobsson, S. Kobayashi, A. H. Kong, P. Mazalli, T. E. Muller-Bravo, M. De Pasquale, L. Rhodes, A. Rossi, J. Sanchez-Sierras, J. Sollerman, A. Andersson, A. Aryan, T. de Boer, J. S. Bright, K. C. Chambers, M. Gromadzki, M. E. Huber, C. Inserra, T. Lowe, P. Minguez, G. S. Narayan, M. Nicholl, G. S. H. Paek, A. Sedgewick, K. W. Smith, J. W. Tweddle, S. Yang,Comments: 21 pages, 21 figuresSubjects: astro-ph.HECreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
With the advent of the Einstein Probe (EP) mission, we are entering a new era in the study of GAMMA-RAY BURSTs (GRBs), enabling the detection of faint, low-luminosity transients that would previously have gone undetected. EP250304a was an event discovered by EP associated with the broad-lined type Ic SUPERNOVA (SN) SN 2025fhm located at z = 0.2. Despite no gamma-ray emission being detected at the time of the EP trigger, we identify evidence for a RELATIVISTIC outflow consistent with a GRB-like JET across multiple wavelengths. We present a detailed spectral and photometric analysis of EP250304a/SN 2025fhm, including multi-band light curve modelling performed with the Redback Python package. We find that this event closely resembles low-luminosity GRB-SNe (llGRB-SNe) such as GRB 060218/SN 2006aj, GRB 100316D/SN 2010bh, and GRB 171205A/SN 2017iuk, all of which exhibit early-time emission consistent with a thermal shocked cocoon. These similarities suggest that EP250304A/SN 2025fhm may belong to an emerging subclass of shocked cocoon-dominated llGRB-SNe, representing the low-luminosity end of a broader continuum of engine-driven GRB-SN explosions.
[abstract 9 / 42] Yes (score: 5) - Title: Probing millisecond MAGNETar formation in binary neutron star mergers through X-ray follow-up of gravitational wave alertsAuthors: Clara Plasse, Alexis Reboul-Salze, Jérome Guilet, Diego Götz, Nicolas Leroy, Raphaël. Raynaud, Matteo Bugli, Tito Dal Canton,Comments:Subjects: astro-ph.HECreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
The nature of the remnant of a binary neutron star (BNS) merger is uncertain. Though certainly a BLACK HOLE (BH) in the cases of the most massive BNSs, X-ray lightcurves from GAMMA-RAY BURST (GRB) afterglows suggest a neutron star (NS) as a viable candidate for both the merger remnant as well as the central engine of these transients. When jointly observed with gravitational waves (GWs), X-ray lightcurves from BNS merger events could provide critical constraints on the remnant's nature. We aim to assess the current and future capabilities to detect a NS remnant through X-ray observations following GW detections. To this end, we simulate GW signals from BNS mergers and the subsequent X-ray emission from newborn millisecond MAGNETars. The GW detectability is modeled for both current and next-generation interferometers, while the X-ray emission is reproduced using a dedicated numerical code that models MAGNETar spin-down and ejecta dynamics informed by numerical-relativity simulations. In our simulations, 2% - 16% of BNS mergers form millisecond MAGNETars. Among these, up to 70% could be detectable, amounting to up to 1 millisecond MAGNETar detection per year with SVOM/MXT-like instruments during the LIGO Virgo KAGRA LIGO India (LVKI) O5 run, with optimal detectability occurring about 2 hours post-merger. For next-generation GW interferometers, this rate could increase by up to three orders of magnitude, with peak detectability 3 to 4 hours post-merger. We also explore how the MAGNETar's MAGNETic field strength and observer viewing angle affect detectability and discuss optimized observational strategies. Although more likely with upcoming GW interferometers, detecting the spin-down emission of a millisecond MAGNETar may already be within reach, warranting sustained theoretical and observational efforts given the profound implications for mergers, GRBs, and NS physics of a single detection.
[abstract 10 / 42] Yes (score: 5) - Title: Constraining the JET base emission of M87* with past and future Event Horizon Telescope observationsAuthors: Noemi La Bella, Michael Janssen, Britton Jeter, Hendrik Müller, Bram Van de Berg, Hung-Yi Pu, Paul Tiede, Heino Falcke,Comments: Accepted for publication in Astronomy & Astrophysics; 14 pages, 10 figuresSubjects: astro-ph.HECreated: 2026-06-03; Updated: 2026-06-05; Datestamp: 2026-06-05
We investigate the detectability of the JET base of M87* at Event Horizon Telescope (EHT) observing frequencies. Although M87 is known to host a prominent RELATIVISTIC JET, detecting JET emission close to the BLACK HOLE at horizon scales remains challenging. Our goal is to determine the minimum JET intensity that can be reliably detected with the recent EHT array configurations. We use synthetic EHT data generated for three array configurations corresponding to the 2021 and 2022 observing campaigns and to a near future EHT campaign. As input models, we employ semi analytic accretion JET models in which the JET emission can be tuned independently of the accretion flow. The synthetic data are reconstructed with regularized maximum likelihood and Bayesian imaging. Jet detectability is assessed through flux density recovery, image fidelity, and uncertainty maps. We find that JET detectability strongly depends on the JET intensity, the array configuration, and imaging methodology. Using our analysis, we determine a lower limit on the JET intensity that can be reliably recovered. The 2022 EHT array configuration represents a significant improvement over earlier arrays, enabling a more robust reconstruction of faint JET features. Our results indicate that the current EHT array is already sensitive to weak JET emission at horizon scales in M87*. The improved short-baseline coverage introduced in 2022 makes faint inner JET features more easily detectable. If the inner JET contributes a significant fraction of the unresolved compact flux, it should become visible in post-2021 observations. On the other hand, if no clear JET signature is found, this would suggest that the horizon-scale JET contributes only a small part of the compact emission. The continued expansion of the EHT will further improve the detection of such JET emission in M87*.
[abstract 11 / 42] Yes (score: 5) - Title: Complex Analysis of Askaryan Radiation: UHECR Reconstruction with Askaryan Radio ArrayAuthors: J. C. Hanson, D. Ibanez-Rodriguez,Comments:Subjects: astro-ph.HECreated: 2026-06-03; Updated: 2026-06-05; Datestamp: 2026-06-05
Ultra-high energy COSMIC RAYs (UHECR) can produce RELATIVISTIC cascades that emit radio-frequency (RF) pulses in the 0.05-1 GHz bandwidth via two distinct effects: the geoMAGNETic effect, and the Askaryan effect. The geoMAGNETic effect occurs when the MAGNETic field of the Earth causes cascade charges to form a transverse current that radiates linearly polarized radiation aligned with the Lorentz force direction. The Askaryan effect is caused by the net negative charge excess in the cascade that radiates linearly polarized radiation along the Cherenkov cone. When UHECR cascades enter solid, RF transparent matter at altitudes where the cascade develops, Askaryan radiation can propagate through the solid matter to RF detectors. The Askaryan Radio Array (ARA) at the South Pole has observed 13 UHECR candidates in precisely this fashion. We present an analytical model that confirms the events are UHECRs. The model includes Askaryan radiation and the ARA RF channel response. The coherently summed waveforms (CSWs) from the UHECR candidates match our model with correlation coefficients between 0.69 and 0.86, and with minimal fractional power differences. Finally, we demonstrate how to use the analytic formalism to obtain the Askaryan $\vec{E}$-field, and that it matches the results from ARA.
[abstract 12 / 42] Yes (score: 5) - Title: Simulations of interaction between outflow and surrounding broken power-law circumnuclear medium: implications for different radio light curves of TDEsAuthors: Xiangli Lei, Qingwen Wu, Chang Zhou, Wei-Hua Lei, Ya-Ping Li, Jiancheng Wu, Weibo Yang,Comments: Submitted to ApJSubjects: astro-ph.HECreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
The complex radio light curves of tidal disruption events (TDEs) challenge our understanding of the properties of both the outflows and the circumnuclear medium (CNM) surrounding supermassive BLACK HOLEs. In this work, we explore outflow-CNM interactions across a broad parameter space using three-dimensional hydrodynamic simulations, adopting a broken power-law CNM density profile with a transition near the Bondi radius. The outflow-CNM interaction inside Bondi radius produces an early radio flare (\(\lesssim 2\) yr) once the emitting region becomes optically thin. A second radio rebrightening can appear a few years later if the outflow decelerates beyond Bondi radius. We also find that either a very dense inner CNM, which causes rapid deceleration, or a rarefied outer CNM suppresses the late rebrightening that will produces a single early-peaked flare. In contrast, a rarefied CNM inside the Bondi radius suppresses the early flare and yields a single late-peaked event. For the case of very dense CNM at large radii, the interaction will trigger a sharp late-time rise as observed in some TDEs. We further explore the interaction of a RELATIVISTIC JET with a broken power-law CNM, which can reproduce the characteristic light curves as observed in JETted TDEs without invoking complex JET structure.
[abstract 13 / 42] Yes (score: 4) - Title: Testing non-circular BLACK HOLE spacetime with X-ray reflectionAuthors: Leda Gao, Swarnim Shashank, Cosimo Bambi,Comments: 13 pages, 6 figures. v2: refereed versionSubjects: gr-qcCreated: 2026-06-03; Updated: 2026-06-05; Datestamp: 2026-06-05
X-ray reflection spectroscopy is a powerful tool for testing the Kerr hypothesis and probing the strong gravity regime around accreting BLACK HOLEs. Most tests of General Relativity (GR) assume that the spacetime around a BLACK HOLE is circular, meaning the metric possesses a specific symmetry structure common to the Kerr solution. However, deviations from circularity are predicted by various modified gravity theories and non-vacuum General Relativity solutions. In this work, we test a specific non-circular metric constructed based on a locality principle, where the deviation from the Kerr spacetime is driven by the local spacetime curvature. To accurately model the reflection spectrum in this background, we implement a RELATIVISTIC ray-tracing code in horizon-penetrating (ingoing Kerr) coordinates, which are favored for their ability to avoid introducing curvature singularities at the horizon in non-circular spacetimes. We apply this model to the high-quality \textit{NUSTAR} spectrum of the Galactic BLACK HOLE binary EXO 1846--031. Our spectral analysis reveals a source with a high inclination angle ($ι\approx 76^{\circ}$) and a near-extremal spin parameter ($a_* \approx 0.98$). While we identify a global minimum in the parameter space suggesting a non-zero deformation ($\ell_{\mathrm{NP}} \approx 0.12$), the 99\% confidence interval fully encompasses the Kerr limit ($\ell_{\mathrm{NP}}=0$). We conclude that the current X-ray reflection data for EXO 1846--031 are consistent with the Kerr hypothesis. This work demonstrates the feasibility of using X-ray reflection spectroscopy to constrain non-circular metrics and establishes a framework for future tests.
[abstract 14 / 42] Yes (score: 4) - Title: On the Nature of Candle-Flame-Shaped Solar Flares and Sub-Alfvénic Supra-Arcade Plasma DownflowsAuthors: Ivan Oparin, Sabastian Fernandes, Bin Chen, Chengcai Shen, Xiaocan Li, Fan Guo, Sijie Yu,Comments: Accepted to ApJSubjects: astro-ph.SRCreated: 2026-06-03; Updated: 2026-06-05; Datestamp: 2026-06-05
Certain solar flares exhibit a distinctive candle-flame or cusp-shaped feature above the bright flare arcade visible in extreme ultraviolet (EUV) and X-ray channels sensitive to high-temperature plasma. The presence of a cusp-like structure is generally regarded as a key piece of morphological evidence for MAGNETic RECONNECTion to power explosive energy release in solar flares. In addition, downward-propagating plasma flows above the flare arcade have often been interpreted as outflows driven by MAGNETic RECONNECTion. However, the relationship between the observed candle-flame-shaped morphology and the underlying MAGNETic field geometry for RECONNECTion remains unclear. Likewise, the observed speed of the plasma downflows has been found to be too low compared to the upstream Alfvén speed predicted by RECONNECTion theories. With the help of a recently developed three-dimensional MAGNETohydrodynamics (MHD) model, we examine the locations where MAGNETic topology changes from antiparallel to closed (Y-points) in a candle-flame-shaped flare, compare the observational emission features with synthetic EUV images generated from the model, and analyze their time evolutions. We also investigate the role of projection effects and line-of-sight integration in the measurements of plasma downflow speeds. Our analysis reveals that the Y-points do not necessarily coincide with the apparent cusp tip. Also, the apparent speeds of the supra-arcade downflows, as derived from tracks in the time-distance plots, underestimate the true Alfvén speeds in the RECONNECTion inflow region by at least a factor of 2 up to an order of magnitude.
[abstract 15 / 42] Yes (score: 4) - Title: Nonthermal Particle Acceleration by Magnetic Pumping in Pulsating PlasmasAuthors: Giuseppe Arrò, Vladimir Zhdankin, Fabio Bacchini,Comments:Subjects: astro-ph.HE physics.plasm-phCreated: 2026-06-03; Updated: 2026-06-05; Datestamp: 2026-06-05
We present a new "pulsating box" setup to investigate particle acceleration in high-beta plasmas undergoing compression-expansion cycles. Our fully kinetic simulations show that particles are efficiently accelerated by MAGNETic pumping, producing nonthermal energy distributions with power-law tails. Numerical results are in excellent agreement with a generalized maximum entropy model that we derive, linking the power-law index of distributions to the injected energy. Our results are relevant for understanding the origin of high-energy particles in space and astrophysical plasmas.
[abstract 16 / 42] Yes (score: 4) - Title: A Decade to Map the Diffuse Universe: FRB-QSO Pairs with HST/COS SpectroscopyAuthors: Jessica Werk, Matthew McQuinn, J. Xavier Prochaska, Sunil Simha, Rongmon Bordoloi, Liam Connor, Andrew Fox, J. Chris Howk, Cameron Hummels, Lordrick Kahinga, Victoria Kaspi, Khee-Gan Lee, Nicolas Lehner, Kiyoshi Masui, Benjamin Oppenheimer, Vikram Ravi, Kate Rubin, Kirill Tchernyshyov, Yong Zheng,Comments: 5 pages, 1 figure; White Paper submitted to STScI and NASA GSFC in response to "Building a Roadmap for Hubble Science into the 2030s"Subjects: astro-ph.GACreated: 2026-06-03; Updated: 2026-06-05; Datestamp: 2026-06-05
Jointly analyzing the sightlines of arcsecond-localized fast radio bursts (FRBs) and UV-bright QUASARs (QSOs) nearby in projection has the potential to provide strong constraints on the phases, mass distributions, and MAGNETic structure of the diffuse universe. Each probe supplies what the other cannot: FRBs provide integrated electron columns (DM), line-of-sight MAGNETic field estimates (RM), and scattering constraints ($τ_{\rm scatt}$) that are independent of gas phase; QSOs provide the redshift- and phase-resolved column densities needed to interpret them. Today, there are only $\sim100$ arcsecond-localized FRBs at $z < 1$, making statistical FRB-QSO pair surveys impossible. By 2035, there will be $\sim10^{5}$. Using the most recent FRB localization forecasts and UV-bright QSO catalogs, we estimate that next-generation interferometers will yield thousands of FRB--QSO pairs at angular separations $θ< 10'$, including $\sim100$ pairs at $θ< 1'$, over a common 20,000\,deg$^2$ footprint by 2035. We outline the science enabled by this sample: constraints on CGM ionization fractions and baryon masses; observational constraints on the role of MAGNETic fields and turbulence in the CGM and cosmic web; sightline-by-sightline partitioning of the cosmic DM budget; and three-dimensional mapping of the multiphase Milky Way and M31 halos. Together, these measurements directly address the physics of feedback, non-thermal pressure support, and energy balance in the diffuse gas that regulates galaxy growth. HST/COS is the only instrument that can carry out this program, and the 2030s are the only decade in which to do it before Habitable Worlds Observatory (HWO) defines the next era of diffuse universe science.
[abstract 17 / 42] (score: 3) - Title: The Discovery of an Active Wind from the Milky Way's Black HoleAuthors: Mark D. Gorski, Elena Murchikova,Comments: 21 pages, 3 main figures, 4 supplemental figuresSubjects: astro-ph.GACreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
Every large galaxy has a BLACK HOLE in its center. The interaction between the BLACK HOLE and its host profoundly shapes galactic evolution and the Universe as a whole. The key features of this interaction are BLACK HOLE JETs -- or more generally, winds -- which every BLACK HOLE must have. Despite the proximity and importance of our Galaxy's central BLACK HOLE, Sagittarius A* (Sgr A*), the active wind from it has eluded scientists for over half a century. Here we report the discovery of a large active wind from Sgr A* using unprecedentedly deep (T$_b \sim30$ mK) and high angular resolution (<0.25") observations with the Atacama Large Millimeter/Submillimeter Array (ALMA). We detect a large conical clearing in the cold molecular gas surrounding Sgr A* that is at least 1~parsec long and has a ~45 degree opening angle. The morphology and energetics of this structure are consistent with active clearing of gas by a hot wind from Sgr A*.
[abstract 18 / 42] (score: 3) - Title: A Unified Dark-Matter--Driven Relativistic Bondi Route to Black-Hole Growth from Stellar to Supermassive ScalesAuthors: Chian-Shu Chen, Feng-Li Lin,Comments: 8 pages, 5 figures, match with the ApJL published version, but with an additional appendix to clarify the usual no-go for the usual Bondi accretion mechanism for SMBHs; v4 correcting a minor typo on Eq. (6) and (S23)Subjects: hep-ph astro-ph.CO astro-ph.GACreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
Observations of luminous QUASARs at $z\gtrsim7$ reveal supermassive BLACK HOLEs (SMBHs) with inferred masses $M_{\rm BH}\sim10^9 \, M_\odot$ formed within the first $\sim700$~Myr of cosmic history. Standard growth channels \textrm{ -- } Eddington-limited gas accretion and hierarchical mergers \textrm{ -- } face severe timescale restrictions. We consider a super-Eddington accretion mechanism aided by the Bondi accretion of a minimal model of self-interacting DARK MATTER (SIDM). We demonstrate that in a {\it critical regime} with a near-RELATIVISTIC sound speed, the Bondi accretion yields an accretion rate that depends only on the mass $m$ of SIDM, thus it is universal to the ambient environment. This critical accretion mechanism for $m\gtrsim 10^{-2}\; {\rm eV}$ can grow seeds as small as $10\,M_\odot$ primordial BLACK HOLEs (PBH) in the early Universe into $10^9$ \textrm{--} $10^{10}\,M_\odot$ SMBHs by $z\sim7$ without fine-tuned environments. Therefore, given a mass distribution of PBHs and a value of $m$, the mass function of primary BLACK HOLEs at late time can be fully determined with masses ranging from stellar to SMBHs. This connects the microscopic physics of DARK MATTER to astrophysical observations of BLACK HOLEs.
[abstract 19 / 42] (score: 3) - Title: Varstrometry for Off-nucleus and Dual Subkiloparsec AGN (VODKA): Three Quadruply Lensed Quasars at Cosmic Noon in HST and JWSTAuthors: Mingrui Liu, Yu-Ching Chen, Nadia L. Zakamska, Xin Liu, Yue Shen, Xuheng Ding, Arran Gross, Hsiang-Chih Hwang, Yuzo Ishikawa, Kedar A. Phadke,Comments: 15 main pages, 11 figures, accepted for publication in ApJSubjects: astro-ph.GACreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
We present results from imaging observations of three quadruply lensed QUASARs by Hubble Space Telescope (HST) and James Webb Space Telescope (JWST) at redshifts $z = 2.550$, 2.975, and 1.500. We model our targets assuming a singular isothermal ellipsoid mass profile and an elliptical SÃ\c{opyright}rsic profile for the lensing galaxies, and reconstruct the geometric configuration of each system with measured Einstein radii of 0.44$'$, 0.58$'$, and 0.49$'$. While no spectroscopic measurements are available for the lenses, we constrain the redshift of each lens to $0.5 < z < 1.2$, $1.0 < z < 1.5$, and $0.4 < z < 0.9$. For all three lenses, the best-fit light model yield a typical de Vaucouleurs $n_{\rm S\acute{e}rsic} \sim 4$ profile and an effective radius $R_e$ around $\sim 1.5 - 3.5$ kpc. We accordingly classify the three lenses as early-type galaxies at an intermediate to high redshift, a common type for strong lensing galaxies. Compared to other known quadruple lenses, the lensing galaxies in this work are at the lower end of the distribution of Einstein radii and upper end of the distribution of the lens redshifts. They represent an interesting quadrant of subarcsecond-separation lenses in the population of single-galaxy strong lensing which have been largely unexplored yet and will be great targets of interest in upcoming high-resolution lensing surveys.
[abstract 20 / 42] (score: 3) - Title: Probing the Dispersion and Rotation Measure Contributions from Supernova Remnants in Fast Radio Burst Source Environments with 1D SNR SimulationAuthors: Zhao Joseph Zhang, Gaku Kawashima, Shiu-Hang Lee, Kentaro Nagamine, Bing Zhang, Yusei Fujimaru,Comments: ApJ, in pressSubjects: astro-ph.HECreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
Fast radio bursts (FRBs) provide a sensitive probe of ionized baryons through their dispersion measure (DM). In addition to slowly evolving cosmological terms, at least two repeaters now show clear secular DM-decrease episodes: FRB~20190520B and FRB~20121102 , supporting a dense, dynamically evolving local environment. We adopt a \emph{forward-modeling} approach and use time-dependent 1D SNR simulations for a young MAGNETar embedded in SN ejecta, combining single-star and binary-stripped progenitors with HD+NEI calculations to follow shock structure, ionization, and electron density. The shocked region contributes only limited DM ($\lesssim10\,{\rm pc\,cm^{-3}}$), while the dominant time-varying component is the unshocked ejecta, whose early behavior follows ${\rm DM}\propto t^{-α}$ with $α\simeq1.8$--$1.9$. Although shocked-region DM is small, shock-amplified MAGNETic fields can still generate substantial RM; in our shock-only RM framework, only the $11\,M_\odot$ SS model reproduces the FRB~20121102 RM evolution. Binary-stripped progenitors generally yield smaller DM than single-star models at fixed $M_{\rm ZAMS}$, with composition-dependent mean molecular weights introducing non-monotonic mass trends. Matching the observed ${\rm dDM}/{\rm d}t$ of FRB~20190520B (and the late-stage slope of FRB~20121102), we infer local SNR DM contributions of tens to hundreds ${\rm pc\,cm^{-3}}$. We also find GHz escape is allowed in most models, with $τ_{\rm ff}=1$ typically reached by $t_{\rm esc}\lesssim70$ yr; for weakly ionized ejecta, the source can be nearly transparent from very early times. These results support a young CCSN/SNR origin for a substantial fraction of ${\rm DM}_{\rm source}$ and highlight that physically consistent local-environment modeling is essential for robust FRB cosmological DM inferences.
[abstract 21 / 42] (score: 3) - Title: Long-term investigation of gamma Cas analogsAuthors: Yael Naze, Gregor Rauw, Robbie Webbe, Myron A. Smith, Christian Motch,Comments: accepted for publication by A&ASubjects: astro-ph.SR astro-ph.HECreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
The subcategory of gamma Cas analogs gathers Be stars with bright and hard X-ray emission. Long-term variations are expected in such objects for two reasons: their Be disk builds and dissipates, and such stars are suspected long-period binaries. Seven targets are analysed in this paper: five of them benefit from a spectroscopic monitoring in the visible (ESO, TIGRE, and amateur data) and three of them have been repeatedly observed at X-ray wavelengths (using XMM-Newton, Chandra, and SWIFT). Broad-band photometric data are also examined. We confirm the binary status of five targets (HD44458, HD110432, HD119682, HD161103, and HD162718) and propose first orbital solutions for all of them (they remain preliminary for two cases). Their long periods (59-322 d) and small velocity amplitudes (K~5km/s) imply low-mass (~1 M_sol) companions, as in other Be binaries and in agreement with expectations from binary interaction models. In parallel, variations of the X-ray flux are detected in all three targets with a large dataset of X-ray observations. For NGC 6649 9 and HD162718, these changes are modest (a factor of three) and uncorrelated to simultaneous optical broad-band photometry (which remains rather stable). In contrast, SS397 varies by nearly one dex and the largest and best monitored X-ray changes correlate well with optical variations. At minimum flux, SS397 keeps a hard X-ray spectrum despite a nearly normal L_X/L_BOL ratio, which has not been seen yet among gamma Cas analogs. Finally, the photometric behaviours on short timescales of HD161103, SS397, and NGC 6649 9 appear linked to broad frequency groups, as typically found for Be stars. The frequency spectrum of HD162718 displays a complex mix of (isolated) periodicities with the main one at 6.658/d. This target is thus one of the rare gamma Cas analogs to display a strong high-frequency signal typical of beta Cep activity. [summarized]
[abstract 22 / 42] (score: 3) - Title: Strong environmental AGN enhancement among DSFGs in z > 2 protoclustersAuthors: Monica Natalia Isla Llave, Fabio Vito, Alberto Traina, Cristian Vignali, Olga Cucciati, Benjamin Forrest, Gayathri Gururajan, Brian Lemaux, Sylvia Adscheid, Sebastiano Cantalupo, Kazuki Daikuhara, Marta Galbiati, Roberto Gilli, Tadayuki Kodama, Stefano Marchesi, Maurillio Pannella, Antonio Pensabene, Maria del Carmen Polletta, Rhythm Shimakawa, Paolo Tozzi,Comments: This manuscript has been submitted to A&A; the arXiv version reflects revisions made in response to referee commentsSubjects: astro-ph.GACreated: 2026-06-03; Updated: 2026-06-05; Datestamp: 2026-06-05
Galaxy protoclusters (PCs) at z > 2 are dense regions in which cold gas availability and elevated galaxy interaction rates trigger intense, often dust-obscured, STAR FORMATION. These mechanisms are also expected to promote super-massive BLACK HOLE (SMBH) growth, but this effect remains unclear, largely due to heterogeneous galaxy selections and ACTIVE GALACTIC NUCLEi (AGN) identification methods in previous studies. We quantitatively assess the impact of PC environment on SMBH growth by measuring the incidence of X-ray AGN among dusty star-forming galaxies (DSFGs) in PCs and in a homogeneously selected control field sample, and investigate the physical mechanisms driving any difference. We consider ALMA-detected DSFGs in sub-mm/mm continuum of seven PCs at 2 < z < 4.5, and construct a selection-matched control sample from the COSMOS survey. We statistically compare X-ray AGN incidence and host galaxy physical properties obtained through uniform spectral energy distribution fitting. We find a significant enhancement of X-ray AGN fraction in PCs by ~2.7x (Poisson significance p = 3e-4). Similar values are found in two redshift bins: ~2.7x at z = 2-3 (p = 0.003) and ~2.6x at z = 3-4.5 (p = 0.03). PC and field DSFG samples are well matched in stellar mass, star-formation rate, and dust mass, ruling out selection effects or systematically higher host masses as the driver. Our results provide quantitative evidence that the dense PC environment enhances AGN incidence and SMBH growth in DSFGs beyond what host galaxy properties alone predict, likely through increased gas availability and interaction-driven fueling. This work is a first step toward a homogeneous assessment of environmental effects on SMBH growth across cosmic time.
[abstract 23 / 42] (score: 3) - Title: AGN Line-Intensity Mapping: A Probe of Faint Black Holes at Cosmic NoonAuthors: Eli Visbal, Greg L. Bryan,Comments: 12 pages, 4 figures, submitted to JCAPSubjects: astro-ph.CO astro-ph.GACreated: 2026-06-03; Updated: 2026-06-05; Datestamp: 2026-06-05
We propose line-intensity mapping (LIM) as a new probe of ACTIVE GALACTIC NUCLEi (AGN). By cross-correlating [Ne V] intensity maps with galaxy redshift surveys, we show that the cumulative AGN line emission can be detected even when individual sources are below the detection threshold. The 97.1 eV ionization potential of [Ne V] makes it an essentially uncontaminated tracer of AGN activity, arising from the narrow line region which is accessible even in heavily obscured AGN. We forecast signal-to-noise ratios using a Fisher matrix formalism for two hypothetical future instruments: a CDIM-like instrument targeting [Ne V] $λ3426$ and a PRIMA-like instrument optimized for LIM targeting [Ne V] $14.3 μ$m. For the CDIM-like case we find strong constraints on the product of the mean AGN intensity and bias, $S_{\rm NeV} b_{\rm NeV}$, across $z=2-3$, with redshift-space distortions enabling individual constraints on $S_{\rm NeV}$ and $b_{\rm NeV}$. The LIM signal retains sensitivity to AGN below the $5σ$ direct detection threshold, which at $z=3$ corresponds to $L_{\rm bol} \sim 5\times10^{43}$ erg s$^{-1}$ and coincides with the faint end of existing luminosity function measurements. Roughly 10% of the total signal originates from below this threshold, with the sub-threshold population detectable at $S/N=9-4$ across $z=2-3$ (for $S_{\rm NeV} b_{\rm NeV}$). The PRIMA-like instrument achieves slightly lower signal-to-noise but provides a complementary probe of the AGN population due to the insensitivity of the $14.3 μ$m line to dust attenuation. AGN LIM can potentially be applied to several scientific problems including tracing the total AGN emissivity history, constraining the BLACK HOLE-halo connection at faint luminosities, and discriminating between supermassive BLACK HOLE seeding mechanisms.
[abstract 24 / 42] (score: 3) - Title: Bulk vs. turbulent motions at the centres of galaxy clusters: AGN-driven turbulence according to TNG-ClusterAuthors: Bipradeep Saha, Annalisa Pillepich, Joey Braspenning, Marine Prunier, Dimitris Chatzigiannakis, Dylan Nelson,Comments: 24 Pages, 17 figures. Comments welcomed. Submitted to MNRASSubjects: astro-ph.GACreated: 2026-06-03; Updated: 2026-06-05; Datestamp: 2026-06-05
The highly dynamic intracluster medium (ICM) influences cluster thermodynamic evolution and probes key physical processes. Quantifying the non-thermal motions is therefore essential for understanding cluster physics and interpreting high spectral-resolution X-ray observations from telescopes like {\it XRISM}. We quantify bulk and turbulent gas motions in 352 galaxy clusters at $z=0$ (${\rm M_{200c}=10^{14.3-15.4}\, M_\odot}$) from the TNG-Cluster suite of MAGNETo-hydrodynamical galaxy simulations. We use a multi-scale filtering Reynolds decomposition to separate total gas velocities into bulk (coherent) and turbulent (small-scale fluctuations) components. We primarily focus on the hot X-ray emitting gas in the central core regions. According to TNG-Cluster, majority of the ICM has subsonic turbulence but with broad velocity distributions reaching $\mathcal{M}_{\rm Turb}\sim 10$ and large cluster-to-cluster variations. In cluster centres, turbulence contributes less than half of the total velocity dispersion $(σ_{v\rm,Turb } \sim 0.5 ~σ_{v,\rm Total})$ for most clusters, with typical turbulent velocity dispersions of $50-75$ km s$^{-1}$ across the mass range, and with sub per cent levels of turbulent pressure support. Clusters that are strong cool cores, or have X-ray cavities, or experienced recent SMBH feedback energy injections exhibit systematically larger turbulent velocity dispersions and more prominent turbulent velocity tails. On average, the turbulent velocity dispersion peaks in cluster centres, decreases slightly to a minimum at $0.1-0.2 \, R_{\rm500c}$, then rises again. Our analysis shows that SMBH feedback is a key driver of turbulence in cluster cores, generating strong but short-lived motion alongside high-velocity outflows. It also calls for caution for interpreting {\it XRISM} observations.
[abstract 25 / 42] (score: 3) - Title: Implementation and Verification of Toroidal Resistive Wall Boundary Conditions in the PIXIE3D MHD code using a Boundary Integral MethodAuthors: Samuel Jones, Luis Chacón, Jason Hamilton, Dan Barnes, Andrés Yagüe-López,Comments: 26 pages, 7 figuresSubjects: physics.plasm-phCreated: 2026-06-03; Updated: 2026-06-05; Datestamp: 2026-06-05
We present the complete formulation of resistive wall boundary conditions in axisymmetric toroidal geometries as implemented in the PIXIE3D extended MAGNETohydrodynamics (MHD) code, along with a complete suite of analytical verification examples that demonstrate correctness in the implementation. The formulation centers around a thin wall approximation and a Boundary Integral Method to solve for the MAGNETic scalar potential in the immediately surrounding vacuum. This requires specialized quadrature rules derived from existing literature to handle the numerical integration of singular and hypersingular integrands (the Green's function of Laplace's equation and its derivatives), for which we provide the nodes and weights. Further, we describe an extension to the formalism to include the effect of a perfectly conducting second, outer wall exterior to the resistive (plasma-facing) wall and separated by vacuum, and exterior to the computational plasma mesh proper. Lastly, we describe an extension to include the effect of current-carrying coils also defined exterior to the plasma mesh in the resistive wall boundary condition treatment. For most aspects of the method, we present self-contained verification examples using analytic solutions in axisymmetric toroidal geometries (with both 2D and 3D plasmas) and show it to be accurate to second order. We demonstrate the algorithm with a vertical displacement event (VDE) using the ITER tokamak geometry.
[abstract 26 / 42] (score: 3) - Title: The X-ray emission of the long-period transient and accreting cataclysmic variable ASKAP J174508.9-505149Authors: M. Imbrogno, M. Veresvarska, Y. L. Wang, N. Rea, F. Coti Zelati, K. Rose, J. Pritchard, D. de Martino, S. Scaringi, Z. Wang, D. L. Kaplan,Comments: Accepted for publication in A&A Letters on 27/05/2026. 7 pages (4 main text+ 3 appendices)Subjects: astro-ph.HECreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
Long-period transients (LPTs) challenge our knowledge of the mechanism producing radio periodic pulsations in compact objects. Some LPTs have been associated with systems hosting a white dwarf and a low-mass star in a detached binary. Recently, a new LPT (ASKAP\,J174508.9-505149) has been classified as an accreting cataclysmic variable (CV). In the present letter, we report on the detailed study of the X-ray variability of ASKAP\,J174508.9-505149 as observed by \emph{XMM-Newton} and \emph{Einstein Probe} between September 2025 and May 2026. Simultaneous optical and radio observations are also presented. We studied the timing variability of the source, and estimated an X-ray periodicity of $P=4868(22)$\,s, consistent with radio and optical periods. We also observe the same periodicity in the hardness ratio extracted from the \emph{XMM-Newton} observation, peaking at the minimum of the modulation. A long-term modulation is also present in the X-rays and in the B-band photometry, but it is poorly constrained by the current dataset. Spectral X-ray analysis shows the presence of a black-body component ($\sim$0.1\,keV), a collisionally ionised plasma ($\sim$15\,keV), and an absorption feature at 0.77 keV (possibly due to Oxygen-VII). This is the third LPT detected in the X-ray band, the second with a detected X-ray periodicity and variable X-ray emission, and the first conclusively recognised as an accreting MAGNETic CV.
[abstract 27 / 42] (score: 3) - Title: Research Note: Ghostly DLAs in SDSS DR16Authors: Patrick Petitjean,Comments:Subjects: astro-ph.GACreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
In Petitjean (2026, arXiv:2605.12188)), we revisited the origin of proximate damped Lyman-alpha absorbers (PDLAs), which trace cold gas within 3000 km/s of the QUASAR redshift, and interpreted their kinematics and physical properties within a unified framework. We showed that most PDLAs are associated with the environment of the AGN and/or the QUASAR host galaxy. We also provided the first census and characterization of absorption systems exhibiting strong absorption from excited levels of atomic ground states among QUASAR-associated absorbers. Among these, ghostly and coronagraphic systems arise in dense, compact gas that partially covers the QUASAR emission regions. Most systems are associated with outflows reaching velocities up to -2000 km/s, while a smaller fraction of inflowing clouds extends to velocities of up to +1200 km/s. In the present work, we provide an updated classification of PDLAs, including a revised catalogue of ghostly systems that more than doubles the number of previously known detections. We investigate the properties of these systems by measuring and discussing the equivalent widths of the detected absorption lines in both stacked spectra and individual ghostly systems. In particular, we show that although most ghostly systems are bona fide DLAs, this is not always the case.
[abstract 28 / 42] (score: 2) - Title: The Synthetic Absorption Line Spectral Almanac (SALSA)Authors: Dylan Nelson, Celine Peroux, Philipp Richter, Matthew M. Pieri, Sebastian Lopez, Rongmon Bordoloi, Siwei Zou, Joseph N. Burchett, Rebecca L. Davies, Rahul Ramesh, Matthew C. Smith, Sanchayeeta Borthakur, Christopher W. Churchill,Comments: https://www.tng-project.org/spectra (comments and suggestions welcome)Subjects: astro-ph.GA astro-ph.COCreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
We create the first large-scale mock spectroscopic survey of gas absorption sightlines traversing the interstellar medium (ISM), circumgalactic medium (CGM), and intergalactic medium (IGM) surrounding galaxies of virtual Universes. That is, we create mock, or synthetic, absorption spectra by drawing lines-of-sight through cosmological hydrodynamical simulations, using a new mesh-free Voronoi ray-tracing algorithm. The result is the Synthetic Absorption Line Spectral Almanac (SALSA), which is publicly released on a feature-rich online science platform (www.tng-project.org/spectra). It spans a range of ions, transitions, instruments, observational characteristics, assumptions, redshifts, and simulations. These include, but are not limited to: (ions) HI, OI, CI, MgI, MgII, FeII, SiII, CaII, ZnII, SiIII, SiIV, NV, CII, CIV, OVI; (instruments) SDSS-BOSS, KECK-HIRES, UVES, COS, DESI, 4MOST, WEAVE, XSHOOTER; (model choices) with/without dust depletion, noise, QUASAR continua, foregrounds; (redshift) from z=0 to z~6; (ancillary data) integrated equivalent widths, column densities, distances and properties of nearby galaxies; (simulations) IllustrisTNG including TNG50, TNG-Cluster, EAGLE, and SIMBA. This scope is not fixed, and will grow and evolve with community interest and requests over time -- suggestions are welcome. The resulting dataset is generic and broadly applicable, enabling diverse science goals such as: (i) studies of the underlying physical gas structures giving rise to particular absorption signatures, (ii) galaxy-absorber and halo-absorber correlations, (iii) virtual surveys and survey strategy optimization, (iv) stacking experiments and the identification of faint absorption features, (v) assessment of data reduction methods and completeness calculations, (vi) inference of physical properties from observables, and (vii) apples-to-apples comparisons between simulations and data.
[abstract 29 / 42] (score: 2) - Title: A Self-Consistent Model of Kinetic Alfven Solitons in Pulsar Wind Plasma: Linking Soliton Characteristics to Pulsar ObservablesAuthors: Manpreet Singh, Geetika Slathia, N. S. Saini, Siming Liu,Comments: 13 Pages, 7 figuresSubjects: physics.plasm-phCreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
A self-consistent model is presented for the formation and propagation of kinetic Alfvén (KA) solitons in mass-loaded filaments within the pulsar wind, where a MAGNETized electron--positron--ion plasma flows along open MAGNETic field lines beyond the light cylinder. Using a reductive perturbation approach, we derive a Korteweg--de Vries (KdV) equation governing the nonlinear evolution of KA solitons in this environment. The soliton amplitude and width depend sensitively on key pulsar observables, including spin period, spin-down rate, and pair multiplicity, as well as on plasma composition and suprathermal particle distributions. Heavy ion species such as Fe$^{26+}$ produce significantly broader solitons through enhanced inertia and dispersion, while increasing pair multiplicity leads to smaller solitons through stronger screening. More oblique propagation (larger $θ$) yields wider but lower-amplitude solitons, whereas more thermalized pair plasmas (higher $κ$) support taller and broader structures. A population-level analysis of 1174 pulsars quantifies the physical scales of these nonlinear structures, showing that millisecond pulsars host the most compact solitons, whereas slower pulsars support broader structures. Within the adopted admissible finite-$β$ regime, this work links soliton properties to measurable pulsar parameters and provides a self-consistent framework for characterizing localized nonlinear plasma structures in finite-MAGNETization regions of pulsar winds and for assessing their role in modulating the local plasma environment.
[abstract 30 / 42] (score: 2) - Title: Bounds on Lorentz invariance violation from muon fluctuations at the Pierre Auger ObservatoryAuthors: The Pierre Auger Collaboration, A. Abdul Halim, P. Abreu, M. Aglietta, I. Allekotte, K. Almeida Cheminant, R. Aloisio, J. Alvarez-Muñiz, A. Ambrosone, J. Ammerman Yebra, L. Anchordoqui, B. Andrada, L. Andrade Dourado, L. Apollonio, C. Aramo, E. Arnone, J. C. Arteaga Velázquez, P. Assis, G. Avila, E. Avocone, A. Bakalova, Y. Balibrea, A. Baluta, F. Barbato, A. Bartz Mocellin, J. P. Behler, C. Berat, M. E. Bertaina, M. Bianciotto, P. L. Biermann, V. Binet, K. Bismark, T. Bister, J. Biteau, J. Blazek, J. Blümer, M. Boháčová, D. Boncioli, C. Bonifazi, N. Borodai, J. Brack, P. G. Brichetto Orquera, A. Bueno, S. Buitink, M. Büsken, A. Bwembya, K. S. Caballero-Mora, S. Cabana-Freire, L. Caccianiga, J. Caraça-Valente, R. Caruso, A. Castellina, F. Catalani, G. Cataldi, L. Cazon, M. Cerda, B. Čermáková, A. Cermenati, K. Cerny, J. A. Chinellato, J. Chudoba, L. Chytka, R. W. Clay, A. C. Cobos Cerutti, R. Colalillo, R. Conceição, G. Consolati, M. Conte, F. Convenga, D. Correia dos Santos, P. J. Costa, C. E. Covault, M. Cristinziani, C. S. Cruz Sanchez, S. Dasso, K. Daumiller, B. R. Dawson, R. M. de Almeida, E. -T. de Boone, B. de Errico, J. de Jesús, S. J. de Jong, J. R. T. de Mello Neto, I. De Mitri, D. de Oliveira Franco, F. de Palma, V. de Souza, E. De Vito, A. Del Popolo, O. Deligny, N. Denner, K. Denner Syrokvas, L. Deval, A. di Matteo, C. Dobrigkeit, J. C. D'Olivo, L. M. Domingues Mendes, Y. Dominguez Ballesteros, Q. Dorosti, R. C. dos Anjos, J. Ebr, F. Ellwanger, R. Engel, I. Epicoco, M. Erdmann, A. Etchegoyen, C. Evoli, H. Falcke, G. Farrar, A. C. Fauth, T. Fehler, F. Feldbusch, A. Fernandes, M. Fernández Alonso, B. Fick, J. M. Figueira, P. Filip, A. Filipčič, T. Fitoussi, B. Flaggs, A. Franco, M. Freitas, T. Fujii, A. Fuster, C. Galea, B. García, C. Gaudu, P. L. Ghia, U. Giaccari, M. Giammarco, C. Glaser, F. Gobbi, F. Gollan, G. Golup, P. F. Gómez Vitale, J. P. Gongora, J. M. González, N. González, D. Góra, A. Gorgi, M. Gottowik, F. Guarino, G. P. Guedes, Y. C. Guerra, L. Gülzow, S. Hahn, P. Hamal, M. R. Hampel, P. Hansen, V. M. Harvey, A. Haungs, M. Havelka, T. Hebbeker, C. Hojvat, J. R. Hörandel, P. Horvath, M. Hrabovský, T. Huege, A. Insolia, P. G. Isar, M. Ismaiel, P. Janecek, V. Jilek, K. -H. Kampert, B. Keilhauer, A. Khakurdikar, V. V. Kizakke Covilakam, H. O. Klages, M. Kleifges, J. Köhler, F. Krieger, M. Kubatova, N. Kunka, B. L. Lago, N. Langner, N. Leal, M. A. Leigui de Oliveira, Y. Lema-Capeans, A. Letessier-Selvon, I. Lhenry-Yvon, L. Lopes, J. P. Lundquist, M. Mallamaci, S. Mancuso, D. Mandat, P. Mantsch, A. G. Mariazzi, C. Marinelli, I. C. Mariş, G. Marsella, D. Martello, S. Martinelli, O. Martínez Bravo, M. A. Martins, H. -J. Mathes, J. Matthews, G. Matthiae, E. Mayotte, S. Mayotte, P. O. Mazur, G. Medina-Tanco, J. Meinert, D. Melo, A. Menshikov, C. Merx, S. Michal, M. I. Micheletti, L. Miramonti, M. Mogarkar, S. Mollerach, F. Montanet, L. Morejon, K. Mulrey, R. Mussa, W. M. Namasaka, S. Negi, L. Nellen, K. Nguyen, G. Nicora, M. Niechciol, D. Nitz, D. Nosek, A. Novikov, V. Novotny, L. Nožka, A. Nucita, L. A. Núñez, S. E. Nuza, J. Ochoa, M. Olegario, C. Oliveira, L. Östman, M. Palatka, J. Pallotta, S. Panja, G. Parente, T. Paulsen, J. Pawlowsky, M. Pech, J. Pękala, R. Pelayo, V. Pelgrims, C. Pérez Bertolli, L. Perrone, S. Petrera, C. Petrucci, T. Pierog, M. Pimenta, M. Platino, B. Pont, M. Pourmohammad Shahvar, P. Privitera, C. Priyadarshi, M. Prouza, K. Pytel, S. Querchfeld, J. Rautenberg, D. Ravignani, J. V. Reginatto Akim, A. Reuzki, J. Ridky, F. Riehn, M. Risse, V. Rizi, E. Rodriguez, G. Rodriguez Fernandez, J. Rodriguez Rojo, S. Rossoni, M. Roth, E. Roulet, A. C. Rovero, A. Saftoiu, M. Saharan, F. Salamida, H. Salazar, G. Salina, P. Sampathkumar, N. San Martin, J. D. Sanabria Gomez, F. Sánchez, F. M. Sánchez Rodriguez, E. Santos, F. Sarazin, R. Sarmento, R. Sato, P. Savina, V. Scherini, H. Schieler, M. Schimp, D. Schmidt, O. Scholten, H. Schoorlemmer, P. Schovánek, F. G. Schröder, J. Schulte, T. Schulz, S. J. Sciutto, M. Scornavacche, A. Sedoski, S. Sehgal, S. U. Shivashankara, G. Sigl, K. Simkova, F. Simon, R. Šmída, S. Soares Sippert, P. Sommers, M. Stadelmaier, S. Stanič, J. Stasielak, P. Stassi, S. Strähnz, M. Straub, T. Suomijärvi, A. D. Supanitsky, Z. Svozilikova, Z. Szadkowski, F. Tairli, M. Tambone, A. Tapia, C. Taricco, C. Timmermans, O. Tkachenko, P. Tobiska, C. J. Todero Peixoto, B. Tomé, A. Travaini, P. Travnicek, C. Trimarelli, M. Tueros, M. Unger, R. Uzeiroska, L. Vaclavek, M. Vacula, I. Vaiman, J. F. Valdés Galicia, L. Valore, P. van Dillen, E. Varela, V. Vašíčková, A. Vásquez-Ramírez, D. Veberič, I. D. Vergara Quispe, S. Verpoest, V. Verzi, J. Vicha, S. Vorobiov, J. B. Vuta, C. Watanabe, A. A. Watson, A. Weindl, M. Weitz, L. Wiencke, H. Wilczyński, B. Wundheiler, B. Yue, A. Yushkov, E. Zas, D. Zavrtanik, M. Zavrtanik,Comments: 15 pages, 9 figures Accepted for publication on PRLSubjects: astro-ph.HE gr-qc hep-phCreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
Quantum gravity theories often modify spacetime symmetries. In particular, Lorentz invariance may be violated when approaching the Planck scale. Although the scales at which interactions occur in extensive air showers induced by ultra-high-energy COSMIC RAYs in the atmosphere are many orders of magnitude below the Planck scale, these violations might still be observable. In this work, the fluctuations in the number of muons in the extensive air showers measured at the Pierre Auger Observatory are exploited, for the first time, to constrain Lorentz invariance violations. The bounds derived in the hadronic sector are the strongest ever obtained, and do not rely on assumptions about the mass composition of ultra-high-energy COSMIC RAYs. The fluctuations in the number of muons constitute a new and powerful observable to further explore Lorentz invariance in a region of the parameter space not accessible to other observables.
[abstract 31 / 42] (score: 2) - Title: Turbulent Nature of the Quasicontinuous Exhaust Regime for Fusion PlasmasAuthors: Kaiyu Zhang, Wladimir Zholobenko, Andreas Stegmeir, Michael Faitsch, Konrad Eder, Christoph Pitzal, Frank Jenko, ASDEX Upgrade Team,Comments:Subjects: physics.plasm-phCreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
We demonstrate a turbulence mechanism that reconciles high plasma confinement with efficient heat exhaust -- a central challenge for fusion energy. Global two-fluid turbulence simulations of the reactor-relevant Quasicontinuous Exhaust regime on the ASDEX Upgrade tokamak reveal that a quasicoherent mode drives mesoscopic oscillations of the pedestal boundary across the MAGNETic separatrix and ejects ballistic filaments (blobs), reproducing both the mean profiles and turbulent fluctuations observed experimentally. This behavior arises from a synergistic interplay between kinetic ballooning modes and resistive X-point modes straddling the separatrix. These first-principles results place extrapolations to future fusion reactors on a firm physical footing.
[abstract 32 / 42] (score: 2) - Title: How nonlinear spectral back transfer limits the temporal coherency of zonal modes?Authors: Rameswar Singh, P H Diamond,Comments:Subjects: physics.plasm-phCreated: 2026-06-03; Updated: 2026-06-05; Datestamp: 2026-06-05
Zonal modes are central to MAGNETic confinement because their radial shears regulate turbulence and transport. While the generation of these flows is well understood, the mechanisms limiting their persistence in collisionless regimes remain unresolved. In this paper, we demonstrate that nonlinear spectral back-transfer of free energy from zonal modes to turbulence sets the fundamental limit on the temporal coherency of the shearing field. Back-transfer events induce stochastic phase and amplitude scattering of zonal shear that limits its auto-coherence time. Using gyrokinetic GENE simulations, we show that back-transfer is highly intermittent and occurs in bursts that co-exist with the zonal flow generation process. The probability distribution of the zonal free energy transfer is non-Gaussian, with positive triangularity (PT) exhibiting substantially higher kurtosis than negative triangularity (NT), reflecting the markedly more intermittent and heavy-tailed character of back-transfer bursts in PT. We find that NT plasmas exhibit significantly reduced back-transfer compared to PT. This suppression increases the shear auto-coherence time τ_{E} and the shearing Kubo number K_{u}, leading to more resilient and effective turbulence regulation despite lower absolute zonal kinetic energy. These results identify back-transfer as a key nonlinear damping mechanism and suggest that it must be explicitly treated in reduced models of drift-wave zonal-flow turbulence.
[abstract 33 / 42] (score: 2) - Title: Hyperaccreting Neutron Stars inside Massive Envelopes: The Implausibility of Thorne-Żytkow ObjectsAuthors: Patrick Chi-Kit Cheong, David Radice, Christopher L. Fryer,Comments: Accepted versionSubjects: astro-ph.HECreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
The evolution of neutron stars (NSs) embedded within massive stellar envelopes is a critical phase in binary stellar evolution, potentially leading to the formation of Thorne-Żytkow Objects (TŻOs) or catastrophic collapse. We present the first fully coupled general RELATIVISTIC hydrodynamics (GRHD) simulations of hypercritical accretion onto NSs that simultaneously incorporate grey two-moment (M1) neutrino transport and an $α$-chain nuclear reaction network. By investigating four distinct progenitor evolutionary stages, we resolve the complex interplay between intense neutrino cooling, multidimensional fluid dynamics, and nuclear feedback. Our results show that while vigorous convection is triggered in the post-shock region, the global energy budget is primarily governed by neutrino cooling, which effectively balances the accretion power. Crucially, even though our M1 transport scheme captures neutrino absorption and localized heating, the efficient cooling sink and high ram pressure of the infalling envelope prevent the formation of any core-collapse SUPERNOVA-like explosion. We find that all nucleosynthetically processed material ($T > 5$~GK) remains strictly gravitationally bound, challenging the assumption that these systems contribute significantly to galactic nucleosynthetic yields via convective dredge-up. The lack of sustained outflows and the persistent hypercritical accretion rates suggest that embedded NSs will rapidly exceed the Tolman-Oppenheimer-Volkoff mass limit on timescales of minutes to hours. We conclude that these systems are not stable TŻOs, but are rather transient precursors to catastrophic BLACK HOLE formation and potential central engines for high-energy transients.
[abstract 34 / 42] (score: 2) - Title: Constraining Lorentz symmetry breaking in bumblebee gravity with extreme mass-ratio inspiralsAuthors: Sheng Long, Zhong-wu Xia, Huajie Gong, Zhoujian Cao, Qiyuan Pan, Jiliang Jing,Comments:Subjects: gr-qcCreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
Extreme mass-ratio inspirals (EMRIs), with their long-lived and highly RELATIVISTIC orbital evolution, can probe strong-field spacetime geometry and provide an important means to test general relativity. In this work, we investigate EMRI waveforms in a Schwarzschild-like BLACK HOLE spacetime arising in bumblebee gravity, where Lorentz symmetry breaking (LSB) is characterized by a dimensionless parameter $\ell$. We construct EMRI waveforms within the Augmented Analytic Kludge (AAK) framework using the modified orbital frequencies and fluxes. We find that $\ell$ significantly affects the orbital evolution and thereby modifies the waveform. These modifications grow with increasing $\ell$ and are further enhanced for more eccentric orbits. Furthermore, using Bayesian analysis, we obtain the posterior distributions of EMRI with the parameter $\ell$ included. Our results show that all injected source parameters are recovered within their $1\,σ$ credible intervals. We find that the bumblebee parameter $\ell$ can be constrained with an uncertainty of order $\mathcal{O}(10^{-4})$ by LISA.
[abstract 35 / 42] (score: 2) - Title: The Influence of Opacity on Inferred MHD Wave Signatures in the Lower Solar AtmosphereAuthors: Samuel J. Skirvin, Samuel D. T. Grant, David B. Jess, Ryan J. Campbell, Shahin Jafarzadeh, Mika V. Kontiainen, Michele Berretti, Timothy J. Duckenfield, Glen Chambers, Marco Stangalini, Luc Rouppe van der Voort,Comments: 18 pages, 12 figures, Accepted for Publication in Frontiers in Astronomy and Space Science for the Special Issue "Magnetohydrodynamic Motions: Daniel K. Inouye Solar Telescope's Window into the Dynamic Sun"Subjects: astro-ph.SRCreated: 2026-06-03; Updated: 2026-06-05; Datestamp: 2026-06-05
Magnetohydrodynamic wave activity in small-scale MAGNETic structures, such as solar pores, provides key insights into energy transport in the lower solar atmosphere. This study presents high-resolution observations of ten solar pores contained within a 43 x 43 Mm$^2$ field of view, obtained with the CRISP instrument at the Swedish 1-m Solar Telescope. We investigate the temporal behaviour of the line-of-sight velocity (vlos) and MAGNETic field (blos) oscillations within the pore structures. Using SIR inversions, we analyse the oscillatory signals at multiple optical depths (log $τ$ levels) to assess how variations in geometric height (z) and temperature relate to the observed blos fluctuations. Our results reveal that higher-frequency oscillations (> 6 mHz) exhibit strong coherences with in-phase fluctuations between blos and z across atmospheric layers, consistent with upward-propagating MAGNETo-acoustic waves. In contrast, coherent lower-frequency oscillations display significant phase differences, which may arise from opacity effects contaminating the inversion response. These findings highlight the importance of accounting for opacity effects when interpreting MAGNETic oscillations, with direct implications for forthcoming high-precision MAGNETic diagnostics from facilities such as DKIST.
[abstract 36 / 42] (score: 2) - Title: Entropy-mode imprints in the solar corona: non-exponential damping and phase shifts of compressive oscillationsAuthors: Dmitrii Kolotkov, Sergey Belov, Mohamed Sherif,Comments: Accepted for publication in ApJ LettersSubjects: astro-ph.SRCreated: 2026-06-03; Updated: 2026-06-05; Datestamp: 2026-06-05
Magnetohydrodynamic (MHD) waves in coronal loops provide key seismological diagnostics through their characteristic time signatures. While fast and slow MAGNEToacoustic modes are routinely exploited, the entropy mode, despite being another eigenmode of the system, remains largely inaccessible due to its non-propagating and non-oscillatory nature. We identify possible observable time-domain signatures of the entropy mode and its indirect effects. Our approach exploits the intrinsically non-adiabatic conditions of the solar corona, under which the entropy mode is closely linked to the compressive slow mode. We consider a one-dimensional coronal loop model with field-aligned thermal conduction, where standing slow and entropy modes are simultaneously excited. We show that the entropy mode leaves distinct imprints on the total loop temperature and density perturbations. Specifically, its rapid decay relative to the slow mode produces a non-exponential damping profile during the initial oscillation cycles and introduces a pronounced asymmetry between the upper and lower temperature and density envelopes. These effects arise naturally from the superposition of two exponentially decaying components with different damping timescales. Furthermore, deviations from the canonical quarter-period phase shift between temperature/density and velocity perturbations in the standing slow mode are explained by the entropy-mode effect. We conclude that the entropy mode may be detected through its impact on compressive oscillations. Revealing its role in non-exponential damping, envelope asymmetry, and phase shifts of compressive oscillations makes the entropy mode potentially accessible to observations and lays the foundation for solar and stellar seismological applications.
[abstract 37 / 42] (score: 2) - Title: Galaxy morphology dependent (BLACK HOLE mass)-(velocity dispersion) relations: implications for gravitational wave forecasts and cosmological simulationsAuthors: Alister W. Graham,Comments: 23 pages (including an Appendix for SCOPE). Submitted to MNRAS on the 13th of May, 2026Subjects: astro-ph.GACreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
The correlation between BLACK HOLE mass, $M_{\rm bh}$, and stellar velocity dispersion, $σ_0$, is revisited using 137 galaxies with quantitative bar strengths and enhanced morphological awareness. Interpreted within the `Triangal' evolutionary framework, gas-rich and gas-poor assembly pathways emerge in the $M_{\rm bh}$--$σ_0$ diagram. To quantify these scaling relations, a versatile Bayesian hierarchical regression code, dubbed the Symmetric COvariance Population Estimator (SCOPE), is introduced. Unlike conditional estimators, SCOPE derives the intrinsic population covariance, natively accommodating asymmetric measurement errors while guaranteeing directional invariance between axes. Primeval, dust-poor S0 galaxies (including dwarf early-type galaxies with $R_{\rm e,gal}\approx1$~kpc) follow a shallow relation ($M_{\rm bh}\proptoσ_0^{2.5\text{--}3.1}$). Explained via the virial theorem, this flattening reframes expectations for intermediate-mass BLACK HOLEs. In contrast, tracing the `Disc Down-sizing' sequence - where dry mergers erase discs - yields a steep relation for massive elliptical and ellicular galaxies ($M_{\rm bh}\proptoσ_0^{7.8\pm1.4}$). The historical practice of applying a single, monolithic scaling relation across all morphological types averages over different formation histories, potentially skewing AGN virial $f$-factor calibrations and systematically under-predicting the ultra-massive BLACK HOLEs needed to generate the nanohertz gravitational wave background. Furthermore, strongly barred, dust-poor S0 galaxies appear offset to higher $σ_0$, while this dynamical signature is lost in the complexities of spiral galaxies. Ultimately, these morphology-dependent relations provide physically-motivated benchmarks for cosmological simulations and a framework for disentangling regimes driven by AGN feedback from those driven by collisionless mergers.
[abstract 38 / 42] (score: 2) - Title: Wave drag in moving plasmas: recent developments and prospectsAuthors: Renaud Gueroult, Aymeric Braud, Julien Langlois,Comments: 14 pages, 5 figuresSubjects: physics.plasm-phCreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
Wave propagation in a medium differs depending on whether this medium is at rest or moving with respect to an observer. Motion can notably lead to modifications of the wave trajectory, of its POLARIZATION, or of its transverse structure. Although these effects are well documented in isotropic dielectrics, they remain largely unexplored and unaccounted for in plasmas, despite the fact that simple models suggest they could in fact be large under certain conditions, as well as recent experimental observations. Here we first review existing models for motion effects on plasma waves, then identify a number of basic challenges that lie in the way of using these models to quantify motion effects in realistic configurations, and finally discuss possible workarounds.
[abstract 39 / 42] (score: 2) - Title: The first decade of gravitational-wave measurements of BLACK HOLE spinsAuthors: Sylvia Biscoveanu,Comments: Prepared for the Galaxies special issue on "Gravitational-Wave Probes of Black Hole Spin and Binary Dynamics"Subjects: gr-qcCreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
A decade after the first direct detection of gravitational waves, the growing catalog of over one hundred confirmed events is revealing new insights into the spins of stellar-mass BLACK HOLEs. Spin measurements have long been heralded as a promising tracer of compact-object binary formation and evolution, as different formation channels predict unique spin signatures on a population level. In this review, we summarize the astrophysics, phenomenology, and current measurements of BLACK HOLE spins. We begin with an overview of the predictions for BLACK HOLE spin magnitudes and orientations from leading formation channels--isolated binary evolution, dynamical formation in clusters, formation in AGN disks, and hierarchical triples. We then describe the imprint of spin effects on the gravitational waveform and the measurability of spin in individual events. Finally, we review current population-level constraints on spin magnitudes, orientations, and effective spin parameters, including correlations with mass and redshift, and discuss their astrophysical implications. We conclude by highlighting open questions and future prospects, emphasizing how improved detector sensitivity will enable increasingly precise spin measurements for both individual events and the binary BLACK HOLE population as a whole.
[abstract 40 / 42] (score: 2) - Title: A New Member of the Fast and Furious Family: A Relativistic and Time-Variable UV Outflow in a Luminous QuasarAuthors: Lucas M. Seaton, Patrick B. Hall, Liliana Flores, Paola Rodríguez Hidalgo, Marianna Veltri, Zezhou Zhu, Javier Serna, W. Niel Brandt, Scott Anderson, Roberto J. Assef, Eduardo Bañados, Catherine J. Grier, Yasaman Homayouni, Sean Morrison, C. Alenka Negrete, Amy L. Rankine, Jessie Runnoe, Donald P. Schneider, Yue Shen, Matthew Temple, Benny Trakhtenbrot, Jonathan R. Trump, Erik Weiss,Comments: 40 pages, 12 figures, 10 tables, published in the Astrophysical JournalSubjects: astro-ph.GACreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
We report the fastest QUASAR outflow first detected in the ultraviolet, via variable C IV and Si IV absorption at outflow velocities $-77,000$ km s$^{-1}$ to at least $-90,000$ km s$^{-1}$, in the radio-quiet QUASAR SDSS J231854.31+243954.2 (J2318). J2318 is a weak-lined QUASAR in the rest-frame ultraviolet, but Gemini GNIRS spectroscopy reveals an H$α$ redshift of $z=2.6781\pm0.0004$. A twenty-year photometric time series shows peak-to-peak variability of 0.5 mag in the $g$ band. The C IV outflow strengthened monotonically over three epochs spanning $\sim$2.2 rest-frame years. The existence of such a high-velocity outflow implies that models of QUASAR outflows must be able to either accelerate gas to $0.3c$ while still preserving C IV and Si IV ions, or enable the formation of C IV and Si IV ions in gas which has been accelerated to $0.3c$. Virial estimates reveal a black-hole mass of $1.65\times10^9~M_\odot$, which leads to an Eddington luminosity and Eddington ratio of $2.4\times10^{47}$ erg s$^{-1}$ and $0.45$, respectively. Using very conservative assumptions, the UV-absorbing outflow alone has an estimated mass loss of $>0.82~M_\odot~{\rm yr}^{-1}$ and a kinetic luminosity ratio $L_{kin}/L_{bol}\geq0.75$%. The lower limit is just above the threshold usually cited for significant feedback on the host galaxy. Comparison to PDS 456, the only other known QUASAR with a UV-absorbing outflow at $0.3c$, suggests that the true $\dot{M}$ and $L_{kin}/L_{bol}$ could be up to two orders of magnitude larger.
[abstract 41 / 42] (score: 2) - Title: A micronova burst in the intermediate polar IGR J17014-4306Authors: Alexandre S. Oliveira, D. C. Souza, G. J. M. Luna, C. V. Rodrigues,Comments: 7 pages, 4 figures, submitted to MNRASSubjects: astro-ph.HE astro-ph.SRCreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
We report the detection of a short optical burst in TESS data of IGR J17014-4306, the eclipsing intermediate polar with the longest known orbital period. The burst lasts 1.56 d and shows multiple peaks, reaching $(9.3 \pm 0.2) \times 10^{33}$ erg s$^{-1}$, and releases a total energy of $(3.25 \pm 0.01) \times 10^{38}$ erg. The burst parameters are consistent with those of a micronova eruption, currently understood as a thermonuclear runaway in the MAGNETically-confined accretion column. From its energy, we infer a burned column mass of $\sim 1.6 \times 10^{-11}$ M$_\odot$, which implies a recurrence time of $\sim 20$ d. Our search for similar events in long-term Gaia, ASAS-SN, and AAVSO light curves reveals 16 possible fast brightenings over $\sim 11$ yr, suggesting that micronova events may be frequent in IGR J17014-4306. Timing analysis of the TESS data shows that the white-dwarf spin period remains stable before and after the burst. During the burst, however, the power spectrum becomes more complex and exhibits multiple peaks. The classification of IGR J17014-4306 as a micronova brings the total number of confirmed systems to eight. Its extreme orbital period and eclipsing nature make it an ideal test-bed for further studies of MAGNETically confined thermonuclear burning on white dwarfs.
[abstract 42 / 42] (score: 2) - Title: A high-energy neutrino flare associated with nearby bright interacting SUPERNOVA SN 2021foaAuthors: Ming-Xuan Lu, Yun-Feng Liang, Xue-Rui Ouyang, Da-Bin Lin, Xiang-Gao Wang, Yi-Zhong Fan,Comments: 21 pages, 5 figuresSubjects: astro-ph.HECreated: 2026-06-04; Updated: 2026-06-05; Datestamp: 2026-06-05
While core-collapse SUPERNOVAe have been widely discussed as potential neutrino sources, definitive observational evidence has remained elusive. In this work, we report evidence of high-energy neutrino emission in the direction of SUPERNOVA SN 2021foa, which is one of the closest and brightest interacting SUPERNOVAe observed to date. Using the second data release of muon track data from the IceCube Neutrino Observatory, we conducted a time-dependent analysis and identified a neutrino clustering that temporally coincides with the optical peak of SN 2021foa, occurring approximately 16 to 22 days after the discovery date, with a maximum test statistic of $\sim 28.2$. Monte Carlo simulations indicate that the probability of observing such a neutrino excess by chance is $\sim6.7 \times 10^{-5}$, corresponding to a significance of $\sim4.0\,σ$. The spatial and temporal correlation strongly suggests that the neutrinos originate from the SUPERNOVA. SN 2021foa is a unique "flip-flop" SUPERNOVA; its spectra repeatedly transitioned between hydrogen-rich (Type IIn) and helium-rich (Type Ibn) phases within 50 days post-peak, reflecting a violent and complex mass-loss history of its progenitor. The inferred neutrino energy exceeds the optical radiative energy and ejecta kinetic energy of the SUPERNOVA by orders of magnitude, suggesting that the neutrino emission is likely powered by a delayed central engine driving a JET that is choked within the dense circumstellar medium.
arXiv:2606.05343 [pdf, ps, other]
arXiv:2606.05312 [pdf, ps, other]
arXiv:2411.02342 [pdf, ps, other]
arXiv:2605.21950 [pdf, ps, other]
arXiv:2606.04332 [pdf, ps, other]
arXiv:2606.05738 [pdf, ps, other]
arXiv:2606.05910 [pdf, ps, other]
arXiv:2606.06213 [pdf, ps, other]
arXiv:2601.04990 [pdf, ps, other]
arXiv:2606.05307 [pdf, ps, other]
arXiv:2606.05514 [pdf, ps, other]
arXiv:2606.05944 [pdf, ps, other]
arXiv:2602.16562 [pdf, ps, other]
arXiv:2605.17195 [pdf, ps, other]
arXiv:2606.05286 [pdf, ps, other]
arXiv:2606.05310 [pdf, ps, other]
arXiv:2509.10615 [pdf, ps, other]
arXiv:2511.09311 [pdf, ps, other]
arXiv:2602.16995 [pdf, ps, other]
arXiv:2603.07012 [pdf, ps, other]
arXiv:2606.04692 [pdf, ps, other]
arXiv:2606.05283 [pdf, ps, other]
arXiv:2606.05301 [pdf, ps, other]
arXiv:2606.05355 [pdf, ps, other]
arXiv:2606.05446 [pdf, ps, other]
arXiv:2606.05842 [pdf, ps, other]
arXiv:2606.06270 [pdf, ps, other]
arXiv:2510.19904 [pdf, ps, other]
arXiv:2510.25972 [pdf, ps, other]
arXiv:2602.14720 [pdf, ps, other]
arXiv:2603.03123 [pdf, ps, other]
arXiv:2604.03421 [pdf, ps, other]
arXiv:2604.23503 [pdf, ps, other]
arXiv:2605.05362 [pdf, ps, other]
arXiv:2606.05318 [pdf, ps, other]
arXiv:2606.05360 [pdf, ps, other]
arXiv:2606.05808 [pdf, ps, other]
arXiv:2606.06195 [pdf, ps, other]
arXiv:2606.06209 [pdf, ps, other]
arXiv:2606.06226 [pdf, ps, other]
arXiv:2606.06305 [pdf, ps, other]
arXiv:2606.06409 [pdf, ps, other]