Current date: 2026-06-01
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Number of records retrieved: 661
Keyword score statistics
score 9 -- 1 abstracts
score 6 -- 4 abstracts
score 5 -- 3 abstracts
score 4 -- 2 abstracts
score 3 -- 4 abstracts
score 2 -- 14 abstracts
in total -- 28 abstracts
Articles that appeared on 2026-06-01
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[abstract 1 / 28] Wow! (score: 9)
- Title: Extreme Transients in Gamma RaysAuthors: Daniela Hadasch, Dmitriy Khangulyan,Comments:Subjects: astro-ph.HECreated: 2026-05-29; Updated: 2026-06-01; Datestamp: 2026-06-01
Extreme gamma-ray transients represent some of the most energetic and physically constraining phenomena in high-energy astrophysics. They are characterized by rapid, large-amplitude variability and by physical conditions approaching fundamental limits on particle acceleration, cooling, and compactness. In this review, we focus on transients detected above around 100 MeV and define extreme events as either those involving catastrophic transformations of astrophysical systems (such as stellar explosions, compact-object mergers, and tidal-disruption events) or those exhibiting evidence for particle acceleration operating in an extreme regime. These systems are powered by the rapid release of gravitational, MAGNETic, nuclear, or kinetic energy, with shocks and MAGNETic RECONNECTion playing a central role in producing ultra-RELATIVISTIC particle populations and non-thermal radiation. We summarize observational and theoretical diagnostics that constrain the size, MAGNETization, and Lorentz factor of the emitting region, including variability timescales, luminosity-timescale correlations, and spectral evolution across the MeV-TeV domain. We further review the complementary capabilities of space-borne gamma-ray instruments, ground-based Cherenkov and air-shower observatories in detecting short-lived, high-energy outbursts. Extreme transient classes discussed include GAMMA-RAY BURSTs, novae, rapidly variable emission from extragalactic and Galactic JETs. Also, because of its extreme aspects, we include flaring emission detected from the Crab Nebula. While each type of these flares poses interesting challenges for phenomenology and theory of these sources, together, these events form the landscape of extreme gamma-ray variability.
[abstract 2 / 28] Yes (score: 6) - Title: Time-domain Radio-loudness of Active Galactic Nuclei: Intermittency, Memory, and Jet EscapeAuthors: Tao An,Comments: accepted for publications in ApJLSubjects: astro-ph.GA astro-ph.HECreated: 2026-05-29; Updated: 2026-06-01; Datestamp: 2026-06-01
The classical radio-loudness parameter $R \equiv f_ν(5\,\mathrm{GHz})/f_ν(4400\,\textÅ)$ divides a radio flux density by an optical/UV accretion tracer, but the two terms do not probe the same clock. The radio numerator can blend compact-core emission from the current engine, lobe and relic plasma left by earlier JET episodes, and host-galaxy SYNCHROTRON emission. We introduce a time-domain radio-loudness (TDRL) description that keeps these contributions separate. The radio numerator is written as compact-core and extended-lobe terms, with recovered fractions set by observing frequency, angular resolution, and surface-brightness sensitivity. For a single intermittently JETted AGN population, a two-state duty cycle filtered by exponential lobe fading gives an exact stationary Beta distribution for the normalized extended-radio response. Its mean is $\fduty$, while its variance scales as $(1+χ_ν)^{-1}$, where $χ_ν\equiv\taunu/t_{\rm switch}$. In this reference limit, the familiar GHz valley near the classical radio-loud/radio-quiet boundary can arise from short radio memory alone, without requiring two intrinsic engine classes. Metre-wave surveys that recover diffuse emission and subtract the host contribution should therefore progressively fill the valley. In the $(\Rcore,\Rlobe)$ plane, a core--lobe mismatch index separates triggering, sustained, and remnant phases, provided orientation-dependent core beaming is modelled or controlled. A complementary two-barrier picture, involving horizon-threading MAGNETic flux and JET escape through the nuclear medium, separates JET launching from the formation of large-scale radio structure. This view makes radio loudness a probe of JET duty cycle, radio memory, and escape through the host environment.
[abstract 3 / 28] Yes (score: 6) - Title: High-redshift GRB 140304A at z = 5.282 with flaring activity: A multi-wavelength studyAuthors: Shashi. B. Pandey, Amit. K. Ror, A. J. Castro-Tirado, A. Pozanenko, V. Lipunov, S. Jeong, I. H. Park, R. Sanchez-Ramirez, B. -B. Zhang, D. Xu, N. R. Butler, C. G. Mundell, S. R. Oates, P. Y. Minaev, A. Volnova, J. Bai, J. Bloom, N. Budnev, A. Castellon, Ch. Cui, M. D. Caballero-Garcia, Maria Gritsevich, G. Garcia-Segura, D. Hiriart, A. Valeev, S. Castillo-Carrion, Yash Sharma, Y. Fan, E. Gorbovskoy, O. Gress, S. Guziy, Y. -D. Hu, Brajesh Kumar, Amar Aryan, Rahul Gupta, E. V. Klunko, V. Kornilov, A. Kutyrev, G. Antipov, A. Kuznetsov, William H. Lee, C. Perez del Pulgar, R. Querel, M. G. Richer, S. E. Schmalz, N. Tiurina, N. Tungalag, K. Zhirkov, A. M. Watson, Ch. Wang, P. Balanutsa,Comments: 22 pages, 12 figures, 6 tables. Accepted for publication in Astronomy & AstrophysicsSubjects: astro-ph.HECreated: 2026-05-29; Updated: 2026-06-01; Datestamp: 2026-06-01
Context. This article presents a detailed multi-wavelength analysis of GRB 140304A at z = 5.282, having uncommon late-time flaring features. The aim is to study GRB 140304A and other similar bursts to understand stellar evolution and formation processes at high-z. Aims. GRBs at high-z, possible flaring activities at different frequencies seen at relatively late-times, help to constrain temporal correlation among contemporaneous flares. In the present study, we plan to constrain such a temporal and spectral study for a sample of high-z bursts, including GRB 140304A. Methods. We use SWIFT, FERMI, and ground-based observations to constrain the temporal and spectral properties of the prompt and afterglow emissions. Using the cross-correlation function, we calculate the spectral lag in the light curves observed in two energy bands of SWIFT's Burst Alert Telescope (BAT) and X-ray Telescope (XRT). Results. Parameter evolution of the prompt emission analysis reveals a hard-to-soft evolution of the spectral peak energy (Ep) and the MAGNETic field strength (B), consistent with the typical population of long GRBs. For GRB 140304A, a rare pattern of spectral lag evolution having positive lag in the early BAT light curves, but no lag is observed in the XRT light curves. We have also observed systematic time delays among the peak times of flares in three different bands, but the optical flares exhibit a morphological correspondence with X-ray or gamma-ray flares. Conclusions. Our analysis shows that the observed positive spectral lag in GRB 140304A is closely related to the hard-to-soft spectral evolution during the prompt emission phase, as seen in some of the other long GRBs. Additionally, there is a clear connection between gamma-ray, X-ray and optical flares with prompt emission, which are produced through SYNCHROTRON radiation during rapid bulk acceleration within the emitting region.
[abstract 4 / 28] Yes (score: 6) - Title: Expanding the Population of Short Gamma-Ray Transients with a Coherent FERMI/GBM Search. A 13-year catalog of short GRBsAuthors: Ariel Perera, Barak Zackay, Tejaswi Venumadhav,Comments:Subjects: astro-ph.HECreated: 2026-05-29; Updated: 2026-06-01; Datestamp: 2026-06-01
In this paper, we present an archival search for short GAMMA-RAY BURSTs (sGRBs) over 13 years (2013-2025) of FERMI/GBM data using a Poisson matched-filter pipeline that performs a fully coherent analysis across all detectors and energy channels, significantly improving sensitivity relative to the onboard triggering algorithms. A central component of the analysis is the empirical estimation of trigger significance using 'timeslided' data, allowing each candidate to be assigned a probability of astrophysical origin. We also developed a new parameter-estimation framework based on the Poisson matched filter, which uses the global structure of the detected event across spectral, temporal, and spatial parameter spaces. This enables us to systematically classify bursts and distinguish between GRBs, soft gamma repeaters, terrestrial gamma-ray flashes, and solar flares. We identify 568 new GRB candidates with $p_{\text{astro}}\geq0.9$ and thousands of MAGNETar bursts, significantly expanding the known short-transient population in GBM data. To further strengthen the significance of the GRB candidates, we performed a targeted follow-up search in SWIFT/BAT rate data. Applying the followup to all of our triggers - including triggers below the detection threshold yielded 1736 temporally coincident events with association probability above $90\%$. The resulting probabilistically ranked catalog substantially expands the population of short GRBs and MAGNETar flares detected in GBM data and provides a statistically robust framework for multimessenger searches.
[abstract 5 / 28] Yes (score: 6) - Title: Insights on the Gamma-Ray Bursts variability in their cosmological rest frameAuthors: Giovanni Della Casa, Fabrizio Fiore, Giuseppe Dilillo, Simonetta Puccetti, Andrea Vacchi,Comments: 12 pages, 18 figures Submitted to A&A. Revised versionSubjects: astro-ph.HECreated: 2026-05-29; Updated: 2026-06-01; Datestamp: 2026-06-01
Gamma-ray bursts temporal profile can be extremely variable, going from a single pulse of a few seconds duration to multiple superimposed pulses occurring over tens or even hundreds of seconds. The variability displayed in the lightcurve of each GAMMA-RAY BURST can be the result of the activity taking place in the central engine that generates these violent phenomena, as well as due to MAGNETic RECONNECTion activities at larger distances. The objective of this work is to find the shortest variability hidden in the lightcurves of the GRBs, with particular focus for the ones with measured redshift, on timescales as short as few milliseconds. This variability will then be related to physical characteristics of the central engine, and evidences of its relation with the spectral parameters of the burst, such as the isotropic energy and peak energy, will be presented. This research is even more relevant in view of the future generation of satellites with improved timing resolution, that will allow us to explore the possible variability in the microsecond region.
[abstract 6 / 28] Yes (score: 5) - Title: Non-Equilibrium Thermodynamics of Black-Hole Coronae: QPOs, Turbulence, and JetsAuthors: Vanessa López-Barquero, Alejandro Jenkins, Christopher S. Reynolds, Andrew Fabian,Comments: 9 pages. 3 figures. Refereed. Accepted for publication. HEPRO-IXSubjects: astro-ph.HE physics.flu-dyn physics.plasm-phCreated: 2026-05-28; Updated: 2026-06-01; Datestamp: 2026-06-01
The variability of X-rays observed from accreting BLACK HOLE systems, including quasi-periodic oscillations (QPOs), suggests a complex nonlinear dynamics in the corona. Here, we propose a new theoretical framework for this variability, based on non-equilibrium thermodynamics. In this model, coronal variability arises from feedback between a macroscopic oscillation of the plasma and the rate at which it is cooled by the inverse Compton scattering of soft photons from the disc. The "pair thermostat'' mechanism then allows the corona to act as a heat engine that extracts work cyclically from the underlying thermal disequilibrium between the low-entropy heating from the BLACK HOLE and the high-entropy cooling by soft photons from the disk, in close analogy to the well-known $κ$-mechanism for pulsating stars. This coronal self-oscillation may explain QPOs without invoking an external periodic driving. Moreover, we argue that this mechanism can generate coronal turbulence and JETs.
[abstract 7 / 28] Yes (score: 5) - Title: Magnetic Eruption and Nucleosynthesis in GRνMHD Simulations of Spinning Neutron Star MergersAuthors: Allen Wen, Jay V. Kalinani, Michail Chabanov, Manuela Campanelli, Riccardo Ciolfi, Yosef Zlochower,Comments: 21 pages, 25 figures, REVTeX 4.2Subjects: astro-ph.HE gr-qcCreated: 2026-05-28; Updated: 2026-06-01; Datestamp: 2026-06-01
We present three-dimensional general RELATIVISTIC MAGNETohydrodynamics simulations of equal-mass binary neutron star mergers with varied neutron star spin configurations and second-moment neutrino transport, following the formation and early evolution of long-lived remnants. We compare a fiducial irrotational binary with binaries having spins that are aligned or antialigned with the orbital angular momentum, and examime how spin affects the merger dynamics, MAGNETic field evolution, outflows, and nucleosynthesis. Compared to the fiducial case, the aligned spin configuration releases more cold, neutron-rich tidal ejecta in the equatorial plane, which enables the development of a more tightly collimated polar outflow erupting from the remnant and inner accretion disk. Conversely, the case with spins antialigned with the orbit experiences a more violent collision at merger, disrupting MAGNETic amplification, loading the environment with debris, and impeding the propagation of MAGNETically driven winds. Strong neutrino reprocessing of the polar outflow in the irrotational and aligned spin cases produces $2.4\times 10^{-3}\,M_\odot$ of proton-rich ($Y_e \geq 0.49$) material, resulting in the synthesis of light r-process elements including $^{56}Ni$, whose subsequent decay potentially sends a unique electroMAGNETic signal from long-lived remnants. However, the outflows remain too dense and slow to be consistent with typical short GAMMA-RAY BURSTs.
[abstract 8 / 28] Yes (score: 5) - Title: Unveiling the population of massive quenched galaxies at $z\ge2$ in the COLIBRE simulations -- II. The role of AGN feedback and environment on their emergenceAuthors: Ángel Chandro-Gómez, Claudia del P. Lagos, Chris Power, Willian M. Baker, Alejandro Benítez-Llambay, Evgenii Chaikin, Harry G. Chittenden, Camila Correa, Carlos S. Frenk, Filip Huško, Kei Ito, Robert J. McGibbon, Themiya Nanayakkara, Sylvia Ploeckinger, Alexander J. Richings, Matthieu Schaller, Joop Schaye, James W. Trayford, Francesco Valentino,Comments: Submitted for publication in MNRAS. This work is Part II of a two-paper series (Part I: arXiv:2512.16208). 23 pages (17 of main body and 6 of appendices). Comments welcomeSubjects: astro-ph.GACreated: 2026-05-29; Updated: 2026-06-01; Datestamp: 2026-06-01
Early ($z \gtrsim 2$) Massive ($M_{\star} \gtrsim 10^{10}\,\mathrm{M_{\odot}}$), Quenched Galaxies (MQGs) challenge current galaxy formation models. In this series, we study these systems using the new COLIBRE cosmological hydrodynamical simulations. Following the broad agreement between its predictions and observations found in the first paper, this second paper explores the processes driving galaxies to become massive and quenched in COLIBRE, identifying Active Galactic Nucleus (AGN) feedback as the primary quenching mechanism in both the thermal (L200m6 simulation) and hybrid (thermal+JET, L200m7h simulation) AGN feedback models implemented. However, the two models behave differently: while the thermal model efficiently quenches massive galaxies at $z>3$, the hybrid model is less effective because BLACK HOLEs (BHs) grow more slowly in the early Universe, and the JET component, which dominates the feedback energy, acts on longer timescales to impact galaxies. Both models predict QUASAR-like MQGs (AGN with $L_{\rm bol}\gtrsim10^{45}\,\mathrm{erg\,s^{-1}}$), with the most luminous systems associated with more recently quenched galaxies. Compared to star-forming galaxies of similar mass, MQGs host more massive BHs and exhibit higher STAR FORMATION efficiencies. These differences arise primarily from their environments before quenching, particularly at local ($\rm 0.3\,cMpc$) to intermediate scales ($\rm 1.0\,cMpc$), where overdense regions are associated with enhanced gas inflows, higher BH accretion and, hence, feedback power. We find that about $54\%$ ($20\%$) of the $z=3$ MQGs survive as the main progenitors of $z=0$ galaxies, although up to $56\%$ ($60\%$) experience rejuvenation episodes at $z<3$ in L200m6 (L200m7h). Our results highlight the central role of BH growth, AGN feedback and environment in driving rapid quenching in the early Universe.
[abstract 9 / 28] Yes (score: 4) - Title: Leptonic and hadronic models of high-energy nebula around V4641 SgrAuthors: Maksim Kleimenov, Andrii Neronov, Foteini Oikonomou, Dmitri Semikoz,Comments: 8 pages, 10 figuresSubjects: astro-ph.HECreated: 2026-05-29; Updated: 2026-06-01; Datestamp: 2026-06-01
A prominent, 200-pc-scale high-energy nebula surrounding the microQUASAR V4641 Sgr is the brightest known gamma-ray source in the Southern sky at $E > 100\,\mathrm{TeV}$. In this paper, we develop self-consistent leptonic, hadronic, and leptohadronic models that reproduce both the observed spectrum and morphology of the source. Purely leptonic models are energetically more favorable yet they require rather specific morphological assumptions. The gamma-ray morphology of the source can be better explained within a hadronic scenario based on the identification of cold gas structures spatially correlated with the observed gamma-ray emission. However, a purely hadronic model for the source emission requires a substantial energy reservoir in protons and fails to reproduce the extended x-ray emission recently detected by XRISM. We show that emission including a combination of leptonic and hadronic components can reproduce both the spectral and morphological properties of the source. We provide predictions for the x-ray and neutrino spectra of the nebula that can discriminate the hadronic and leptonic contributions to the overall source signal.
[abstract 10 / 28] Yes (score: 4) - Title: High-ionization coronal lines trace QUASAR-like activity in recently quenched galaxies at high redshiftAuthors: F. Valentino, K. Ito, M. Farcy, F. Fontanot, C. Lagos, G. De Lucia, M. Hirschmann, G. Brammer, V. Kokorev, M. Hamadouche, P. Zhu, G. Scarpe, A. Pensabene, K. E. Whitaker, W. M. Baker, P. Araya-Araya, J. Antwi-Danso, D. Ceverino, A. L. Faisst, S. Fujimoto, S. Gillman, O. Ilbert, C. K. Jespersen, T. Kakimoto, M. Kubo, A. W. S. Man, G. Magdis, M. Onodera, R. Shimakawa, M. Tanaka, S. Toft, L. Xie, J. R. Weaver, P. -F. Wu,Comments: Submitted to A&A, 14 pages, 9 figures, 1 appendixSubjects: astro-ph.GA astro-ph.HECreated: 2026-05-28; Updated: 2026-06-01; Datestamp: 2026-06-01
We report the detection of the high-ionization line [NeV]$λ$3427 in the JWST/NIRSpec archival spectra of 6 massive quenched galaxies at $z \sim 1.5-4.5$, identified from a parent sample of 87 systems. With an ionization potential of approximately 97 eV, [NeV] can only be produced by strong nuclear activity in these massive systems, providing a clean and unambiguous tracer of highly accreting supermassive BLACK HOLEs uncontaminated by residual STAR FORMATION. For 4 of the 6 [NeV]-detected systems, we detect broad H$α$ emission ($\mathrm{FWHM} \gtrsim 4000$ km s$^{-1}$), yielding BLACK HOLE masses of $M_{\rm BH} = 10^{8.5-9.5}\,M_\odot$, consistent with local scaling relations with stellar mass and velocity dispersion. The [NeV] luminosities imply QUASAR-like bolometric outputs ($L_{\rm bol} = 10^{45-46}$ erg s$^{-1}$) and Eddington ratios of $λ_{\rm Edd} \approx 10$-$50$%, with BLACK HOLE accretion rates of a few $M_\odot$ yr$^{-1}$ that match or exceed the residual STAR FORMATION rates in the most extreme cases. The strongest [NeV] emitters are preferentially found in the youngest post-starburst systems ($D_n4000 \lesssim 1.3$), while old quenched galaxies are systematically devoid of such activity, a trend independently reproduced by theoretical models. These results reveal that intense, radiatively efficient SMBH growth can persist several hundred Myr after the main quenching epoch, with duty cycles of approximately 100-200 Myr. They also underscore the importance of very high accretion episodes and rates in the theoretical models that seek to reproduce the earliest quenched galaxies in the universe.
[abstract 11 / 28] (score: 3) - Title: Evaluation of the beam-induced dePOLARIZATION of the HJET target at the EICAuthors: A. A. Poblaguev,Comments: 17 pages, 11 figures, 5 tablesSubjects: physics.ins-det physics.acc-phCreated: 2026-05-28; Updated: 2026-06-01; Datestamp: 2026-06-01
The Polarized Atomic Hydrogen Gas Jet Target (HJET) has played a central role in the absolute calibration of proton beam POLARIZATION at RHIC and is foreseen as a key component of the hadron polarimetry program at the future Electron--Ion Collider (EIC). The substantially higher beam current, reduced bunch spacing, and shorter bunch length planned for EIC operation motivate a careful reassessment of possible beam-induced dePOLARIZATION of the JET target. In this paper, the dePOLARIZATION of ground-state hydrogen atoms caused by the time-dependent MAGNETic field of the circulating polarized proton beam is quantitatively evaluated. The hydrogen atom is treated as a four-level hyperfine system in a holding MAGNETic field, and transitions driven by harmonic components of the bunch-induced MAGNETic field are analyzed using time-dependent quantum-mechanical evolution along atomic trajectories. Numerical tracking of hydrogen atoms through the beam region is performed using nominal EIC beam parameters. It is shown that, for a holding field of $120 \mathrm{mT}$ (as used at RHIC), the resulting dePOLARIZATION of the JET target at the EIC is negligibly small, $\lesssim 0.01\%$, and well below the level relevant for EIC POLARIZATION accuracy requirements. The stability of this result with respect to plausible variations of the EIC proton beam parameters is also evaluated. In addition, possible effects under alternative experimental conditions are also examined.
[abstract 12 / 28] (score: 3) - Title: A Rapid Evolution in the Observed Mbh/M* Relation at z > 3 Revealed via Spectro-photometric SED-ModelingAuthors: Ansh R. Gupta, Anthony Taylor, Emma Curtis-Lake, Maddie Silcock, Óscar A. Chávez Ortiz, Steven L. Finkelstein, Hollis B. Akins, Bren E. Backhaus, Guillermo Barro, Laura Bisigello, Madisyn Brooks, Caitlin M. Casey, Stephane Charlot, Jacopo Chevallard, Anna Feltre, Giovanni Gandolfi, Mauro Giavalisco, Norman A. Grogin, Michaela Hirschmann, Tiger Yu-Yang Hsiao, Junehyoung Jeon, Shardha Jogee, Jeyhan S. Kartaltepe, Dale D. Kocevski, Anton M. Koekemoer, Vasily Kokorev, Gene C. K. Leung, Ray A. Lucas, Fabio Pacucci, Nor Pirzkal, Adele Plat, Rachel S. Somerville, Jonathan R. Trump, Alba Vidal-García, Xin Wang, L. Y. Aaron Yung,Comments: Main text 19 pages, 9 figures. Submitted to ApJ. Comments welcome! Machine-readable tables and figure sets are available at https://zenodo.org/records/20419666Subjects: astro-ph.GACreated: 2026-05-28; Updated: 2026-06-01; Datestamp: 2026-06-01
Spectroscopic observations from JWST have uncovered a plethora of ACTIVE GALACTIC NUCLEi (AGN) at z > 4 with BLACK HOLE (BH) mass (Mbh) to stellar mass (M*) ratios significantly above the local relation when using standard virial mass scaling relations. However, M* estimates of AGN may be inaccurate due to limitations in spectral energy distribution (SED) fitting codes, exemplified by a lack of physically-motivated AGN line emission models. Here, we fit NIRSpec/PRISM spectra of 39 galaxies at z ~ 3.5-7 selected as broad-line AGN from the CEERS and RUBIES surveys. Applying kinematic decompositions from NIRSpec/G395M spectra, we fit their continuum and narrow-component line fluxes using the BEAGLE-AGN SED fitting tool. While limitations of BEAGLE-AGN make it difficult to model little red dots (LRDs), we find that M* estimates of non-LRDs are, surprisingly, only modestly impacted by the inclusion or not of AGN narrow-line region (NLR) and continuum emission model components. We further find that non-LRD AGN at z < 3.5 are consistent with the local Mbh/M* relation while those at z > 4.5 display elevated ratios. While we cannot rule out observational biases or systematic uncertainties as partial causes, this transition over just ~500 Myr is driven entirely by changes in M* rather than an evolving Mbh distribution. These findings are consistent with models in which rapid BH growth results in elevated Mbh/M* ratios at early times, with a swift late-time assembly of host galaxies returning sources to the local relation at z < 4.
[abstract 13 / 28] (score: 3) - Title: Storm-Time Cusp Precipitation: Insights from TRACERS Multi-Crossing ObservationsAuthors: Shirsh Lata Soni, David M. Miles, Jasper Halekas, Stephen A. Fuselier, George Hospodarsky, Marit Øieroset, K. J. Trattner, S. M. Petrinec, Jeremy Faden, Ivar Christopher, Chris Pikar, Sarah A. Henderson, Daniel Da Silva, Scott Bounds, Robert Strangeway,Comments: Submitted to JGR: space Physics (under review)Subjects: physics.space-phCreated: 2026-05-28; Updated: 2026-06-01; Datestamp: 2026-06-01
The dayside cusp provides a direct pathway for solar wind plasma entry into the MAGNETosphere ionosphere system through MAGNETic RECONNECTion. Using low altitude ion and electron measurements from TRACERS, together with upstream solar wind and geoMAGNETic conditions, we investigate the evolution of the cusp during a geoMAGNETic storm on 30 September 2025, spanning its rising, main, and recovery phases, and compare these with a quiet-time reference. Storm-time observations show broader and more poleward precipitation regions and enhanced electron energy flux, indicating intensified dayside coupling. To interpret these variations, we combine solar wind and IMF measurements with the maximum MAGNETic shear RECONNECTion model to determine X-line locations and use a Tsyganenko field model to compute event-specific field-line transit distances between the X-line and TRACERS. The results demonstrate that cusp morphology and latitude track IMF-driven RECONNECTion geometry, and that realistic path lengths are essential for quantitative RECONNECTion-rate estimates, highlighting the capability of TRACERS to resolve storm-time cusp evolution. Enhanced cusp precipitation during the recovery phase is consistent with IMF conditions, indicating sustained solar wind driving rather than intrinsic storm-phase effects.
[abstract 14 / 28] (score: 3) - Title: Gyrokinetic global simulation of Alfvenic ion temperature gradient mode in reversed MAGNETic shearAuthors: Gengxian Li, Zhixin Lu, Philipp Lauber, Matthias Hoelzl, Guo Meng, Yong Xiao,Comments:Subjects: physics.plasm-phCreated: 2026-05-29; Updated: 2026-06-01; Datestamp: 2026-06-01
In this work, a systematic study of electroMAGNETic instabilities driven by the temperature gradient in MAGNETically confined fusion plasmas with reversed MAGNETic shear is conducted using gyrokinetic particle-in-cell simulations. An electroMAGNETic instability arising in the low-beta regime is investigated, where beta=8*pi*nT/B^2 denotes the ratio of plasma pressure to MAGNETic pressure. Within a reversed shear safety factor (q) profile, when a mode rational surface coincides with the position of zero shear, an instability dominated by only one poloidal harmonic emerges, rather than the conventional ion-temperature-gradient (ITG) mode. Simulation results demonstrate that the instability exhibits pronounced electroMAGNETic POLARIZATION even in the low-beta regime, with a real frequency significantly higher than that of ITG modes, and show that it is destabilized by the temperature gradient and not by the density gradient. This instability can be observed even for a monotonic q profile with weak MAGNETic shear. Based on a systematic comparison with other typical electrostatic and electroMAGNETic instabilities, this instability is identified as a weak shear Alfvenic-ion-temperature-gradient (WSAITG) mode, which may provide an explanation for the low-frequency Alfven modes (LFAM) observed in experiments. Wave-particle resonance analysis in phase space reveals that, in contrast to the ITG mode, well-passing particles provide an additional resonant population that drives the WSAITG mode.
[abstract 15 / 28] (score: 2) - Title: Strong deflection limit analysis of BLACK HOLE lensing in inhomogeneous plasmaAuthors: Fabiano Feleppa, Valerio Bozza, Oleg Yu. Tsupko,Comments: 18 pages, 13 figures, 2 tables; v6: corrected typos in Eqs. (89) and (120); results and conclusions unchangedSubjects: gr-qcCreated: 2026-05-29; Updated: 2026-06-01; Datestamp: 2026-06-01
This paper investigates gravitational lensing effects in the presence of plasma in the strong deflection limit, which corresponds to light rays circling around a compact object and forming higher-order images. While previous studies of this case have predominantly focused on the deflection of light in a vacuum or in the presence of a homogeneous plasma, this work introduces an analytical treatment for the influence of a non-uniform plasma. After recalling the exact expression for the deflection angle of photons in a static, asymptotically flat and spherically symmetric spacetime filled with cold non-MAGNETized plasma, a strong deflection limit analysis is presented. Particular attention is then given to the case of a Schwarzschild spacetime, where the deflection angle of photons for different density profiles of plasma is obtained. Moreover, perturbative results for an arbitrary power-law radial density profile are also presented. These formulae are then applied to the calculation of the positions and magnifications of higher-order images, concluding that the presence of a non-uniform plasma reduces both their angular size and their magnifications, at least within the range of the power-law indices considered. These findings contribute to the understanding of gravitational lensing in the presence of plasma, offering a versatile framework applicable to various asymptotically flat and spherically symmetric spacetimes.
[abstract 16 / 28] (score: 2) - Title: On the effective spin-mass ratio relation of binary BLACK HOLE mergers that evolved in isolationAuthors: Sambaran Banerjee, Aleksandra Olejak,Comments: 38 pages, 28 figures. New figures and expanded text. Resubmitted to OJA after addressing referee report. Comments are welcomeSubjects: astro-ph.HE astro-ph.SR gr-qcCreated: 2026-05-29; Updated: 2026-06-01; Datestamp: 2026-06-01
The ground-based measurement of gravitational waves (GW) from merging binary BLACK HOLEs (BBH) allows independent determination of spins of stellar-remnant BLACK HOLEs (BH). The observed population of BBH mergers exhibits two intriguing peculiarities related to BH spins, namely, a positively biased distribution of the effective spin parameter, $χ_{\rm eff}$, and an apparent anti-correlation between merger mass ratio, $q$, and $χ_{\rm eff}$. Here we investigate the potential mechanisms for such observed properties, in BBH mergers via isolated binary evolution. We synthesise BBH mergers with the fast binary evolution code BSE. The role of various physical assumptions is explored, including tidal spin-up, compact remnant mass, and mass transfer physics. We compare the properties of BBHs that form through stable mass transfer (SMT) and common envelope evolution (CE). We find that both the asymmetry in the $χ_{\rm eff}$ distribution and the $χ_{\rm eff}$ anti-correlation can be natural outcomes of isolated-binary BBH formation. The anti-correlation is especially pronounced for SMT-channel BBH mergers that experience a mass-ratio reversal, i.e., those where the second-born BH is the more massive one. The anti-correlation arises from the dependence of orbital shrinking during mass transfer and the Roche lobe size on the system's mass ratio. This characteristic $χ_{\rm eff}-q$ trend diminishes with increasing metallicity and when the isolated-binary BBH merger population is mixed with a significant contribution of dynamically formed BBH mergers or the newly formed BH's spin is misaligned relative to the parent star's spin. Our results demonstrate that isolated massive binary evolution via the SMT sub-channel can reproduce trends in the observable BBH merger population, with the characteristic signatures in mass, mass ratio, and spin distributions.
[abstract 17 / 28] (score: 2) - Title: Vortex driven Schwinger pair creation in the MAGNETosphere of SgrA*Authors: Zaza N. Osmanov,Comments: 7 pages, 1 figure1Subjects: astro-ph.HECreated: 2026-05-28; Updated: 2026-06-01; Datestamp: 2026-06-01
In this work, we explore the possibility of Schwinger pair creation triggered by MAGNETo-centrifugal effects in the MAGNETosphere of SgrA*. We show that these effects become extremely efficient in the presence of a vortex-driven MAGNETic field, whose strength exceeds previous estimates by several orders of magnitude. The dynamics of MAGNETo-centrifugally accelerated charged particles leads to charge separation, thereby parametrically exciting Langmuir waves. The associated electric field grows exponentially and upon reaching the Schwinger critical threshold, initiates efficient electron-positron pair production, which is ultimately saturated by annihilation processes.
[abstract 18 / 28] (score: 2) - Title: Evidence for Three Subpopulations of Merging Binary Black Holes at Different Primary MassesAuthors: Sharan Banagiri, Eric Thrane, Paul D. Lasky,Comments:Subjects: astro-ph.HECreated: 2026-05-29; Updated: 2026-06-01; Datestamp: 2026-06-01
With the release of the fourth LIGO--Virgo--KAGRA gravitational-wave catalog (GWTC-4), we are starting to gain a detailed view of the population of merging binary BLACK HOLEs. The formation channels of these BLACK HOLEs is not clearly understood, but different formation mechanisms may lead to subpopulations with different properties visible in gravitational-wave data. Adopting a phenomenological approach, we find GWTC-4 data supports the presence of at least three subpopulations, each associated with a different range of BLACK HOLE mass and with sharp transition boundaries between them. Each subpopulation is characterized by different distributions for either the mass ratios, the black-hole spin magnitudes or both. Subpopulation A with primary mass $m_1 \leq 27.7^{+4.1}_{-3.4} M_{\odot}$ ($90 \%$ credibility), is characterized by a nearly flat mass ratio distribution $q=m_2/m_1$, and by small spin magnitudes ($χ\leq 0.5^{+0.1}_{-0.1}$). Subpopulation B with $27.7^{+4.1}_{-3.4} M_{\odot} \leq m_1 \leq 40.2^{+4.7}_{-3.2} M_{\odot}$, has a much sharper preference for mass ratio $q \approx 1$. Subpopulation C, with $m_1 \geq 40.2^{+4.7}_{-3.2} M_{\odot}$, has support for large spin magnitudes, and tentative support for mass ratios $q\approx0.5$. We interpret these transitions as evidence for multiple subpopulations, each potentially associated with a different formation pathways. We suggest potential formation scenarios for each subpopulations, and suggest that Subpopulation B may be associated with chemically homogeneous evolution or population III stars. Our findings for Subpopulation C are largely consistent with recent claims of hierarchical mergers, but with some curious differences in properties.
[abstract 19 / 28] (score: 2) - Title: Graybody factors and absorption cross-sections of non-exchange BLACK HOLEs in Instein-coupled scalar fieldsAuthors: Sihao Fan, Wenjun Guo, Chen Wu,Comments:Subjects: gr-qcCreated: 2026-05-29; Updated: 2026-06-01; Datestamp: 2026-06-01
This paper studies scalar field perturbations coupled with Einstein tensors of non-exchange BLACK HOLEs. We use the POLARIZATION method to calculate graybody factors and absorption cross-sections selected by different parameters, and verify the latest correspondence between graybody factors and quasi-normal states. The results show that the larger the value of the non-exchange parameter $θ$ and the coupling constant $η$ introduced into the model, the smaller the absorption cross-section. Furthermore, we found that this correspondence is accurate for non-commutative BLACK HOLEs at the $1$ limit of large angular momentum quantum numbers.
[abstract 20 / 28] (score: 2) - Title: Near-axis quasi-isodynamic databaseAuthors: Eduardo Rodriguez, Gabriel G. Plunk,Comments:Subjects: physics.plasm-phCreated: 2026-05-29; Updated: 2026-06-01; Datestamp: 2026-06-01
In this work, we investigate the landscape of quasi-isodynamic stellarators using the near-axis expansion of the MAGNETic field. Building on recent theoretical developments, we construct a database of more than 800,000 stable, approximately quasi-isodynamic vacuum MAGNETic configurations. These configurations span a range of field period numbers and other geometric control parameters, including the MAGNETic axis shape and plasma elongation. To evaluate each configuration, we use a broad set of measures, including effective ripple, sensitivity of the Shafranov shift to changes in plasma beta, the prevalence of maximum-J trapped particles, and the Rosenbluth-Hinton residual, among others. This enables an exhaustive, thorough and quantitative characterization of the database. Statistical analysis and modern machine learning techniques are then employed to find correlations, and identify key descriptors and heuristics to help understand tendencies that govern the behaviour of numerical optimization. The database provides baseline configurations for further studies, and to serve as tailored initial conditions for optimization. With this work we initiate a long term program to complete a systematic exploration of quasi-isodynamic stellarator design space.
[abstract 21 / 28] (score: 2) - Title: Anisotropic Diffusion in Pulsar Halos: Interpreting the asymmetric morphology of Geminga and Monogem halos measured by HAWCAuthors: Si-Zhe Wu, Chao-Ming Li, Ruo-Yu Liu,Comments: 11 pages, 8 figures, 2 tableSubjects: astro-ph.HECreated: 2026-05-29; Updated: 2026-06-01; Datestamp: 2026-06-01
Pulsar halos are produced by electrons and positrons diffusing in the interstellar medium around their parent pulsar wind nebulae. Recent observations by HAWC and LHAASO have revealed asymmetric morphologies in the halos surrounding Geminga and Monogem. The anisotropic diffusion model provides a natural explanation for such asymmetries, where the morphology is determined by the viewing angle of the mean MAGNETic field, the Alfvénic Mach number ($M_{\rm A}$), and the pulsar distance. In this work, we model the measured morphologies based on this framework and constrain the properties of interstellar MAGNETic turbulence. We find that the mean MAGNETic field orientations within the two halos are different, implying that they reside in different MAGNETic coherence regions, whereas the Alfvénic Mach numbers are relatively close ($M_{\rm A}\sim 0.2$). The results suggest a local MAGNETic field coherence length of approximately 100pc. Our study demonstrates that the morphology of pulsar halos serves as a powerful diagnostic tool for the properties of interstellar MAGNETic fields, highlighting the need for more accurate morphological measurements and sophisticated diffusion modeling in future studies.
[abstract 22 / 28] (score: 2) - Title: 5D BLACK HOLEs and mirror (topological) stars from nonlinear electrodynamics: Existence and stabilityAuthors: Kirill A. Bronnikov, Sergei V. Bolokhov, Milena V. Skvortsova,Comments: 16 pages, 5 figures. Description extended, a few references addedSubjects: gr-qcCreated: 2026-05-29; Updated: 2026-06-01; Datestamp: 2026-06-01
We consider static, spherically symmetric solutions of 5D general relativity with MAGNETic fields governed by nonlinear electrodynamics (NED) with the Lagrangian $L(\cal F)$, ${\cal F} = F_{AB} F^{AB}$, and show that generic solutions describe either 5D BLACK HOLEs (also called black strings due to a circular extra dimension) or so-called mirror stars with perfectly reflecting boundary surfaces (also called topological stars), not to be confused with 4D configurations of mirror matter considered in particle physics. Two particular examples of such solutions have been obtained, admitting analytic expressions for the metric coefficients and $L(\cal F)$, and their stability under radial (monopole) perturbations is studied. While the whole obtained family of BLACK HOLE solutions turns out to be stable, mirror star solutions prove to be stable only in a certain range in the parameter space. We thus extend to the Einstein-NED system the results previously obtained for Einstein-Maxwell fields.
[abstract 23 / 28] (score: 2) - Title: QPOs from the Viscous Transonic Accretion Flow Around a Spinning Black HoleAuthors: Sanjit Debnath, Indranil Chattopadhyay, Soumyadip Mandal, Raj Kishor Joshi, Priyesh Kumar Tripathi, M. Saleem Khan,Comments: 14 pages, 10 figures; Accepted for publication in Journal of High Energy Astrophysics (JHEAP)Subjects: astro-ph.HECreated: 2026-05-29; Updated: 2026-06-01; Datestamp: 2026-06-01
We investigate the dynamics of transonic advective accretion flows around spinning BLACK HOLEs in the presence of viscosity. The spacetime of a Kerr BLACK HOLE is approximated using a pseudo-potential. We study viscously driven shock oscillations over a range of BLACK HOLE spin parameters. Our results show that the frequency range of quasi-periodic oscillations (QPOs) obtained from the power density spectra depends strongly on the BLACK HOLE spin. Low-spin systems predominantly exhibit low-frequency QPOs, whereas rapidly rotating BLACK HOLEs (greater than 0.9 Kerr parameter) produce QPOs spanning a broad range from low to high frequencies, comparable to those observed in BLACK HOLE X-ray binaries. We further obtain a correlation between the QPO frequency and the power-law photon index by computing the spectrum for a 10 solar mass BLACK HOLE.
[abstract 24 / 28] (score: 2) - Title: Simultaneous modeling of FeII emission in the optical and near-infrared in a prototypical Narrow-Line Seyfert 1 galaxyAuthors: Denimara Dias dos Santos, Swayamtrupta Panda, Alberto Rodríguez-Ardila, Murilo Marinello,Comments: Accepted for publication in ApJ; 21 pages, 15 figuresSubjects: astro-ph.GACreated: 2026-05-28; Updated: 2026-06-01; Datestamp: 2026-06-01
This work investigates the FeII emission in ACTIVE GALACTIC NUCLEi (AGN), combining observational data from optical and near-infrared (NIR) spectra of the prototypical FeII emitter IZw1 with state-of-the-art photoionization modeling. Using updated FeII atomic datasets (Smyth et al. 2019; Tayal & Zatsarinny 2018; Bautista et al. 2015), we explore a wide parameter space to determine the physical conditions of FeII-emitting regions in the broad-line region (BLR). Our results show that optical ($R_{\rm 4570}$) and NIR ($R_{\rm 1μm}$) FeII emission can be simultaneously reproduced under consistent conditions, with the best agreement obtained using the Smyth et al. (2019) dataset, for hydrogen densities of $10^{11.0}$ to $10^{12.0}$ cm$^{-3}$ and near-solar metallicity. We quantify, for the first time, the impact of Lyman-$α$ fluorescence on the physical conditions of FeII emission in both regimes, revealing its dominant role in the NIR and, in contrast, highlighting the stronger influence of collisional processes in the optical. Additionally, for the first time, we compare optical and NIR FeII emission simultaneously with OI and the CaII triplet (CaT), reinforcing their connection to similar spatial regions and physical properties, as well as their usefulness as better proxies for optical FeII. Our findings support the idea of a vertical BLR structure, with NIR FeII and OI originating in less dense regions of the cloud than optical FeII and CaT.
[abstract 25 / 28] (score: 2) - Title: Mapping the Universe as a Bianchi I cosmology with Gaia dataAuthors: Valeri V. Makarov, Asta Heinesen, Thomas Schücker,Comments: Accepted for publicationSubjects: astro-ph.CO astro-ph.GACreated: 2026-05-28; Updated: 2026-06-01; Datestamp: 2026-06-01
Measurements of tangential drifts of distant QUASARs and galactic nuclei on the celestial sphere provide a novel and independent method of testing cosmological hypotheses. In this work, we employ an axisymmetric Bianchi I model as a relatively simple phenomenological model that is useful for quantifying departures from the cosmological principle. Using a quality-filtered sample of 1.2 million proper motion vectors of distant QUASARs from Gaia Data Release 3, we perform global fits of the position drift fields with vector spherical harmonics (VSH) to second degree for five non-overlapping subsets of the sources with redshifts from 0.5 to 3, and assess the ability of the Bianchi I model to describe the signal. We theoretically demonstrate that an axisymmetric Bianchi I model produces a signal that can be described as a single quadrupole VSH term with an eigendirection which is aligned with the axis of maximum expansion anisotropy. We estimate this preferred direction from the Gaia data and the VSH fit, and perform point-estimates of the amplitude of the signal as a function of redshift. Although a significant quadrupole signal is detected in each bin, the increase of the amplitude of the signal with redshift predicted by the Bianchi I model is not confidently confirmed. The estimated value of the local expansion shear is higher than expected. Possible advances in describing the kinematic patterns of a high-redshift Universe with more complex cosmologies accommodating time-dependent anisotropy and rotation are discussed.
[abstract 26 / 28] (score: 2) - Title: Interstellar Scintillation of Three Nearby Pulsars with FASTAuthors: Ying-ying Ren, Shi-jun Dang, Zi-wei Wu, Yu-lan Liu, Yan-qing Cai, Qi-jun Zhi, Lun-hua Shang, Ru-shuang Zhao,Comments: Journal of High Energy Astrophysics (JHEAp), doi:10.1016/j.jheap.2026.100628Subjects: astro-ph.HECreated: 2026-05-29; Updated: 2026-06-01; Datestamp: 2026-06-01
Interstellar scintillation probes the properties of the ionized interstellar medium as well as the dynamical behavior of pulsars themselves. Using the Five-hundred-meter Aperture Spherical Radio Telescope, we obtained hour-long observations of PSRs~J0837+0610, J1136+1551, and J1239+2453. We detected a single scintillation arc in PSRs~J0837+0610 and J1239+2453, and identified three distinct arcs in PSR~J1136+1551. Our analysis reveals that the arc curvature scales with observing frequency as $η\propto ν^{-2.0\pm0.6}$ for PSR J0837+0610, and as $η\propto ν^{-1.9\pm0.6}$ for PSR J1239+2453. For PSR J1136+1551, the two clearest arcs exhibit scaling relations of $η\propto ν^{-1.6\pm0.6}$ and $η\propto ν^{-2.0\pm0.4}$, respectively. However, the frequency dependence of the third arc could not be constrained due to its low signal-to-noise ratio at higher frequencies. Moreover, the corresponding scattering screens are measured at distances ranging from 30 to 420 pc from Earth. However, long-term scintillation monitoring or VLBI observations are needed to reliably measure the scattering screen.
[abstract 27 / 28] (score: 2) - Title: The MeerKAT Thousand-Pulsar Polarisation Array II: Searches for Ultralight Axion-Like Dark MatterAuthors: Zi-Yan Yuwen, Michael Sarkis, Yin-Zhe Ma, Tao Liu, Jing Ren, Patrick Weltevrede, Xiao Xue,Comments: 14 pages in total, 9 figuresSubjects: astro-ph.HE astro-ph.COCreated: 2026-05-29; Updated: 2026-06-01; Datestamp: 2026-06-01
We construct Pulsar Polarisation Arrays (PPA), using regular pulsars monitored in MeerKAT's Thousand Pulsar Array (TPA) Programme, to search for Axion-like Dark Matter (ALDM) within Milky Way. Specifically, from a catalogue of 1237 regular pulsars, we select the 50 ones with the highest signal-to-noise ratio and set upper limits on the ALDM Chern-Simons coupling. We find no signals with statistical significance over the mass range of $[10^{-23},10^{-20}]\,{\rm eV}$ in the six-year MeerKAT's data. By combining the high-quality TPA pulsars and the accurate ionospheric subtraction of spinifex, we establish the most sensitive upper limits to the date on the ALDM Chern-Simons coupling, namely $\lesssim 10^{-14} - 3\times 10^{-13}\,{\rm GeV}^{-1}$, for the mass range of $[10^{-23},10^{-21}]\,{\rm eV}$ except at $m_a \sim 1.3 \times 10^{-22}\,$eV. This study underscores the great potential of constructing regular-pulsar PPAs for scientific tasks.
[abstract 28 / 28] (score: 2) - Title: Collective Winds of Massive Star Clusters as the Dominant PeVatrons for Galactic Cosmic RaysAuthors: Zijian Qiu, Sujie Lin, Lili Yang,Comments: 15 pages, 10 figures, 3 tables. Submitted to PRDSubjects: astro-ph.HECreated: 2026-05-29; Updated: 2026-06-01; Datestamp: 2026-06-01
The knee feature in the cosmic-ray energy spectrum around 4 PeV is widely believed to have a Galactic origin, but the acceleration mechanism and identification of PeVatrons remain key open questions in high-energy astrophysics. Recent precise measurements by LHAASO reveal that the proton and helium spectra exhibit a common rigidity-dependent spectral break at ~ 3.5 PV, imposing a stringent constraint on source models. In this work, we construct, for the first time, a time-dependent cosmic-ray injection model that incorporates the full evolution of massive stars together with the dynamical development of wind termination shocks. We find that stellar winds of individual massive stars cannot explain the common spectral break observed by LHAASO, as they yield distinct rigidity cutoffs for protons and helium. By contrast, collective winds of massive star clusters naturally reconcile this discrepancy through the mixing effect of stars at different evolutionary stages. We propose a stellar-dominated model in which SUPERNOVA remnants dominate the GeV-TeV range, individual stellar winds dominate the TeV range, and collective cluster winds dominate the PeV knee region. This model successfully reproduces the rigidity-dependent spectral features of various species near 100 GV and 0.1 PV. It further makes two testable predictions for future observations. Around 0.5 PV, the energy spectra of carbon and oxygen are expected to exhibit hardening similar to that of helium, which can be verified by LHAASO observations. In the multi-TV range, the energy spectrum of magnesium is not expected to show hardening similar to that observed for helium, carbon, and oxygen, which can be tested by DAMPE observations.
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