Current date: 2026-05-19
Setting default datestamp limit: 0
Datestamp limit: 2026-05-19 (0 days ago)
Created/updated limit: 2026-05-12 (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=2026-05-19&until=2026-05-19&set=physics&metadataPrefix=arXiv
Scoring abstracts
Number of records retrieved: 1190
Keyword score statistics
score 10 -- 2 abstracts
score 9 -- 1 abstracts
score 8 -- 1 abstracts
score 6 -- 1 abstracts
score 5 -- 10 abstracts
score 4 -- 10 abstracts
score 3 -- 10 abstracts
score 2 -- 37 abstracts
in total -- 72 abstracts
Articles that appeared on 2026-05-19
-
[abstract 1 / 72] Wow! (score: 10)
- Title: Exploring the Transitional Parameter Space of Blazars using Gamma-ray and X-ray Population DiagnosticsAuthors: Zahoor Malik, Sikandar Akbar, Zahir Shah,Comments: 11 pages, 8 figures, SubmittedSubjects: astro-ph.HECreated: 2026-05-17; Updated: 2026-05-19; Datestamp: 2026-05-19
We investigate the $γ$-ray and X-ray population properties of changing-look BLAZARs (CLBs) using sources from the Fourth \textit{FERMI} LAT Source Catalog Data Release 4 (4FGL-DR4) together with X-ray information from the Living \textit{SWIFT} XRT Point Source (LSXPS) catalog. The CLB sample is compared with large populations of confirmed BL Lac objects (BLLs) and flat-spectrum radio QUASARs (FSRQs) using spectral, variability, and broadband properties. In the $γ$-ray parameter space, CLBs mainly occupy intermediate and overlap regions between the BLL and FSRQ populations. However, the centroid locations in different parameter planes, along with the PCA and UMAP projections, show that the CLB population lies closer to the FSRQ region. The X-ray analysis also shows a similar behavior, where the overall distribution of CLBs in the X-ray parameter space is found to be nearer to FSRQs than to BLLs. In addition, the X-ray/$γ$-ray coupling relations and random-forest classification probabilities are consistent with this trend. Overall, the results suggest that CLBs form a transitional population between the two main BLAZAR subclasses while retaining characteristics closer to the FSRQ population.
[abstract 2 / 72] Wow! (score: 10) - Title: GRMHD Simulations of Magnetized Accretion Disk/Jet: Variabilities of Black Holes and Spectral Energy Distributions in Magnetic StatesAuthors: Rohan Raha, Banibrata Mukhopadhyay, Koushik Chatterjee,Comments: Published in Universe as an invited article to the Special Issue "Magnetized Dense Matter in Compact Stars: From Fundamental Properties to Astrophysical Observables", 30 pages, 8 Figures, 2 TablesSubjects: astro-ph.HECreated: 2026-05-17; Updated: 2026-05-19; Datestamp: 2026-05-19
We perform three-dimensional general RELATIVISTIC MAGNETohydrodynamic (GRMHD) simulations of a near-maximally spinning BLACK HOLE (spin parameter, a = 0.998) with varying initial MAGNETic field geometries, systematically exploring the parameter space connecting MAGNETically arrested disk (MAD), intermediate (INT), and standard and normal evolution (SANE) accretion states. The MAGNETic flux threading the BLACK HOLE horizon emerges as the fundamental state variable controlling JET efficiency, flow MAGNETization, and radiative output across all three states. We introduce complementary diagnostics-broadband spectral energy distributions spanning radio through hard X-ray frequencies and time-resolved X-ray light curves-that together connect simulation dynamics directly to multiwavelength observables. The radiative output follows a clear MAD > INT > SANE hierarchy in time-averaged luminosity, mean X-ray emission, as well as variability. Furthermore, MAD exhibits the highest fractional variability through quasi-periodic MAGNETic flux eruption events, and INT and SANE show moderate variability driven by episodic RECONNECTion and stochastic MRI turbulence, respectively. Scaling to GRS 1915+105, Cyg X-1, and HLX-1, we demonstrate that all twelve temporal classes of GRS 1915+105 map naturally onto our three MAGNETic states, Cyg X-1's persistent hard state is reproduced by a sustained INT configuration, and HLX-1's extreme luminosities arise through efficient Blandford-Znajek extraction in MAD states scaled to higher BLACK HOLE mass.
[abstract 3 / 72] Wow! (score: 9) - Title: A 14-year-old Mystery: The Peculiar Case of the Engine-driven SN 2012apAuthors: Itai Sfaradi, Raffaella Margutti, Ryan Chornock, A. J. Nayana, Eli Wiston, Fabio De Colle, Tracy E. Clarke, Wendy M. Peters, Paz Beniamini, Wenbin Lu, Rodolfo Barniol Duran, Michael Bietenholz, Collin T. Christy, Deanne L. Coppejans, Maria R. Drout, Dina Ibrahimzade, Michal J. Michalowski, Dan Milisavljevic, Conor M. B. Omand, Yihan Wang, Kate D. Alexander, Carles Badenes, Joe Bright, Jonathan Granot, Erica Hammerstein, Wynn V. Jacobson-Galan, Natalie LeBaron, Kohta Murase, Gitika Rameshan, Huei Sears, Michael Stroh, Giacomo Terreran,Comments: 24 pages, 8 figures, 5 tables; Submitted to ApJSubjects: astro-ph.HECreated: 2026-05-15; Updated: 2026-05-19; Datestamp: 2026-05-19
We present late-time ($δt > 3000$ d) optical (Keck), X-ray (Chandra and NUSTAR), and radio (VLA, ALMA, and the uGMRT) observations of the Type Ic-BL SN 2012ap. Previous studies of this SN suggested that it stands out as a key example of a weak engine-driven explosion due to the lack of GAMMA-RAY BURST detection and a mildly RELATIVISTIC ejecta. Recently, radio sky surveys revealed the rebrightening of the radio emission from this SN, highlighting the possibilities of a density enhancement at large radii or the existence of an off-axis RELATIVISTIC JET. While the late-time optical spectra does not exhibit the broad emission lines seen in other interacting SNe, our analysis of the broadband radio and X-ray emission implies that both scenarios are plausible. If a density enhancement is responsible for the radio rebrightening, it has to result from a change in the mass-loss rate and/or wind velocity, possibly due to the transition of the progenitor from a red supergiant to a Wolf-Rayet star. If the late-time radio component is a result of an off-axis RELATIVISTIC JET, we find that an energetic narrow JET viewed at $θ_{\rm obs} \geq 80^{\circ}$ is needed. In this scenario, SN 2012ap is not a result of a weak engine-driven explosion, and, instead, it is similar to other GRBs. However, radio rebrightenings of Type Ic-BL SNe are not enough on their own to determine the existence of off-axis JETs and our planned VLBA observation will help reveal the true nature of this SN.
[abstract 4 / 72] Wow! (score: 8) - Title: Constraining the MAGNETic field strength of a flaring radio core in the compact steep spectrum source 3C 138Authors: Shan Li, Sang-Sung Lee, Whee Yeon Cheong, Tao An, Seiji Kameno, Ruediger Kneissl,Comments: 10 pages, 7 figures. Accepted for publication in Astronomy & Astrophysics (A&A)Subjects: astro-ph.GA astro-ph.HECreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
Compact steep spectrum (CSS) sources generally show weak Doppler boosting, yet some exceptions show multi-year-scale radio flux variability and high-energy activity. Since 2022, the CSS QUASAR 3C 138 has been in a radio high state accompanied by multiple gamma-ray outbursts, offering unique opportunities to study changes in JET physical conditions. We estimated the SYNCHROTRON self-absorption (SSA) MAGNETic field ($B_{\rm SSA}$) in the SSA core of 3C 138 during its high state and compared it with the equipartition MAGNETic field ($B_{\rm eq}$) to assess the core field environment. Using extended Korean Very long-baseline interferometry Network (KVN) data at 22, 43, 86, and 129 GHz (2024-2025), we calibrated the visibilities and modeled resolved components with circular Gaussians. A single-zone SSA model fitted to the core spectrum provided the turnover frequency and peak flux density, from which we estimated the $B_{\rm SSA}$ and $B_{\rm eq}$. We used Very Large Array and Atacama Large Millimeter/submillimeter Array data to constrain the broadband spectra with the same model. The KVN SSA core shows a turnover at about 33 GHz and a peak flux of about 1.45 Jy. The inferred $B_{\rm SSA}$ is far below equipartition, with $B_{\rm SSA}/B_{\rm eq}\approx0.05$. The flux variability of 3C 138 is driven by a compact, particle-dominated core. Shock-driven particle injection in the inner JET could account for the core brightening and the production of X-ray/gamma-ray emissions through an inverse-Compton process without requiring extreme RELATIVISTIC beaming effects.
[abstract 5 / 72] Yes (score: 6) - Title: Jet-Structure Imprint on the Curvature Tail of Gamma-Ray Burst Prompt EmissionAuthors: Zhen-Yu Yan, Xiao-Hong Zhao, Hendrik J. van Eerten, Jun Yang, Jiang-Chuan Tuo, Shu-Xu Yi, Chen-Wei Wang, Wen-Jun Tan, Shao-Lin Xiong, Bin-Bin Zhang,Comments: Accepted for publication in ApJ; 14 pages, 5 figures and 3 tablesSubjects: astro-ph.HECreated: 2026-05-16; Updated: 2026-05-19; Datestamp: 2026-05-19
Even though the prompt emission of GAMMA-RAY BURSTs (GRBs) is highly beamed, high-latitude emission still produces a distinct light curve break after the intrinsic emission ceases and the edge of the JET comes into view. This curvature effect offers a direct probe of the JET structure during the prompt phase. To uncover the geometric structure of the GRB JET encoded in the prompt light-curve evolution, we develop a numerical model that calculates SYNCHROTRON light curves from structured JETs to interpret the observed break. We apply this model to the prompt emission of GRB 230307A, which displays a rare late-time break. Our analysis demonstrates that simple spherical outflow and top-hat JET models are inadequate to reproduce the light curve. Instead, the observations are best described by a power-law wing JET with a uniform core ($θ_{\rm core}=0.0147$ rad) and a surrounding power-law wing. Our results demonstrate that the break in late-time prompt emission can be a powerful diagnostic of GRB JET structure.
[abstract 6 / 72] Yes (score: 5) - Title: Method for testing diffusive shock acceleration and diffusion propagation of 1-100 TeV cosmic electrons with multiwavelength observations of the Geminga halo and pulsar wind nebulaAuthors: Weikang Gao, Li-Zhuo Bao, Kun Fang, En-sheng Chen, Siming Liu, HongBo Hu,Comments: 11 pages, 4 figures,Published in Phys. Rev. D 113, 103024. DOI: https://doi.org/10.1103/lyfj-dhlySubjects: astro-ph.HECreated: 2026-05-17; Updated: 2026-05-19; Datestamp: 2026-05-19
Diffusive shock acceleration and diffusion propagation are essential components of the standard COSMIC RAY model. These theories are based on extensive observations of high-energy solar processes, providing substantial direct evidence in the MeV energy range. Although the model is widely and successfully used to explain high-energy cosmic phenomena, direct validation has been elusive. The multi-wavelength spectra and angular profile measurements of the Geminga pulsar wind nebula and its pulsar halo, particularly the precise spectral observations by HAWC and LHAASO-KM2A in recent years, offer a rare opportunity to test these theories with COSMIC RAYs energies between 1 TeV and several hundred TeV. These observations are expected to elevate the direct testing of theoretical models from multi-MeV to sub-PeV energies. In this work, a method is developed to test the diffusive shock acceleration and diffusion propagation model between one and several hundred TeV energies through the latest spectral and morphological data of the Geminga region from HAWC and FERMI-LAT. Our results show that the theories of diffusive shock acceleration and diffusion propagation are consistent with experimental observations. However, the published morphological data adopted rather wide energy bins and currently do not allow a high precision test of the inferred energy dependent diffusion coefficient by observed energy spectra with DSA theory. It is anticipated that future HAWC and LHAASO-KM2A observations will yield higher-precision results, and the confirmation of a rapidly increasing diffusion coefficient above 100 TeV would serve as important evidence supporting the diffusive shock acceleration and diffusion propagation theory. Similar tests would be both important and valuable for other models.
[abstract 7 / 72] Yes (score: 5) - Title: The GRB Intrinsic Duration Distribution: Progenitor Insights Across Cosmic TimeAuthors: Nicole M. Lloyd-Ronning, Omer Bromberg, Tsvi Piran,Comments: accepted to ApJSubjects: astro-ph.HECreated: 2026-05-17; Updated: 2026-05-19; Datestamp: 2026-05-19
We present the distribution of the intrinsic duration of GAMMA-RAY BURSTs' prompt emission. This expands upon the analysis of Bromberg et al., 2012 and Bromberg et al. 2013 who showed evidence for collapsar progenitors based on the presence of a plateau in the distribution of $T_{90}$, the duration over which 90 % of the prompt emission is observed for any given detector. We confirm the presence of this plateau in the distribution of duration corrected for cosmological time dilation (what we call intrinsic duration, $T_{int}$), but shifted to smaller timescales by a factor of $1/(1+z_{\rm av}) \sim 1/3$, where $z_{\rm av}$ is the average GRB redshift. More significantly, we show this plateau is only present in the sample of GRBs with redshifts greater than $(1+z) \sim 2$, and does not appear in the duration distribution of lower redshift GRBs. This result aligns with suggestions that the low redshift population of GRBs has a significant contribution from non-collapsar progenitors (while the high redshift sample is dominated by collapsars). We also show the difference in this distribution between spectrally hard and soft GRBs, confirming that a plateau is only present for the soft subset of GRBs. However, when we separate the soft GRBs into low and high redshift subsets, we find that only the high redshift soft GRBs show evidence of a plateau, while the low-redshift soft GRBs do not. This suggests there exists a significant subset of spectrally soft non-collapsar progenitors at low redshift. Finally, we use the end time of the plateau to constrain the GRB progenitor density profile and radius, and show the maximum size of a collapsar is a few tenths of a solar radius.
[abstract 8 / 72] Yes (score: 5) - Title: Polarization Signatures of Inspiraling Hotspots around Kerr Black HolesAuthors: Pablo Ruales, Delilah E. A. Gates, Alejandro Cárdenas-Avendaño,Comments: 16 pages, 8 figures v2: Updated to match published versionSubjects: astro-ph.HE gr-qcCreated: 2026-05-16; Updated: 2026-05-19; Datestamp: 2026-05-19
Polarimetric interferometry is a powerful tool for probing both BLACK HOLE accretion physics and the background spacetime. Current models aimed at explaining the observed multiwavelength flares in Sgr A* often assume hotspots moving on geodesic, Keplerian orbits. In many scenarios, though, a hotspot may instead follow an inspiraling trajectory, potentially transitioning into a plunge toward the BLACK HOLE. In this work, we present a general framework to simulate the polarized emission from generic equatorial inspiraling hotspots in Kerr spacetime using a parametric four-velocity profile. This parametrization defines a continuous family of flows, ranging from Cunningham's disk model (fixed radius orbits outside the innermost stable circular orbit and plunging motion within the innermost stable circular orbit) to purely radial motion, thereby extending the standard assumptions. Within this framework, we show that inspiral motion produces a distinctive observational signature: a precessing, unwinding evolution of the polarimetric Stokes Q-U looping pattern, in sharp contrast with the closed Q-U loops associated with stable orbits at a fixed radius. We then explore how the morphology of these signatures depends on BLACK HOLE spin, observer inclination, and MAGNETic-field configuration. The presented model can be applied to current and near-future interferometric observations of linear POLARIZATION, offering a new avenue to probe the physics of matter spiraling inward and the RELATIVISTIC velocities of plunging plasma.
[abstract 9 / 72] Yes (score: 5) - Title: Variable ADAF disk as the origin of Changing-Look AGNAuthors: Chun Xu,Comments: Preprint. 8 pages, 1 figure. Two additional examples are added: GSN 069 with QPE and PG1211+143 with UFO/Fe linesSubjects: astro-ph.HECreated: 2026-05-16; Updated: 2026-05-19; Datestamp: 2026-05-19
We propose that changing-look AGN transitions arise from variations in the size of the inner ADAF disk. The AGN accretion disk consists of an outer thin disk and an inner thick ADAF component, whose size is intrinsically unstable and evolves over time. The size variations of the ADAF are governed by a parameter η, which represents the turbulence strength within the accretion flow. ηalso determines the accretion rate onto the central BLACK HOLE and controls JET formation and outflow rate, with the latter regulating the line-of-sight absorption. From the perspective of a variable ADAF, changing-state and changing-observation AGN are two sides of the same coin. We further discuss gigahertz-peaked and compact steep-spectrum radio sources as possible manifestations of intermediate-to-large scale ADAFs. Finally, we propose that AGN unification models should include both orientation and ADAF size as key parameters.
[abstract 10 / 72] Yes (score: 5) - Title: Multiwavelength Probes of Cosmic Ray Transport in Molecular Cloud StructuresAuthors: Hayden P. H. Ng, Ellis R. Owen, Naomi Tsuji, Szu-Ting Chen,Comments: 21 pages, 11 figures, 3 tables. Accepted for publication in PASJSubjects: astro-ph.HE astro-ph.GACreated: 2026-05-15; Updated: 2026-05-19; Datestamp: 2026-05-19
We investigate how COSMIC RAY (CR) transport in molecular clouds and their substructures can be probed using multi-wavelength observations. The detailed microphysics regulating the penetration and coupling of CRs in dense molecular structures is unsettled. Self-generated turbulence can produce scattering and diffusive transport, while ion-neutral damping in cold, dense gas promotes ballistic CR propagation. We construct a self-consistent framework for CR transport and interactions in MAGNETized molecular clouds, considering three limiting propagation scenarios: ballistic transport, diffusion, and a hybrid configuration with a diffusive envelope and quasi-ballistic core. By forward-modeling pion-decay $γ$-ray emissivities, CR-driven ionization-rate profiles, and electron SYNCHROTRON emission in the hard X-ray band, we connect GeV attenuation and propagation signatures to independent diagnostics of secondary production and CR penetration. As an illustrative example, we apply our framework to the Taurus molecular cloud complex and selected embedded clumps. We show that CR scattering may be substantially enhanced on clump scales, with inferred CR diffusion coefficients suppressed relative to canonical interstellar medium (ISM) values at GeV energies. In this interpretation, CRs are more closely coupled with dense gas in the ISM, and a diffusive envelope boosts the effective gas column density encountered by the CRs. This increases the hadronic interaction rate in the cloud. In turn, the secondary CR electron injection is also increased, and CR ionization rates are elevated at higher densities. We show that a hard X-ray SYNCHROTRON emission component is also generated, which may be detectable with near-future facilities. Finally, we discuss how future $γ$-ray, X-ray, and ionization constraints will provide firm tests of CR propagation theories in molecular cloud environments.
[abstract 11 / 72] Yes (score: 5) - Title: Bidirectional Plasma Jets Driven by Magnetic Reconnection: Observations by GST and SDOAuthors: Yangyu Liu, Jinhua Shen, Xu Yang, Shuai Gu, Jianping Li, Haisheng Ji,Comments: published in ApJSubjects: astro-ph.SRCreated: 2026-05-17; Updated: 2026-05-19; Datestamp: 2026-05-19
Using high-resolution photospheric and chromospheric observations taken by the Goode Solar Telescope (GST), we studied two groups of bidirectional plasma JETs occurring in active region NOAA 13110. Supplementary observations are also provided by Solar Dynamics Observatory's (SDO) Atmospheric Imaging Assembly (AIA) and Helioseismic and Magnetic Imager (HMI). From the photospheric observations and MAGNETograms, the two successive bidirectional plasma JETs were initially located in the vicinity of the polarity inversion lines and at the intersection of the umbra and penumbra of the sunspot, followed by MAGNETic flux emergence and cancellation. As the cool filamentary threads are continuously emerging from the lower chromosphere and interact with overlying horizontal MAGNETic loops, it leads to the bidirectional JETs, erupting outflow plasmoids, and heating coronal MAGNETic loops. We find that the bidirectional JETs extended from the central excitation location in opposite directions, at the speed of about dozens of km s$^{-1}$. For the first JET, the initial brightening first appears in 304 angstroms, about 30 s earlier than the H$α$ observations, indicating that MAGNETic RECONNECTion takes place in the transition region. While the initial RECONNECTion for the second JET occurs simultaneously in H$α$ and 304 angstroms, showing the recurrent eruptions. These observations confirm that the bidirectional plasma JETs can be generated by MAGNETic RECONNECTion between the rising filamentary threads or material and the overlying horizontal MAGNETic loops. Our results provide new insights into the generation of the bidirectional plasma JETs and RECONNECTion-based coronal heating.
[abstract 12 / 72] Yes (score: 5) - Title: Accretion geometry and spectral evolution in 1A 1118-61: a comparison of the 2009 and 2026 outburstsAuthors: Kinjal Roy, Aru Beri, Rahul Sharma, Phil Charles,Comments: 16 pages, 13 figures. Under review ApJSubjects: astro-ph.HECreated: 2026-05-17; Updated: 2026-05-19; Datestamp: 2026-05-19
We present a detailed spectro-temporal study of the Be X-ray binary pulsar $1A$ $1118-61$ during its brightest recorded outburst in 2026, using \textit{SWIFT} and \textit{NUSTAR} observations, and compare its properties with the 2009 outburst. Coherent pulsations at $\sim400$ s are detected throughout the outburst, with pulse profiles evolving strongly with energy and luminosity, indicating changes in emission geometry. A transient quasi-periodic oscillation (QPO) at $\sim$0.11 Hz is observed during the rising phase. The luminosity dependence of the QPO frequency during the current and previous outbursts suggests an origin associated with instabilities near the MAGNETospheric radius. The broadband spectra are well described by thermal Comptonization and show clear spectral hardening at higher luminosities. A cyclotron line is detected in the two \textit{NUSTAR} observations, with its energy remaining nearly constant despite a factor of $\sim25$ change in luminosity. Long-term monitoring reveals that the 2026 outburst is systematically harder and brighter, suggesting significant difference in the accretion structure and emission regions between the two outbursts.
[abstract 13 / 72] Yes (score: 5) - Title: Classification of IGR J20084+3221 as an Intermediate Polar using X-ray and Optical ObservationsAuthors: Julian Gerber, Jeremy Hare, John A. Tomsick, Daniel Stern, Aarran W. Shaw,Comments: 9 pages, 5 figures, submitted to MNRASSubjects: astro-ph.HECreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
IGR J20084+3221 is a previously unclassified Galactic source first detected by INTEGRAL. Chandra observations led to possible classifications of either a MAGNETic Cataclysmic Variable (mCV) or high mass X-ray binary (HMXB) based on the hardness of its spectrum. Here, we report follow-up observations taken by XMM-Newton, NUSTAR, and the Hale Telescope at Palomar Observatory. Based on these observations, we conclude that IGR J20084+3221 is most likely an Intermediate Polar (IP) type mCV. Timing analysis of the X-ray data found a significant peak period of $P=635.0\pm0.4$ s, which we interpret to be the spin period of the white dwarf (WD). The X-ray spectrum is well fit to an absorbed Bremsstrahlung model with components accounting for partial covering, reflection, and a fluorescent Fe-line, all typical for an IP. The optical spectrum shows clear emission lines, consistent with emission dominated by an accretion disk. We find counterparts to the source across the optical and infrared (IR) bands, and, despite uncertainties in the distance and extinction, we estimate that the source is too faint in the IR to be an HMXB. Given the evidence pointing towards an IP classification, we fit the X-ray spectrum to a post-shock region model where we find a WD mass of $M=1.09^{+0.12}_{-0.11}\mathrm{M}_{\odot}$, larger than the average mass for a WD in an mCV.
[abstract 14 / 72] Yes (score: 5) - Title: Search for the Highest-energy Quasiperiodic Oscillation in the Black Hole X-Ray Binary Candidate SWIFT J1727.8-1613Authors: Xiang Ma, Qing-Cang Shui, Ming-Yu Ge, Liang Zhang, Jin-Lu Qu, Shuang-Nan Zhang, Lian Tao, Li-Ming Song, Shu Zhang, Hua Feng, Yue Huang,Comments: 7 pages, 6 figures, Published in The Astrophysical Journal, 1002, 180 (2026)Subjects: astro-ph.HECreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
We report the first detection of a low-frequency quasiperiodic oscillation (QPO) extending above 250 keV in the BLACK HOLE X-ray binary candidate SWIFT J1727.8-1613 using Insight-HXMT observations during its 2023 outburst. SWIFT J1727.8-1613 is one of the brightest X-ray transients discovered and presents a valuable opportunity for studying high-energy properties of QPOs. Owing to the large effective area of Insight-HXMT in hard X-ray, our observations indicate a remarkably strong QPO signal in the power spectrum above 100 keV. We utilize advanced Hilbert-Huang transform techniques to analyze phase-folded light curves across a wide range of energy bands, observing significant QPOs from 100 to 300 keV in the NaI and CsI detectors, respectively. The detection of QPO profiles above 250 keV can achieve significance levels of ${\sim} 8.9σ$ for the NaI detector and ${\sim} 5.7σ$ for the CsI detector. Our results indicate a decrease in QPO fractional rms above 100 keV and an increased soft phase lag with energy, suggesting a geometric origin for the QPOs, likely linked to the precession of a small-scale JET.
[abstract 15 / 72] Yes (score: 5) - Title: Spectral energy-loss bump and $γ$-ray pulsar halosAuthors: Kun Fang,Comments: 10 pages, 7 figuresSubjects: astro-ph.HECreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
LHAASO J0248$+$6021, a possible $γ$-ray pulsar halo associated with PSR J0248$+$6021 (J0248), exhibits a highly curved spectrum as revealed by LHAASO and FERMI-LAT measurements. We propose a direct interpretation of this large curvature: the energy-loss bump in the parent electron spectrum has not yet significantly departed from the high-energy cutoff. This requires either that the ambient MAGNETic field strength $B$ around J0248 be lower than the typical value in the interstellar medium, or that the electron injection age be significantly shorter than the pulsar characteristic age. For the much older Geminga pulsar, the expected energy-loss bump in its $γ$-ray halo spectrum has shifted below $100\ \text{GeV}$, in excellent agreement with FERMI-LAT measurements. Thus, the broadband spectra of young and old pulsar halos find a unified interpretation in the picture of a time-dependent energy-loss bump. Meanwhile, the spectral measurements of LHAASO J0248$+$6021 only constrain the combination of $B$ and electron injection age. The uncertainty in $B$ leads to an order-of-magnitude variation in the fitted diffusion coefficient. Future X-ray observations are expected to break the degeneracies.
[abstract 16 / 72] Yes (score: 4) - Title: Chromosphere of the quiet sun: II. Atmospheric response to small-scale MAGNETic flux emergenceAuthors: Quentin Noraz, Mats Carlsson, Guillaume Aulanier,Comments: Under press for publication in Astronomy & Astrophysics. Summary shortened for Arxiv submissionSubjects: astro-ph.SRCreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
Coupling between the photosphere, chromosphere and corona in the quiet Sun (QS) is governed by a complex interplay between MAGNETic structuring, heating, mass loading, and radiative cooling. Constraining how this balance responds to variations in small-scale MAGNETic flux remains limited. We investigate how chromospheric heating and its thermodynamic coupling to higher atmospheric layers vary as a function of small-scale MAGNETic flux emergence. We performed a parametric set of 3D radiative-MHD simulations with the Bifrost code, starting from a weakly MAGNETised QS reference model and injecting horizontal MAGNETic flux of increasing amplitude into the sub-surface convection zone. The resulting chromospheric dynamics, heating, mass loading, and coronal response were analysed. Chromospheric temperatures and mechanical heating rise monotonically with increasing MAGNETic-field strength. Although the fractional contribution of shocks decreases, RECONNECTing current sheets keeps maintaining about 50%. In contrast, the temperature at the base of the corona exhibits a non-monotonic response, reaching a maximum at intermediate MAGNETic amplitudes and decreasing for the strongest-field case. We show that stronger MAGNETic-field strength increases chromospheric heating, which increases the coronal-base density through efficient mass loading, and amplifies radiative losses. These density-driven radiative losses dominate the coronal energy balance and thus lead to reduced coronal-base temperatures despite increased heating. Our results demonstrate the sensitivity of chromospheric structure and dynamics to small-scale flux emergence, and its key role in regulating coronal thermodynamics. This result illustrates the chromosphere-s role as a thermodynamic gatekeeper, and further warrants future investigations of atmospheric models relevant to global solar-wind models and space-weather forecasts.
[abstract 17 / 72] Yes (score: 4) - Title: Multiwavelength Analysis of PSR J0437-4715 with Pulse Profile ModelingAuthors: Liqiang Qi, Juan Zhang, Weiwei Xu, Shijie Zheng, Mingyu Ge, Ang Li, Shuang-Nan Zhang, Hua Feng, Fangjun Lu,Comments:Subjects: astro-ph.HECreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
We present a multi-wavelength analysis of the nearby millisecond pulsar PSR J0437--4715, combining Hubble Space Telescope (HST) far-ultraviolet, ROSAT soft X-ray, and XMM-Newton X-ray data, to model its broadband emission and energy-resolved pulse profiles, and infer key stellar parameters via Bayesian inference. The broadband emission includes cold thermal, hot thermal, and non-thermal components: cold bulk surface emission is modeled with a non-MAGNETized partially-ionized hydrogen atmosphere; hot-spot emission adopts the pulse profile modeling technique with a non-MAGNETized fully-ionized hydrogen atmosphere model; and non-thermal emission is included as a phase-invariant power-law component. By adopting an informative prior on the hot-spot geometry informed by radio POLARIZATION position angle measurements, the joint multi-instrument analysis yields a statistically viable and radio-consistent solution with a gravitational mass of 1.38$\pm$0.03~M$_\odot$ and an equatorial circumferential radius of 13.25$_{-0.35}^{+0.34}$~km (68\% confidence intervals). The hot-spot geometry consists of two spherical caps with uniform temperature distributions: the primary hot spot is situated at a colatitude of $\approx$130$^{\circ}$, and the secondary hot spot lies at a colatitude of $\approx$9$^{\circ}$, close to the north pole. It yields tighter radius constraints than HST+ROSAT fits and shifts the radius posterior distribution to larger values relative to NICER-only fits. This work demonstrates the importance of multi-wavelength data in refining neutron star mass-radius measurements and resolving geometric degeneracies.
[abstract 18 / 72] Yes (score: 4) - Title: XRISM detection of the 6.4 keV Fe K$α$ line in the RADIO GALAXy Cygnus AAuthors: Anwesh Majumder, T. Heckman, L. Gu, A. Simionescu, B. R. McNamara, A. Ptak, E. Hodges-Kluck, M. Yukita, M. W. Wise, N. Roy,Comments: 10 pages, 4 figures. Submitted in ApJSubjects: astro-ph.HE astro-ph.COCreated: 2026-05-16; Updated: 2026-05-19; Datestamp: 2026-05-19
We detail the spectral analysis of a 170 ks XRISM Resolve observation of the core of Cygnus A. The high spectral resolution of Resolve have enabled us to probe the inner accretion region of Cygnus A by analyzing the 6.4 keV Fe K$α$ line complex. We find that it consists of two Keplerian broadened components. (1) A broad component with a velocity dispersion of $3400^{+800}_{-600}$ km s$^{-1}$ and (2) a narrow component of $440^{+60}_{-50}$ km s$^{-1}$. For an inclination of $50^{\circ}-85^{\circ}$, constrained by VLBI, we find that the broad component arises from a distance of $\sim 0.1-0.17$ pc ($800-1400$ gravitational radii) and the narrow component from $\sim 6-10$ pc ($50,000-80,000$ gravitational radii) from the central BLACK HOLE depending on the inclination angle. Our result suggests that the origin of the broad component is consistent with the broad line region and the narrow component from the torus of Cygnus A. We also find a potential emission line possibly from intermediate ionized Fe XVII with a very low dispersion ($<80$ km s$^{-1}$) that originates from either the outer edge of the torus or the narrow line region. Finally, we find that the Fe K edge is redshifted compared to the Fe K$α$ line components, suggesting a line of sight bulk velocity of $470 \pm 100$ km s$^{-1}$. Such a shift may be due to an inflowing wind or relative motion between the two components originating from the near and far side of an inflowing torus, respectively.
[abstract 19 / 72] 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: 2026-05-16; Updated: 2026-05-19; Datestamp: 2026-05-19
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 two up to an order of magnitude.
[abstract 20 / 72] Yes (score: 4) - Title: Understanding corona and disk evolution in BLACK HOLE X-ray binaries through a comprehensive study of their broadband variability and QPO characteristicsAuthors: Biki Ram, Manoneeta Chakraborty,Comments: 16 pages, 17 Figures, Accepted for publication in MNRASSubjects: astro-ph.HECreated: 2026-05-17; Updated: 2026-05-19; Datestamp: 2026-05-19
The shape of the power spectrum of the BLACK HOLE low-mass X-ray binary evolves systematically over different spectral states during an outburst. Therefore, the power colours (ratio of the variability amplitude at different frequency ranges) and the hue parameter, quantifying the power spectral shape, can be utilised to identify the spectral states of the system. We present the comprehensive power colour analysis and subsequent identification of spectral states using the entire archival data (2016-2024) from AstroSat. We detected 29 QPOs (quasi-periodic oscillations), along with several associated harmonics and shoulders, and investigated their properties as a function of hue. We examined the evolution of the QPO RMS variability and time lag, along with hue and QPO frequency. We report a sign change in the average QPO time lag around the QPO frequency of ~2 Hz for high inclination sources, during the hard-to-hard intermediate state transition. At lower frequency, the hard lags showed an increasing trend reaching up to ~36 ms, but the soft lags above 2 Hz remained confined within ~10 ms, suggesting an evolution to a compact corona. Conversely, for low inclination sources, no such transition was found. Furthermore, for high inclination sources, the harmonic lag remains unaffected during state transition, in contrast to the QPO lag behaviour. Our results are consistent with a transition from an elongated JET-like corona to a compact corona and reveal vital clues about the dynamical evolution of the corona and disk.
[abstract 21 / 72] Yes (score: 4) - Title: Population synthesis of ACTIVE GALACTIC NUCLEi based on the radiation-regulated unification modelAuthors: D. Gerolymatou, S. Paltani, C. Ricci, T. T. Ananna,Comments: Submitted for publication in A&ASubjects: astro-ph.HE astro-ph.GACreated: 2026-05-17; Updated: 2026-05-19; Datestamp: 2026-05-19
X-ray surveys of ACTIVE GALACTIC NUCLEi (AGNs) provide direct constraints on the properties of individual AGNs, such as their emission, obscuration, and accretion rate. Previous AGN population synthesis models have not addressed such properties self-consistently. Here, we use a simulation-based inference (SBI) approach to constrain the geometrical and physical properties of the AGN population. We perform numerical simulations with our ray-tracing code, RefleX, which allows the self-consistent modelling of the X-ray emission of AGNs with flexible circumnuclear and source geometries. We create our synthetic population by sampling the intrinsic active BLACK HOLE mass function (BHMF) and Eddington ratio distribution function (ERDF) of local AGNs, and we construct a geometry based on the radiation-regulated model, along with Eddington-ratio-dependent emission spectra. Using the RefleX-simulated emission of the AGN population, we aim to simultaneously reproduce the cosmic X-ray background (CXB), differential AGN number counts, and several observed absorption properties of local AGNs, such as the fraction of $N_\mathrm{H}$ in bins of log($N_\mathrm{H}$), the Compton-thick fraction as a function of limiting flux, and the number of obscured and unobscured AGNs as a function of Eddington ratio. With this approach, we test the consistency of the radiation-regulated model with a very comprehensive set of X-ray observables, while constraining the size and density of the dusty torus and the evolution of the local AGN population. We derive an intrinsic Compton-thick fraction of $40\pm3$%, and find that a simple evolutionary prescription controlling the active fraction of supermassive BLACK HOLEs is sufficient for our synthetic population to reproduce the CXB.
[abstract 22 / 72] Yes (score: 4) - Title: Nuclear Activity and Host Galaxy Properties of Low-Luminosity AGN Identified from VLA ObservationsAuthors: M. N. Rosli, A. Annuar,Comments: 20 pages, 7 figuresSubjects: astro-ph.GA astro-ph.HECreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
Low-luminosity ACTIVE GALACTIC NUCLEi (LLAGN; $L_{\rm bol} < 10^{42}$~erg~s$^{-1}$) may comprise a significant fraction of the local AGN population, yet their weak emission makes them difficult to detect. In this paper, we analyse 38 LLAGN identified from a 15~GHz sub-arcsecond Very Large Array survey and assess the effectiveness of X-ray, optical, and infrared wavelengths in identifying LLAGN. We found that optical emission-line diagnostics recovered $84.2^{+15.8}_{-22.9}$\% (32/38) of the sample, X-rays detected $63.2^{+25.7}_{-19.6}$\% (24/38), and infrared methods only identified $13.2^{+14.5}_{-8.0}$\% (5/38), reflecting limited X-ray sensitivity, weak or absent optical lines, and strong host galaxy contamination in the infrared. Compared to \textit{SWIFT}--BAT AGN, our LLAGN are $\sim$ 4.1~dex fainter in bolometric luminosity (log $L_{\mathrm{bol}} \approx$ 39.3 - 41.9 erg s$^{-1}$), host smaller BLACK HOLEs ($\sim$0.7~dex lower), and accrete at much lower rates (log $λ_{\text{Edd}} \approx$ -6.5 to -1.3, i.e., $\sim$ 4.2~dex lower). Host galaxies span a broad range of morphologies, from disk- to bulge-dominated, with a subset exhibiting prominent bulges, potentially representing systems where nuclear activity has faded while the bulge remains dominant. LLAGN also reside in galaxies with lower stellar masses ($\sim$0.3~dex) and suppressed STAR FORMATION rates ($\sim$0.5~dex) relative to \textit{SWIFT}--BAT AGN. Overall, LLAGN in our sample systematically host smaller and weakly accreting BLACK HOLEs, residing in galaxies with diverse morphologies, but lower stellar masses and reduced STAR FORMATION activity, demonstrating the connection between low-level BLACK HOLE accretion and host galaxy properties in the local Universe.
[abstract 23 / 72] Yes (score: 4) - Title: Two kinds of Galactic source populations could explain the cosmic-ray observation up to the "knee" regionAuthors: Furong Li, Wei Liu, Yali Shao, Yi-Qing Guo,Comments: 14 pages, 10 figures, Accepted for publication in ApJSubjects: astro-ph.HECreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
Observations of diffuse gamma rays above hundreds of TeV from the Galactic disk provide strong evidence for the existence of PeV cosmic-ray accelerators--so-called PeVatrons--in the Galaxy. However, mounting observations have ruled out most SUPERNOVA remnants as likely PeVatron candidates, suggesting instead that multiple populations of cosmic-ray sources exist in the Galaxy. Recently, the LHAASO collaboration reported the detection of ultra-high-energy gamma rays from microQUASARs, establishing that the BLACK HOLEs in these systems, which accrete matter from companion stars, are powerful PeV particle accelerators. In this work, we propose a two-component source model to explain the observed cosmic-ray spectra and composition up to the PeV range. Below approximately 100 TeV, SUPERNOVA remnants serve as the dominant sources; above this energy, microQUASARs are considered the primary candidate population. Within this scenario, the assumption of a charge-dependent cutoff well accounts for the latest measurements, including the proton and helium spectra up to the PeV range, the energy-dependent composition, and the all-particle spectrum. In contrast, the nuclei-dependent cutoff hypothesis is ruled out by the data.
[abstract 24 / 72] Yes (score: 4) - Title: A 4200-hour HyperFlash and ÉCLAT campaign on the hyperactive FRB 20240114A: constraining energetics with the most brilliant burstsAuthors: O. S. Ould-Boukattine, A. J. Cooper, A. M. Cook, J. W. T. Hessels, D. M. Hewitt, J. Huang, I. Cognard, T. J. Dijkema, M. P. Gawroński, W. Herrmann, F. Kirsten, A. Moroianu, Z. Pleunis, W. Puchalska, S. Ranguin, M. P. Snelders, T. Telkamp,Comments: Submitted to MNRAS. Comments welcomeSubjects: astro-ph.HECreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
Hyperactive repeaters provide a unique window into the evolving environments and energy budgets of fast radio burst (FRB) sources, though they may not be representative of the FRB population in general. High-cadence observations are key to capturing the rarest and most energetic bursts, which occur only once per hundreds to thousands of hours. Here we present an unprecedented $4{,}200$-hour observing campaign targeting FRB 20240114A as part of the HyperFlash and ÉCLAT FRB monitoring programs. Over $806$ days, we detected $178$ high-energy ($\sim$$10^{40-42}$ erg) bursts with HyperFlash, which together amount to $4.4 \times 10^{42}$ erg of released radio energy (assuming isotropic emission and 1-GHz emission bandwidth). The cumulative energy of the HyperFlash bursts is about twice that of $\sim$$11{,}000$ lower-energy bursts detected with FAST, emphasising the significant role that the highest-energy bursts play in depleting the central engine's stored energy. In fact, the single most brilliant burst from our sample, which we term the STROOP, contributes roughly $1/3$ of all the energy we measure, and is at the maximum energy seen in studies of both repeating and apparently one-off FRBs alike. We also find a break in the burst energy distribution at $\sim$$2\times10^{40}$ erg and a linear dispersion measure (DM) increase of $+0.96 \pm 0.06$ pc cm$^{-3}$ over a period of $318$ days. We discuss these findings in the context of a MAGNETar source model and highlight comparisons with the energetics of intermediate and giant X-ray/$γ$-ray flares from Galactic sources.
[abstract 25 / 72] Yes (score: 4) - Title: Pulse profile modelling of the 2024 outburst of the accreting millisecond pulsar SRGA J144459.2-604207Authors: Bas Dorsman, Tuomo Salmi, Anna L. Watts, Mason Ng, Anna Bobrikova, Alessandro Di Marco, Duncan K. Galloway, Sebastien Guillot, Mariska Hoogkamer, Yves Kini, Fabio La Monaca, Vladislav Loktev, Matteo Lucchini, Christian Malacaria, Ying-Han Mao, Alessandro Papitto, Juri Poutanen,Comments: Submitted to MNRAS. A full reproduction/results package will be made available via Zenodo repository (link in paper) following reviewSubjects: astro-ph.HE astro-ph.SRCreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
Pulse profile modelling via RELATIVISTIC ray-tracing can constrain the system parameters of neutron stars, notably their mass and radius. Among these objects, accreting millisecond pulsars (AMPs) are promising targets, because they are bright in X-rays and their potentially polarized radiation can lead to complementary constraints on the emission geometry. We perform combined analysis of NICER and IXPE observations of the recently discovered the 448-Hz pulsar SRGA J144459.2-604207, with IXPE providing X-ray POLARIZATION information. NICER and IXPE jointly favour a large mass and radius for our best-fitting model, for which the neutron star has two independent hotspots. The primary hotspot is centered near the northern rotational pole, the secondary in the southern hemisphere, and the observer inclination is in the range 50-75 degrees. The primary hotspot is large (up to half the surface area) and contributes the majority of the non-pulsed X-rays, while the secondary is hotter and the major contributor to the overall pulse profile shape. However, many parameters are inferred to be near the prior bounds, which could indicate that the model does not adequately account for important physics. Furthermore, we tested several different methodologies for joint analysis of the two data sets: the results are sensitive to the method used, something that merits further study with synthetic data. In the future, we expect simultaneously recorded data will lead to improved parameter constraints, especially when multi-band and polarized data are combined.
[abstract 26 / 72] (score: 3) - Title: Observation of a cross-section enhancement near the $t\bar{t}$ production threshold in $\sqrt{s}=13$ TeV $pp$ collisions with the ATLAS detectorAuthors: ATLAS Collaboration,Comments: 64 pages in total, author list starting page 47, 12 figures, 4 tables, published at Reports on Progress in Physics. All figures including auxiliary figures are available atSubjects: hep-exCreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
A measurement of $t\bar{t}$ production is presented in the invariant-mass region near the pair production threshold, $m_{t\bar{t}} \sim 345$ GeV, in final states with two charged leptons and multiple JETs. The measurement is based on $140\,\mathrm{fb}^{-1}$ of proton-proton collision data collected at $\sqrt{s} = 13$ TeV with the ATLAS detector at the Large Hadron Collider. The data are compared to two models of $t\bar{t}$ production: a baseline model including only perturbative QCD predictions for the hard process at approximate next-to-next-to leading order accuracy in the strong coupling, and an extended model that, in addition, incorporates non-RELATIVISTIC QCD simulations that also include the formation of colour-singlet quasi-bound-states near the $t\bar{t}$ threshold. The agreement between the data and the models is quantified via a profile-likelihood fit to the reconstructed $m_{t\bar{t}}$ distributions, in bins of two angular observables sensitive to spin-correlations in the $t\bar{t}$ system. An excess of events is observed over the baseline perturbative QCD prediction, with an observed significance over $8$ standard deviations. This excess is consistent with the formation of colour-singlet and spin-singlet $S$-wave quasi-bound $t\bar{t}$ states, as predicted by non-RELATIVISTIC QCD, and corresponds to an observed cross-section of $9.3^{+1.4}_{-1.3}$ pb.
[abstract 27 / 72] (score: 3) - Title: Halo-driven Origin and Suppression of Over-massive Black Holes and Little Red DotsAuthors: Ritik Sharma, Mahavir Sharma,Comments: 9 pages, 5 figures, submitted, comments welcomeSubjects: astro-ph.GA astro-ph.CO astro-ph.HECreated: 2026-05-15; Updated: 2026-05-19; Datestamp: 2026-05-19
We present a theoretical model in which the recently detected over-massive BLACK HOLEs (OBHs), and possibly Little Red Dots (LRDs), arise during a halo-driven transient phase preceding the established coevolution of supermassive BLACK HOLEs (SMBHs) and their host galaxies. In this model, halo gravity drives an early phase of rapid BLACK HOLE growth, leading to systems in high-redshift haloes that lie above the local scaling relations. As the halo evolves, a transition in halo thermodynamics leads to the onset of a hot, pressure-supported medium that suppresses accretion, reducing the BLACK HOLE growth rate and driving the system toward the local BLACK HOLE mass$-$stellar mass relation. LRDs may represent an observational manifestation of the rapid, halo-driven growth phase, while OBHs trace its direct mass signature. Our model thus provides a unified framework in which these systems form and evolve toward the regulated coevolution observed in the local Universe.
[abstract 28 / 72] (score: 3) - Title: FIRM3D: Fast ion reduced models in 3DAuthors: Elizabeth Paul, Alexey Knyazev, Michael Czekanski, Alexandra Lachmann, Abdullah Hyder, Christopher Albert, Matt Landreman,Comments:Subjects: physics.plasm-phCreated: 2026-05-16; Updated: 2026-05-19; Datestamp: 2026-05-19
The dynamics of energetic particle (EP) species, born from fusion reactions or plasma heating schemes, are critical for predicting the behavior of MAGNETic confinement fusion experiments and future fusion reactors. Because energetic particles are largely collisionless, the orbits of Monte Carlo samples drawn from a given distribution function can be efficiently integrated in prescribed electroMAGNETic fields. In addition to the static MAGNETo-hydrodynamic (MHD) equilibrium fields produced by the electroMAGNETic coils of a fusion device, MHD waves can be excited by -- and resonantly transport -- energetic particle populations. FIRM3D is an open-source Python/C++/CUDA software suite for modeling energetic particle dynamics in 3D MAGNETic fields, available at https://github.com/ColumbiaStellaratorTheory/firm3d. The core guiding-center integration routines grew out of SIMSOPT (Landreman et al., 2021), but have been extended to include additional physics and diagnostics not typically required in the stellarator optimization context. This standalone framework enables focused development of energetic particle physics capabilities with minimal dependencies, making it accessible to the broader stellarator and plasma physics community. Components of FIRM3D include interfaces with MHD equilibrium and wave stability software (BOOZ_XFORM, AE3D, FAR3D); CPU and GPU parallelized integration of the guiding center orbit equation, with symplectic and Runge-Kutta integrator options; and orbit visualization and transport diagnostics, including Poincare maps, orbit classification, and weighted Birkhoff averaging.
[abstract 29 / 72] (score: 3) - Title: Simulation study of the COSMIC RAY Sun shadow with a time-dependent solar MAGNETic field modelAuthors: Jie Xia, Ming-Yang Cui, Qiang Yuan, Yi Zhang, Guang-Lu Shi, Li Feng,Comments: 9 pages, 6+2 figure, 2 tables; accepted for publication in Physical Review DSubjects: astro-ph.HE astro-ph.SR physics.space-phCreated: 2026-05-16; Updated: 2026-05-19; Datestamp: 2026-05-19
During the propagation of COSMIC RAYs in the solar system, the Sun will block those particles and form a shadow whose position and depth are very important probe of the MAGNETic fields in the Sun's corona, in the interplanetary space, and the Earth's vicinity. In this work we carry out Monte Carlo studies of the Sun shadow, with a novel approach to take into account daily variations of the coronal and interplanetary MAGNETic field models. This treatment is suitable for studies of short-term variations of the Sun shadow, which become detectable by the Large High Altitude Air Shower Observatory (LHAASO) experiment. Two different coronal MAGNETic field models, the Potential Field Source Surface (PFSS) and Current Sheet Source Surface (CSSS) models, with observational time-varying photospheric MAGNETic fields as boundary conditions, are studied in this work. The interplanetary MAGNETic fields are then derived using the Parker spiral model based on the coronal ones. Furthermore, both the coronal and interplanetary MAGNETic field strengths are corrected using the Parker Solar Probe (PSP) measurements. We compare the simulation results with the daily observations of Sun shadow by LHAASO in 2021, and find that the CSSS model generally shows better consistency of the displacement of the Sun shadow than the PFSS model.
[abstract 30 / 72] (score: 3) - Title: Magnetised CGM Gas at z~1 revealed by SPICE-RACSAuthors: Sunil Malik, S. P. O'Sullivan, A. J. M. Thomson, C. S. Anderson, C. Van Eck, L. Rudnick, Amit Seta, B. M. Gaensler, Y. K. Ma, Takuya Akahori, D. Alonso-López, M. Brüggen, E. Carretti, S. W. Duchesne, T. J. Galvin, G. Heald, O. Hlinka, A. Khadir, S. A. Mao, R. Omae,Comments: 9 pages, 13 figures, Accepted for publication in A&A LettersSubjects: astro-ph.GA astro-ph.COCreated: 2026-05-16; Updated: 2026-05-19; Datestamp: 2026-05-19
Magnetic fields are expected to permeate the circumgalactic medium (CGM) of galaxies, yet direct constraints at high redshift remain limited by the lack of high-quality Faraday rotation measure (RM) data. Using the RMs from SPICE-RACS DR2 combined with the DESI DR1 QUASAR catalogue, we compile the largest sample to date of 2483 QUASAR sightlines with associated RMs, including 612 with intervening Mg II absorbers tracing foreground galaxies and 1871 control sightlines without Mg II absorbers. After subtracting the Galactic RM contribution and restricting the analysis to sightlines with low Milky Way HI column density and H$α$ intensity, we obtain a foreground-cleaned sample of 757 QUASARs (191 Mg II / 566 control) spanning redshifts $0.13
[abstract 31 / 72] (score: 3) - Title: Shafranov shift and finite $β$ effects on Alfvén Eigenmodes and microinstabilities in global electroMAGNETic gyrokinetic simulationsAuthors: B. Rofman, G. Di Giannatale, A. Mishchenko, E. Lanti, A. Bottino, T. Hayward-Schneider, J. N. Sama, A. Biancalani, B. F. McMillan, S. Brunner, L. Villard,Comments:Subjects: physics.plasm-phCreated: 2026-05-16; Updated: 2026-05-19; Datestamp: 2026-05-19
Future nuclear fusion reactors will have to confine plasma with strong kinetic gradients and small fractions of fusion-born energetic particles (EP) that are ~100 times hotter than the thermal ions. In our analysis, we assume the existence of a stable MHD equilibrium and study the unstable plasma perturbations. In this electroMAGNETic, kinetic, multi-scale, self-organizing system, all species contribute both to the Shafranov shift (equilibrium effect) and to the plasma $β$ (plasma response). Nonetheless, due to the high complexity of the problem, many works neglect these effects. We use the global, gyrokinetic code ORB5 to study the plasma stability. Starting from an electrostatic, thermal plasma with adiabatic electrons in a $β= 0$ ideal-MHD equilibrium, we systematically increase the realism of our models. And study the linear stability and nonlinear fluxes of Toroidal Alfvén Eigenmodes (TAE), and the Ion Temperature Gradient (ITG), and Kinetic Ballooning Modes (KBM) microinstabilities as they arise. Linearly, we find that Shafranov shift effects are a function of the toroidal mode number, that they are mainly stabilizing, and stronger at longer wavelengths, impacting TAEs the most with a 90% reduction in growth rate for cases which consistently account for the EP pressure in the MHD equilibrium. Leading to a law of diminishing returns for the TAE growth rate as a function of EP fraction. We find that with Shafranov shift asymptotically pushes the ITG frequency up and the TAE frequency down. Furthermore, we show that KBMs are strongly damped by both EPs (kinetic) and Shafranov shift (equilibrium) effects. Nonlinearly we find that the linear TAE stabilization does not effect the saturation levels. Nonetheless, the heat and particle fluxes carried by the TAE, are reduced by the Shafranov shift. While, the ITG fluxes and saturation levels are unaffected by the Shafranov shift.
[abstract 32 / 72] (score: 3) - Title: Radio Emission from Fast Blue Optical Transients Powered by Trans-RELATIVISTIC Shocks in Confined Circumstellar MaterialAuthors: Liang-Duan Liu, Jia-Sen Zhang, Zhao-Sheng Zhang, Yun-Wei Yu,Comments: 13 pages, 8 figures, 2 tablesSubjects: astro-ph.HECreated: 2026-05-17; Updated: 2026-05-19; Datestamp: 2026-05-19
Fast blue optical transients (FBOTs) are luminous, rapidly evolving explosions whose radio emission provides a sensitive probe of shock interaction and the circumstellar material (CSM) surrounding the progenitor. However, the origin of their diverse radio light-curve morphologies, especially the very steep post-peak declines seen in several well-sampled events, remains unclear. We present a forward-shock SYNCHROTRON model in which mildly RELATIVISTIC ejecta interact with a dense but radially confined CSM. The CSM is described by a broken power-law density profile, and the radio emission is modeled by including both SYNCHROTRON self-absorption and external free-free absorption. Applying this framework to multi-frequency radio observations of a representative sample of FBOTs, we show that their radio diversity can be explained by shock propagation through a finite CSM shell. The early radio evolution is regulated by absorption, while the rapid post-peak fading marks the forward shock's transition from the dense inner CSM into a more tenuous outer environment. The inferred shock velocities are trans-RELATIVISTIC, $v_{\rm sh}\sim0.1$--$0.5c$. The radio-emitting CSM requires high mass-loading rates, $\dot{M}\sim10^{-4}$--$10^{-3}\,M_{\odot}\,{\rm yr}^{-1}$, but modest total CSM masses, $M_{\rm CSM}\sim10^{-4}$--$10^{-2}\,M_{\odot}$. These properties point to brief episodes of enhanced mass loss in the final years to decades before explosion, rather than long-lived steady winds. Our results provide a dynamically consistent interpretation of FBOT radio emission and establish radio light curves as a diagnostic of the immediate pre-explosion mass-loss history of FBOT progenitors.
[abstract 33 / 72] (score: 3) - Title: Anisotropic Ejecta from Binary Neutron Star Mergers: Self-Consistent Main Thermal and Late-Time Radio Emission of NS-Powered KilonovaeAuthors: Jia-Xiang Chen, Shao-Ze Li,Comments: 12 pages, 8 figures, accepted for publication in ApJSubjects: astro-ph.HECreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
The interaction between the fast-moving ejecta and the interstellar medium can produce long-lasting radio signals after binary neutron star mergers. Searching for such radio signals is a way to test the central engine of kilonovae and short GAMMA-RAY BURSTs. With a MAGNETar as the central engine, the spin-down energy powers the main thermal and late-time radio emissions of the kilonova. However, both the thermal and radio emissions are strongly affected by the ejecta distribution, e.g., the two-component ``blue" and ``red" emissions of AT 2017gfo corresponding to the GW 170817 event. In this study, we investigate the distribution of the merger ejecta, analyzing several possible anisotropic distributions and demonstrating their impacts on the emission properties, particularly the late-time radio light curves. Under a bipolar and equatorial ejecta configuration, corresponding to the wind and dynamical components of the merger ejecta, the late-time radio light curves reveal distinct two-peak features, which are consistent with the main thermal light curves. The anisotropic distribution of the ejecta intrinsically connects the main thermal and late-time radio emissions, forming a self-consistent evolutionary picture. A combined analysis of the main thermal and late-time radio emissions provides a way to constrain the geometry of the merger ejecta and to probe the properties of the central engine. Furthermore, using the fitting parameters from the main thermal emission of AT 2017gfo, we calculate the corresponding potential late-time radio light curves. The results show that, under typical parameters, the non-detection of radio signals in observations is consistent with the theoretical expectation.
[abstract 34 / 72] (score: 3) - Title: SDSS-V: Revealing a weak accretion state in X-ray selected red QUASARsAuthors: Paloma Guetzoyan, James Aird, Amy L. Rankine, Stephanie M. LaMassa, Peter Breiding, Mara Salvato, Johannes Buchner, Zsofi Igo, Roberto J. Assef, Hector Ibarra-Medel, Catarina Aydar, Castalia Alenka Negrete, Claudio Ricci, W. N. Brandt, Dong-Woo Kim, Dominika Wylezalek, Scott F. Anderson, Donald P. Schneider, Delvin Demke, Anton M. Koekemoer,Comments: Submitted to MNRASSubjects: astro-ph.GACreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
Red QUASARs (rQSOs) have been recognized as a short-lived, early stage in the evolutionary cycle of Active Galactic Nuclei (AGN), with fundamental differences in their intrinsic properties compared to blue QUASARs (bQSOs). In this work, we present the first large X-ray sample of 380 rQSOs, selected from the eROSITA/SDSS-V collaboration, providing uniform X-ray detection with optical spectroscopy accros half the sky, in the German hemisphere of eROSITA. We combine X-ray imaging, optical spectroscopy, and multi-wavelength photometry to fully probe the accretion, absorption and host properties of rQSOs. Independent Component Analysis is used to reconstruct optical spectra in a data-driven and non-parametric approach, while accounting for dust reddening and host contamination. rQSOs are intrinsically X-ray weak compared to bQSOs, with a higher fraction found at low X-ray luminosities (over 50$\%$ of the rQSO sample have $L_X < 10^{43.5} \, \rm erg \, s^{-1}$). We investigate the relative X-ray strength of rQSOs by measuring the spectral slope indicator $α_{OX}$. Despite their suppressed X-ray emission, rQSOs are not optically faint, but show low $α_{OX}$ values, indicating weak X-ray emission relative to their bright optical continua. X-ray spectral measurements reveal large gas column densities relative to optical reddening due to dust, implying that X-ray absorption could arise from dust-free gas close to the supermassive Black Hole (BH) rather than a classical dusty torus, while the dust responsible for optical reddening likely resides on larger host-galaxy scales or is associated with dusty gas carried in disc winds. rQSOs trace a phase of suppressed BH assembly relative to stellar mass growth, suggesting that they represent a distinct evolutionary stage where BH accretion is suppressed while the host galaxy continues to grow.
[abstract 35 / 72] (score: 3) - Title: Spatiotemporal representation of a two-vortex RECONNECTion as a single rotating vortexAuthors: Jordan M. Adams,Comments:Subjects: physics.opticsCreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
Reconnections and rotations of lines are dual descriptions of the same saddle-shaped spacetime surface. We show that a RECONNECTion between two line occurring over time is a single line that rotates over space progression. Both rotating lines and RECONNECTions possess the same saddle shape sheet geometry in four-dimensional space-time, with different orientations. Cyclic precessing lines occurring over time are arrays of RECONNECTions occurring spatially. We show that a MAGNETic RECONNECTion occurring over time can be seen as a single continuous line vector potential rotating spatially, where the full evolution traces a saddle shape surface. Finally, we show that a single tilted spatiotemporal optical vortex precesses with spatial progression, and as a result can be seen as two vortices RECONNECTing. Given the unique spatiotemporal evolution, we also analyzed the RELATIVISTIC angular momentum of these electroMAGNETic fields.
[abstract 36 / 72] (score: 2) - Title: Modelling DSA, FAST and CRAFT surveys in a z-DM analysis and constraining a minimum FRB energyAuthors: Jordan Hoffmann, Clancy W. James, Marcin Glowacki, Jason X. Prochaska, Alexa C. Gordon, Adam T. Deller, Ryan M. Shannon, Stuart D. Ryder,Comments: 17 pages, 7 figures, submitted to PASASubjects: astro-ph.CO astro-ph.HECreated: 2026-05-16; Updated: 2026-05-19; Datestamp: 2026-05-19
Fast radio burst (FRB) science primarily revolves around two facets: the origin of these bursts and their use in cosmological studies. This work follows from previous redshift-dispersion measure ($z$-DM) analyses in which we model instrumental biases and simultaneously fit population parameters and cosmological parameters to the observed population of FRBs. This sheds light on both the progenitors of FRBs and cosmological questions. Previously, we have completed similar analyses with data from the Australian Square Kilometer Array Pathfinder (ASKAP) and the Murriyang (Parkes) Multibeam system. With this manuscript, we additionally incorporate data from the Deep Synoptic Array (DSA) and the Five-hundred-meter Aperture Spherical Telescope (FAST), invoke a Markov chain Monte Carlo (MCMC) sampler and implement uncertainty in the Galactic DM contributions. The latter leads to larger uncertainties in derived model parameters than previous estimates despite the additional data. We provide refined constraints on FRB population parameters and derive a new constraint on the minimum FRB energy of log$\,E_{\mathrm{min}}$(erg)=39.49$^{+0.39}_{-1.48}$ which is significantly higher than bursts detected from strong repeaters. This result may indicate a low-energy turnover in the luminosity function or may suggest that strong repeaters have a different luminosity function to single bursts. We also predict that FAST will detect 25-41% of their FRBs at $z \gtrsim 2$ and DSA will detect 2-12% of their FRBs at $z \gtrsim 1$.
[abstract 37 / 72] (score: 2) - Title: Constraints on primordial non-Gaussianity from QuaiaAuthors: Giulio Fabbian, David Alonso, Kate Storey-Fisher, Thomas Cornish,Comments: Matches version published in JCAP. Material relevant for this analysis is available at https://github.com/gfabbian/quaia-fnlSubjects: astro-ph.CO gr-qcCreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
We analyse the large-scale angular clustering of QUASARs in the \gaia-\unwise QUASAR catalog, \quaia, and their cross-correlation with maps of the lensing convergence of the Cosmic Microwave Background (CMB), to constrain the level of primordial non-Gaussianity (PNG). Specifically, we target the scale-dependent bias that would be induced by PNG on biased tracers of the matter inhomogeneities on large scales. The \quaia sample is particularly well suited for this analysis, given the large effective volume covered, and our ability to map out the main potential sources of systematic contamination and mitigate their impact. Using the universality relation to characterise the response of the QUASAR overdensity to PNG ($p_ϕ=1$), we report constraints on the local-type PNG parameter $f_{\rm NL}$ of $f_{\rm NL} =-20.5^{+19.0}_{-18.1}$ (68\% C.L.) by combining the QUASAR auto-correlation and its cross-correlation with CMB lensing in two tomographic redshift bins (or $f_{\rm NL} =-28.7^{+26.1}_{-24.6}$ if assuming a lower response for QUASARs, $p_ϕ=1.6$). The error on $f_{\rm NL}$ can be further improved if the cross-correlation between the tomographic redshift bins is included. Using the CMB lensing cross-correlations alone, we find $f_{\rm NL} =-13.8^{+26.7}_{-25.0}$ and $f_{\rm NL} = -15.6^{+42.3}_{-34.8}$ for $p_ϕ=1$ and $p_ϕ=1.6$ respectively. These are the tightest constraints on $f_{\rm NL}$ to date from angular clustering statistics and cross-correlations with CMB lensing.
[abstract 38 / 72] (score: 2) - Title: Non-Gaussianity in SMICAAuthors: M. Citran, H. V. Tran, G. Patanchon, B. van Tent,Comments: 35 pages, 14 figures. v2: Corrected mistake in and extended analysis of section 6.4 (figure 10), conclusions unchanged v3: Corrected affiliation of one author v4: Version as published on JCAP, added DOISubjects: astro-ph.COCreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
We develop a new formalism for the component separation method Spectral Matching Independent Component Analysis (SMICA) in order to include the information contained in the foregrounds beyond second-order statistics. We also develop a binned bispectrum estimator that works directly using maps of different frequency channels, capable of determining the bispectrum of multiple components at the same time, shifting the traditional approach to non-Gaussianity estimation from a cleaned map to the component separation step, for a better handling of foreground uncertainty. We test our method on 400 E and B POLARIZATION simulations based on the LiteBIRD experiment, containing the two main sources of contamination for CMB POLARIZATION experiments: polarized dust and SYNCHROTRON emission. We show that the bispectrum does not improve the precision of the power spectrum estimation or of the spectral parameters. However, we are capable of recovering the correct 3-point correlator of the foregrounds and standard constraints on primordial non-Gaussianity in a coherent multi-frequency and multi-component framework. The advantage of our approach is that it combines data in an optimal way accounting for the power spectrum and the bispectrum of the various components, which is not true for the standard approach.
[abstract 39 / 72] (score: 2) - Title: Measurements of QUASAR proximity zones with the Ly$α$ forest of DESI Y1 QUASARsAuthors: Ryuichiro Hada, Paul Martini, David H. Weinberg, Zheng Zheng, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. Cuceu, A. de la Macorra, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, G. Gutierrez, J. Guy, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, R. Joyce, D. Kirkby, T. Kisner, A. Kremin, C. Lamman, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, A. Muñoz-Gutiérrez, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, I. Pérez-Ràfols, G. Rossi, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou,Comments: 22 pages, 7 figures, 1 table; accepted for publication in ApJSubjects: astro-ph.GA astro-ph.COCreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
The intergalactic medium (IGM) around QUASARs is shaped by their dense environments and by their excess ionizing radiation, forming a "QUASAR proximity zone" whose size and anisotropy depend on the QUASAR's halo mass, luminosity, age, and radiation geometry. Using over 10,000 QUASAR pairs from the Dark Energy Spectroscopic Instrument (DESI) Year 1 data, with projected comoving separations $r_{\perp} < 2\,h^{-1}{\rm Mpc}$, we investigate how the proximity zone of foreground QUASARs at $z\sim2{\rm-}3.5$ affects Lyman-alpha absorption in their background QUASARs. The large DESI sample enables unprecedented precision in measuring this "transverse proximity" effect, allowing a detailed investigation of the signal's dependence on the projected separation of QUASAR pairs and the luminosity of the foreground QUASAR. We find that enhanced gas clustering near QUASARs dominates over their ionizing effect, leading to stronger absorption on neighboring sightlines. Under the assumption that QUASAR ionizing luminosity is isotropic and steady, we infer the IGM overdensity profile in the vicinity of QUASARs, finding overdensities as high as $Δ\sim 10$ at comoving distance $\sim 1\,h^{-1}{\rm Mpc}$ from the most luminous systems. Surprisingly, however, we find no significant dependence of the proximity profile on the luminosity of the foreground QUASAR. This lack of luminosity dependence could reflect a cancellation between higher ionizing flux and higher gas overdensity, or it could indicate that QUASAR emission is highly time variable or anisotropic, so that the observed luminosity does not trace the ionizing flux on nearby sightlines.
[abstract 40 / 72] (score: 2) - Title: Convolutional causal learning for aerodynamic flowsAuthors: Ryo Koshikawa, Ryo Araki, Qiong Liu, Kai Fukami,Comments: To appear in Journal of Fluid MechanicsSubjects: physics.flu-dyn physics.comp-phCreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
This study aims to capture aerodynamic causality from snapshot data with a time-varying mode decomposition technique referred to as information-theoretic machine learning. The current approach extracts time-dependent informative vortical structures, contributing to the future evolution of the aerodynamic coefficients. The present decomposition is employed with a convolutional neural network, enabling the identification of the spatial continuous mode. In addition, a low-order representation, characterizing the informative vortical structures and their corresponding aerodynamic coefficients, can also be identified by considering autoencoder-based data compression. The present technique is applied to a range of aerodynamic examples, including extreme vortex-gust airfoil interactions, experimentally measured transverse JET-wing interaction, and a turbulent separated wake across different Reynolds numbers. For the cases of gust-wing interaction, the time-varying gust effect on the lift response is extracted in an interpretable manner. With the example of a turbulent wake, the relationship between large-scale vortical motion and lift force is identified without any spatial length-scale information. The proposed approach could serve as a foundation for data-driven causal modeling and control for a range of unsteady flows.
[abstract 41 / 72] (score: 2) - Title: Is the overconcentration of pristine populations in Galactic globular clusters real? An N-body approach to the problemAuthors: P. Berczik, O. Sobodar, F. Flammini Dotti, M. Sobolenko, M. Ishchenko, R. Spurzem, M. Giersz, A. Askar,Comments: 6 pages, 5 figures, submitted to the A&A LetterSubjects: astro-ph.GACreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
Recent observations indicate that in some Milky Way globular clusters (GCs) pristine red giant branch (RGB) stars appear more centrally concentrated than enriched ones. This contradicts most multiple stellar population (MSP) formation scenarios, which predict that the enriched (second) population (2P) should initially be more concentrated than the pristine (first) population (1P). Previous MOCCA Monte Carlo simulations suggested that this apparent overconcentration is a transient effect arising in clusters that have lost a large fraction of their initial mass and host an active BLACK HOLE subsystem (BHS), and is visible only when RGB stars are used as tracers. In this letter, we test this interpretation using tailored NBODY6++GPU models evolved with direct N-body simulations, providing an independent validation that does not rely on a statistical treatment of relaxation. We performed direct N-body simulations with the NBODY6++GPU code, adopting initial conditions designed to reproduce the dynamical regime relevant to the proposed mechanism. The simulations include updated stellar and binary evolution, dynamical interactions, and the Galactic tidal field, enabling a direct comparison with MOCCA results. The simulations confirm that the spatial distributions and kinematics inferred from RGB stars can be strongly affected by stochastic fluctuations and interactions with the BHS. Preferential ejection of 2P RGB and their progenitors from the cluster center leads to a transient apparent overconcentration of 1P RGB stars, in agreement with earlier MOCCA predictions.
[abstract 42 / 72] (score: 2) - Title: Propagation effects of Lorentz violation in gravitational wavesAuthors: A. A. Araújo Filho, N. Heidari, Iarley P. Lobo,Comments: 33 pages and 5 figures -- version accepted for publication in EPJCSubjects: gr-qc hep-thCreated: 2026-05-16; Updated: 2026-05-19; Datestamp: 2026-05-19
We investigate the propagation of gravitational waves in the presence of Lorentz- and diffeomorphism-violating operators within the linearized gravitational sector of the Standard Model Extension. Focusing on isotropic contributions, we analyze the combined effects of the CPT-even dimension-four coefficient $\mathring{k}^{(4)}_{(I)}$ and the CPT-odd dimension-five coefficient $\mathring{k}^{(5)}_{(V)}$ on tensorial gravitational radiation. The modified dispersion relation induces both a rescaling of the propagation speed and helicity-dependent corrections, leading to birefringence and POLARIZATION mixing without introducing additional propagating degrees of freedom. We derive the retarded Green function associated with the modified wave operator and obtain explicit expressions for the gravitational waveform generated by matter sources. As an application, we examine a binary BLACK HOLE system and show how Lorentz violation alters the observed strain through shifted retarded times, amplitude rescaling, and higher derivative corrections to the quadrupole formula. Using GW170817/GRB 170817A, published GWTC-3 propagation tests, and conservative POLARIZATION consistency arguments, we translate existing observational constraints into bounds on $\mathring{k}^{(4)}_{(I)}$ and $\mathring{k}^{(5)}_{(V)}$.
[abstract 43 / 72] (score: 2) - Title: Photon Sphere for a Dilatonic Dyonic Black Hole in a Model with an Abelian Gauge Field and a Scalar FieldAuthors: V. D. Ivashchuk, U. S. Kayumov, A. N. Malybayev, G. S. Nurbakova,Comments: 10 pages, LaTeX, 1 figure, 1 table (a few typos in the References have been eliminated; the notation for the polynomial in (4.16) is changed)Subjects: gr-qcCreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
Dilatonic dyon BLACK HOLE solution with gravitational radius $2 μ$ and two charges $Q_1$ and $Q_2$ (electric and MAGNETic ones) in the gravitational $4d$ model with one scalar field and one 2-form is considered. Dilatonic coupling constant $λ$ obeys $λ^2 = \frac{1}{2}$. The circular orbits for null geodesics are explored. The 3rd order polynomial master equation for radius $R_0$ of photon sphere is studied. It has only one solution which obeys $R_0 > 2 μ$. The circular null geodesics are shown to be unstable. The BLACK HOLE shadow is studied and relations for shadow angle and critical impact parameter are obtained.
[abstract 44 / 72] (score: 2) - Title: Exploring the link between coil non-planarity and MAGNETic surface geometry across a dataset of QI stellaratorsAuthors: Andrea Pavone, Sehyun Kwak, Felix Warmer,Comments:Subjects: physics.plasm-phCreated: 2026-05-17; Updated: 2026-05-19; Datestamp: 2026-05-19
Stellarator fusion devices confine plasma by means of complex, non-planar electroMAGNETic coils. Understanding how the shape of the plasma boundary determines the required complexity of the coil set is a central open question in stellarator design, with direct implications for engineering feasibility and the prospects of building next-generation fusion power plants. In this work we address this question using a large data-driven study. Starting from the Constellaration dataset of quasi-isodynamic (QI) stellarator plasma boundaries, we compute a set of filamentary coil configurations using constrained optimisation within SIMSOPT, and define quantitative coil-complexity metrics (torsion, SVD non-planarity score, inboard-side inclination angle, spectral width) together with a rich set of surface and MAGNETic geometry features (second fundamental form, principal-direction rotation rate, surface curvatures, and MAGNETic axis properties). Univariate and multivariate statistical analyses, reveal a strong, central role of the surface geometry: the principal-direction rotation rate of the plasma boundary is the single best predictor of coil non-planarity, while a Random Forest model using up to four surface features achieves R2 = 0.882 for the same target. These results provide quantitative evidence that the rate of change of the principal curvatures cross the plasma boundary are the primary drivers of coil non-planarity in this dataset of quasi-isodynamic stellarators.
[abstract 45 / 72] (score: 2) - Title: Ellipsoidal modulation and multi-wavelength activity in the pre-cataclysmic binary RX J1553.0+4457Authors: S. -Y. Wu, M. Gritsevich, Q. -H. Lao, A. J. Castro-Tirado, Z. Li, Y. -D. Hu, I. Pérez-García, R. Sánchez-Ramírez, N. Castro-Segura, E. J. Fernández-García, M. D. Caballero-García, S. Guziy, I. Olivares, J. D. Sakowska, G. García-Segura, D. Hiriart, W. H. Lee, P. J. Meintjes, H. J. van Heerden, A. Martín-Carrillo, L. Hanlon, A. Maury, L. Hernández-García, I. M. Carrasco-García, S. Castillo-Carrión, A. Castellón, S. B. Pandey, C. J. Pérez del Pulgar, A. J. Reina, J. -M. Bai, Y. -F. Fan, C. -J. Wang, Y. -X. Xin, D. -R. Xiong, X. -H. Zhao, J. Mao, B. -L. Lun, K. Ye, C. -Z. Cui, A. F. Valeev, B. -B. Zhang, T. -R. Sun,Comments: 16 pages, 10 figures, 6 tables. Updated title, author list, abstract, and minor textual revisionsSubjects: astro-ph.SR astro-ph.HECreated: 2026-05-17; Updated: 2026-05-19; Datestamp: 2026-05-19
RX J1553.0+4457 (TMTS J15530469+4457458) is a detached post-common-envelope binary containing a cool white dwarf and an active late-type companion. We present a multi-wavelength study combining BOOTES multi-band photometry, six sectors of public TESS full-frame imaging, Einstein Probe/FXT X-ray observations, CAFOS optical spectroscopy, and archival ultraviolet-to-mid-infrared photometry. The BOOTES data reveal two short optical flares separated by about 3 h, with amplitudes of roughly 1-1.5 mag and faster decay at shorter wavelengths. The combined TESS light curve shows a stable signal at P = 0.083782 d, consistent with the first harmonic of the known spectroscopic orbital period, and its folded morphology indicates ellipsoidal modulation from a tidally distorted late-type companion rather than an irradiation-dominated waveform. TESS flare energetics lie in the active M-dwarf regime. The Einstein Probe/FXT spectra show a factor of about 4 decline in the 0.3-10 keV flux, mainly associated with decreasing emission measures. The broadband SED is reproduced by a cool white dwarf plus a late-type M dwarf, with no clear hot-continuum or mid-infrared excess. RX J1553.0+4457 is therefore best interpreted as a detached pre-cataclysmic binary whose rapid optical variability is dominated by MAGNETic activity and whose orbital modulation is ellipsoidal, although a weak wind-fed or intermittent accretion contribution remains possible.
[abstract 46 / 72] (score: 2) - Title: Generic Peculiar Motions in FLRW SpacetimesAuthors: Bahram Mashhoon,Comments: 25 pages; v2: presentation improvedSubjects: gr-qcCreated: 2026-05-16; Updated: 2026-05-19; Datestamp: 2026-05-19
In the standard Friedmann-Lemaître-Robertson-Walker (FLRW) spacetime, we consider a local cosmic test mass that is boosted in some direction relative to the standard comoving observers. The geodesic (FERMI) normal coordinate system established around the world line of the boosted cosmic mass is constructed within an approximation scheme and the resulting spacetime metric is compared with the corresponding metric of the FERMI system established around the world line of a comoving observer. The circular gravitoMAGNETic field around the direction of motion of the boosted cosmic mass is studied.
[abstract 47 / 72] (score: 2) - Title: Polarization Birefringence and Waveform Systematics in GW231123Authors: Tonghua Liu, Chenggang Shao, Kai Liao,Comments: 9 pages, 4 figures, comments are welcomeSubjects: astro-ph.HECreated: 2026-05-14; Updated: 2026-05-19; Datestamp: 2026-05-19
GW231123 is a short, massive binary-black-hole event whose source properties show strong waveform dependence. We use this event to test gravitational-wave POLARIZATION birefringence, modeled as a frequency-dependent rotation of the tensor-POLARIZATION basis. Instead of sampling a distance-normalized coefficient directly, we sample the band-differential rotation $δ_{\rm br}=Δ(448\,\mathrm{Hz})-Δ(20\,\mathrm{Hz})$ with prior $[-π,π]$, and report the derived coefficient $β_{\rm br}^{\rm derived}$ for comparison with standard propagation parametrizations. We analyze three waveform families: IMRPhenomXPHM (XPHM), IMRPhenomXO4a (XO4a), and NRSur7dq4. The derived posteriors are consistent with the general relativity value, giving $90\%$ upper limits $|β_{\rm br}^{\rm derived}|_{90}=0.378,\,0.097,\,0.273$ for XPHM, XO4a, and NRSur7dq4, respectively. The directly sampled $δ_{\rm br}$ posterior remains broad, with $|δ_{\rm br}|_{90}\simeq2.8\,\mathrm{rad}$, so the accumulated rotation across the analysis band is weakly constrained. The Bayes factors are waveform dependent: $\ln\mathcal{B}_{\rm br/GR}=-1.26\pm0.30$, $+3.64\pm0.28$, and $-0.86\pm0.29$, respectively. We therefore find no waveform-robust evidence for parity-violating propagation. The positive XO4a result is better interpreted as a waveform-dependent birefringence-like response associated with the mass-ratio--distance--spin degeneracy of this short high-mass event.
[abstract 48 / 72] (score: 2) - Title: Particle Dynamics, Shadow and Hawking Sparsity of a Kalb-Ramond Black Hole Coupled to Nonlinear ElectrodynamicsAuthors: Faizuddin Ahmed, Ahmad Al-Badawi, İzzet Sakallı,Comments: 12 pages. Comments are welcomeSubjects: gr-qc astro-ph.HE hep-thCreated: 2026-05-15; Updated: 2026-05-19; Datestamp: 2026-05-19
We study the timelike and null geodesic structure of a static, spherically symmetric BLACK HOLE sourced by a Kalb--Ramond (KR) field coupled to nonlinear electrodynamics (NED). The geometry is characterized by the mass $M$, the MAGNETic monopole charge $q$, and the Lorentz-violating parameters $(γ,λ)$. Closed-form expressions are derived for the effective potential, as well as the specific energy and angular momentum of massive particles on circular orbits. We further analyze the photon sphere, BLACK HOLE shadow, and the Lyapunov exponent associated with unstable null circular geodesics. The latter determines the eikonal quasinormal-mode frequencies through $ω_{\rm eik}=(\ell+1/2)\,Ω_c-i(n+1/2)\,|λ_L|$. The shadow radius is compared with the Event Horizon Telescope (EHT) observations of M87$^\ast$ and Sgr~A$^\ast$, allowing us to identify the viable region in the $(q,γ)$ parameter space. Finally, we compute the Hawking temperature, horizon area, and the Gray--Visser sparsity parameter. We demonstrate that the combined effects of the KR field and MAGNETic monopole charge increase the sparsity parameter from the Schwarzschild value $16π^3 \simeq 496$ to nearly $1.7\times10^3$. This indicates a significantly sparser Hawking cascade compared to the Schwarzschild case, while the photon ring remains consistent with the EHT $1σ$ observational bounds across most of the physically allowed parameter range.
[abstract 49 / 72] (score: 2) - Title: The limits of feedback from ACTIVE GALACTIC NUCLEiAuthors: Andrew Pontzen, Hiranya V. Peiris, Joop Schaye, Matthieu Schaller,Comments: 17 pages, 8 figures. Companion letter (Peiris et al.) in this listingSubjects: astro-ph.GA astro-ph.COCreated: 2026-05-15; Updated: 2026-05-19; Datestamp: 2026-05-19
We use FLAMINGO to investigate why feedback from ACTIVE GALACTIC NUCLEi (AGN) significantly depletes gas in galaxy groups but is ineffective in clusters. We delineate three radial zones: an inner zone where AGN feedback heats halo gas via shocks; an intermediate buoyancy zone where the heated halo gas rises; and an outer zone where the outflow may stall in a termination shock. Heating in the inner zone self-limits because, once the gas is sufficiently hot, shocks become too weak to deposit further entropy. Consequently, outflows have a ceiling entropy value ($360\, {\rm keV\, cm^2}$) that is nearly independent of halo mass. These values (and trends with redshift and feedback variants) are explained using an argument based on the Rankine-Hugoniot relations. Outflows rise at fixed entropy through the buoyancy zone, escaping the halo if the ceiling value is sufficiently elevated over that of the inflowing gas. This condition is satisfied only for halo masses $M_{\rm 200m}<10^{13.7}\,{\rm M_\odot}$, because inflow entropy tracks the virial relation. Variants with stronger (or weaker) feedback have a higher (or lower) entropy ceiling and a correspondingly modified critical mass of $M_{\rm 200m}=10^{14.0}\,{\rm M_\odot}$ (or $10^{13.5}\,{\rm M_\odot}$). In clusters above the critical mass, the increased inflow entropy causes the outflow to stall and potentially shock at the 'splashback' radius. We derive an expression for the time evolution of the virial gas fraction, which shows how lingering gas is reincorporated as the halo virial radius expands. This effect dominates over outflows unless they rejoin the Hubble flow; as a result, virial gas fractions rise as a function of mass starting at $M_{\rm 200m} = 10^{13.0}\,{\rm M_\odot}$. These effects explain why groups have depleted gas, while clusters have close to the cosmic baryon fraction.
[abstract 50 / 72] (score: 2) - Title: Thermostats, Not Engines: A New Picture of Halo Gas RegulationAuthors: Hiranya V. Peiris, Andrew Pontzen, Madalina N. Tudorache, Anik Halder, Stephen Thorp, Sinan Deger, Joop Schaye, Matthieu Schaller,Comments: 7 pages, 3 figures, 1 table. Comments welcome. Companion paper Pontzen et al. in this arxiv listingSubjects: astro-ph.CO astro-ph.GACreated: 2026-05-15; Updated: 2026-05-19; Datestamp: 2026-05-19
We propose that BLACK HOLE feedback regulates gas in massive halos by establishing an entropy ceiling; the resulting buoyant gas migrates to the virial radius with no additional energy input required. The FLAMINGO simulations support this picture: at the virial radius, outflow entropy is mass-independent for isotropic thermal feedback but depends on the solid angle of directly heated gas for JET feedback. Above a critical halo mass $M_\rm{crit} \approx 10^{13.5\text{--}14}\, M_\odot$, virial shocks overwhelm the ceiling, predicting rejuvenation of STAR FORMATION in the most massive galaxies, supported by new low-redshift evidence from STAR FORMATION rates and morphologies.
[abstract 51 / 72] (score: 2) - Title: Searching for the Third Wheel: High-Contrast Imaging Constraints on Tertiaries to Black Hole and Neutron Star BinariesAuthors: Pranav Nagarajan, Kareem El-Badry, Aniket Sanghi,Comments: 20 pages, 12 figures, Submitted to PASPSubjects: astro-ph.SR astro-ph.HECreated: 2026-05-15; Updated: 2026-05-19; Datestamp: 2026-05-19
Hierarchical triple evolution provides a promising alternative to isolated binary formation models for BLACK HOLEs (BHs) and neutron stars (NSs) with low-mass stellar companions. To search for tertiaries, we perform deep, adaptive optics-assisted, near-infrared imaging of five quiescent BH low-mass X-ray binaries (LMXBs), Gaia BH1, and twelve Gaia NSs. We detect several faint stars previously unresolved in survey imaging, but none are close enough to robustly rule out a chance alignment. To achieve high contrast sensitivity at close separations, we use the reference star differential imaging strategy with the Karhunen-Loéve Image Processing algorithm to model and subtract the point-spread function of each target. We identify tertiary candidates in the speckle-dominated regime, but injection-recovery tests suggest most 5$σ$ detections are likely artifacts. We derive $5σ$ contrast curves and convert these to limits on the mass of main sequence (MS) tertiaries and the effective temperature of white dwarf (WD) tertiaries consistent with a non-detection. We rule out plausible MS tertiaries and young, hot WD tertiaries at projected separations $\gtrsim 500$ au for the Gaia compact object binaries and $\gtrsim 2000$ au for the more distant BH LMXBs. While the recent discovery of a $1.2\,M_{\odot}$ tertiary to V404 Cygni supports triple formation scenarios for BH LMXBs, our results suggest such companions are relatively rare. Our observations remain consistent with intermediate-mass tertiaries that have since evolved into cool WDs, detectable with deeper JWST imaging. Follow-up observations are required to measure proper motions and confirm or rule out physical association of tertiary candidates.
[abstract 52 / 72] (score: 2) - Title: Rapidly Rotating Neutron Star Collapse in Massive Scalar-Tensor TheoriesAuthors: José Carlos Olvera M., Daniela D. Doneva, Pablo Cerdá-Durán, José A. Font, Stoytcho S. Yazadjiev,Comments: 25 pages, 20 figuresSubjects: gr-qc astro-ph.HECreated: 2026-05-15; Updated: 2026-05-19; Datestamp: 2026-05-19
We present a full 3D numerical evolution code to study neutron stars in massive-scalar-tensor theories. The code is embedded in the Einstein Toolkit framework and its implementation constitutes a modified version of the Baumgarte-Shapiro-Shibata-Nakamura formalism with an additional nonminimally coupled scalar field. The approach we follow preserves the standard hydrodynamic evolution for matter fields, allowing eventually for a straightforward inclusion of more microphysical effects and better flexibility. Using this code, we examine the gravitational collapse of rapidly rotating, scalarized neutron stars to a BLACK HOLE by exploring the influence of the scalar field on the dynamical features of the process and on the gravitational-wave emission. We find that for the configurations studied in this work, there is an observational degeneracy in the tensorial gravitational-wave emission between collapsing scalarized stars and their counterparts in general relativity. However, this degeneracy can be broken through the emission of scalar radiation, which carries an energy of ~10^-3 M_sun c^2. This is orders of magnitude higher than the quadrupolar emission (~10^-7 M_sun c^2) and might be used as an observational probe of modified gravity. We also find that rapid rotation can enhance this signal, since fast rotating stars can sustain larger scalar field amplitudes.
[abstract 53 / 72] (score: 2) - Title: The Torques Acting on Accreting Millisecond X-Ray Pulsars in the Outburst and Quiescent States, and During the Long-Term EvolutionAuthors: Fatmanur Ertugrul, Ali Arda Gencali, Unal Ertan, Ndiogou Niang,Comments: 10 pages, 6 figures, accepted for publication in MNRASSubjects: astro-ph.HECreated: 2026-05-15; Updated: 2026-05-19; Datestamp: 2026-05-19
Accreting millisecond X-ray pulsars (AMXPs) are transient X-ray sources likely to be in the final evolutionary phases of low-mass X-ray binaries (LMXBs). In this work, we have investigated the torque and X-ray luminosity variations of five AMXPs during outburst and quiescence, using a model previously employed to explain some typical behaviours of LMXBs. Most of these systems spin up in the outburst state and spin down in quiescence, while they slow down on the long term. We have obtained reasonable results with the model in agreement with these observations. We have found that the torques produced by the disc-MAGNETosphere interaction, the MAGNETic dipole radiation, and the mass accretion are compatible with the X-ray luminosity and rotational properties of the sources in their outburst and quiescent states, and during the resultant long-term evolution. Nevertheless, our results are not sufficient to rule out the spin-down contribution of the gravitational radiation torques due to significant timing noise and uncertainties about the bolometric corrections for X-ray luminosity during the outbursts of some sources.
[abstract 54 / 72] (score: 2) - Title: A Rare Population of Intermediate-mass Helium Stars Between Hot Subdwarfs and Wolf-Rayet StarsAuthors: Gui-Yu Wang, Yong Shao, Jian-Guo He, Yu-Dong Nie, Xiao-Jie Xu, Xiang-Dong Li,Comments: 18 pages, 15 figures, accepted by ApJSubjects: astro-ph.SR astro-ph.HECreated: 2026-05-16; Updated: 2026-05-19; Datestamp: 2026-05-19
Helium stars stripped of their hydrogen envelopes represent pivotal phases in binary evolution, yet their origins, particularly within the intermediate-mass range of $2-8\, M_{\odot}$, still remain poorly understood. This population bridges the gap between low-mass hot subdwarfs and massive Wolf-Rayet stars, but has remained largely unobserved. In this study, we employ binary population synthesis to systematically investigate the formation and properties of intermediate-mass helium stars (IMHeS) across various galactic metallicities. Our results indicate that metallicity and common-envelope ejection efficiency are the dominant factors shaping the IMHeS population. We estimate that several thousand IMHeS exist in the Milky Way, with several hundred more in the Magellanic Clouds. The vast majority of IMHeS reside in binaries, with fewer than $10\%$ appearing as single stars. Among IMHeS binaries, $\gtrsim 50\%$ are expected to have main-sequence companions, and the remainder host compact companions (including helium stars, white dwarfs, neutron stars, or BLACK HOLEs). The former systems form mainly through stable mass transfer, whereas the latter arise predominantly from common envelope evolution. Our work provides quantitative predictions for the populations of these elusive stars formed through binary interactions and offers guidance for future observational searches.
[abstract 55 / 72] (score: 2) - Title: Static electroMAGNETic Love tensors of 5-dimensional Myers-Perry BLACK HOLEsAuthors: Boyang Yu,Comments: 24 pagesSubjects: hep-th gr-qcCreated: 2026-05-16; Updated: 2026-05-19; Datestamp: 2026-05-19
We study the separable master equations for the electroMAGNETic and gravitational perturbations in five-dimensional Myers-Perry BLACK HOLEs. In the static limit, while the master equation for the electric POLARIZATION of the Maxwell field reduces to that of a massless scalar field, the MAGNETic POLARIZATION and gravitational perturbation yield Heun equations for both its angular and radial components. Remarkably, these Heun equations fall into a special class that admits exact analytic solutions in terms of hypergeometric functions. We reconstruct the gauge field using master fields and study its asymptotic behavior. When expanding the result in the basis of modified spherical harmonics, we find modes with higher angular momentum arise in response to the excitation of sources with lower angular momentum. The static tidal Love tensor that characterizes such mixing structure of the response can be computed iteratively. We also discuss the possible near zone approximation of the master equations for the MAGNETic POLARIZATION.
[abstract 56 / 72] (score: 2) - Title: Nonlinear electrodynamics in MAGNETars: systematic effects on radius constraints and timing analysisAuthors: Gabriel A. Porto, Jonas P. Pereira, Eduardo Bittencourt, Elda Guzmán-Herrera,Comments: 13 pages, 1 tableSubjects: astro-ph.HE gr-qcCreated: 2026-05-16; Updated: 2026-05-19; Datestamp: 2026-05-19
Magnetars are among the most extreme laboratories in the universe, harboring surface MAGNETic fields reaching $10^{15}$~G. At these supercritical scales, Maxwell's linear electrodynamics is superseded by Nonlinear Electrodynamics (NLED). While vacuum birefringence has provided initial observational evidence for these effects, its broader impact on photon propagation remains largely unexplored. In this work, we demonstrate that NLED significantly alters photon propagation in the vicinity of MAGNETars, deviating light from standard null-geodesics. We estimate that neglecting these corrections leads to relative errors in inferred stellar radii by means of ray-tracing techniques of approximately $10\%$. Furthermore, we find that NLED induces a systematic minimal travel-time delay of approximately $350~n$s, a value that already far exceeds the $100$~ns temporal resolution of missions like NICER. These results are critical for the interpretation of X-ray pulse profiles from current and future observatories, such as eXTP, which rely on high-precision light-bending and timing models to determine neutron-star masses and radii. Finally, our results underscore the role of MAGNETars as a vital window into the physics of superdense matter and supercritical fields, and we briefly highlight other astrophysical observables--such as glitches and antiglitches--that may be affected by NLED.
[abstract 57 / 72] (score: 2) - Title: Elastic wave propagation governs impulse enhancement in pulsed JETs through flexible nozzlesAuthors: Paras Singh, Daehyun Choi, Saad Bhamla, Chandan Bose,Comments:Subjects: physics.flu-dynCreated: 2026-05-17; Updated: 2026-05-19; Datestamp: 2026-05-19
Inspired by cephalopod JET propulsion through compliant funnels, this study investigates elastic wave propagation and energy exchange in passively deforming cylindrical nozzles through three-dimensional, two-way fluid-structure interaction simulations. Flexible nozzles with varying stiffness ($Eh = 75 - 500~\mathrm{N\,m^{-1}}$, where $E$ and $h$ are Young's modulus and nozzle thickness, respectively) are subjected to a pulsatile JET inflow at $Re \sim 4000$. Increasing nozzle flexibility reduces the deformation-wave speed in accordance with Moens-Korteweg scaling, thereby prolonging the nozzle expansion phase. This delayed expansion enhances JET entrainment and elastic energy storage while suppressing early shear-layer roll-up and vortex formation. During contraction, the stored elastic energy is released, thereby enhancing JET acceleration and vortex formation. For the most flexible nozzle, the primary vortex-ring circulation increases by 52.13%, the vortex convection distance by 9.00%, and the peak outlet kinetic energy flux by a factor of 4.62 compared with a rigid nozzle. These effects collectively yield a 61.92% increase in total hydrodynamic impulse. These findings identify passive wave-speed tuning via nozzle compliance as a mechanism to enhance pulsed-JET thrust for bio-inspired underwater propulsion.
[abstract 58 / 72] (score: 2) - Title: Role of Magnetic Field in the Redistribution of Turbulence from Large-Scale Structures to Small-Scale FluctuationsAuthors: Tanmay Karmakar, Rosh Roy, Lavkesh Lachhvani, Raju Daniel, Bhoomi Khodiyar, Prabal K. Chattopadhyay, Abhijit Sen, Sayak Bose,Comments:Subjects: physics.plasm-phCreated: 2026-05-17; Updated: 2026-05-19; Datestamp: 2026-05-19
Magnetized plasmas with equilibrium density gradients support drift-wave turbulence, which is often regulated by self-generated zonal flows. In this work, we experimentally examine the effect of increasing the MAGNETic field on turbulence characteristics in a linear plasma device. As the MAGNETic field is increased from 600 to 1000 G, zonal flow is suppressed while the mean flow increases. Spectral analysis of density and potential fluctuations shows a redistribution of power from low-frequency (0.1-1 kHz) to high-frequency (1-300 kHz) components, along with an increase in the spectral slope and the ratio PHF/PLF. This change is linked to a reduction in Reynolds stress due to the loss of correlation between radial and poloidal velocity fluctuations, which possibly weakens the drive for zonal flow generation. Similar behavior is observed near the peak gradient region, also indicating its global nature. The present results suggest a transition from a zonal-flow-dominated regime to a state dominated by smaller-scale fluctuations, possibly influenced by mean flow shear. These findings highlight how the MAGNETic field redistributes spectral energy across frequency scales in drift-wave turbulent plasmas
[abstract 59 / 72] (score: 2) - Title: Precise and Rapid Parameter Inference of Kilonova with Conditional Variational AutoencoderAuthors: Surojit Saha, Albert K. H Kong,Comments: 18 pages,9 images, Accepted for publication in Publications of the Astronomical Society of the Pacific (PASP)Subjects: astro-ph.HECreated: 2026-05-17; Updated: 2026-05-19; Datestamp: 2026-05-19
The coalescence of binary neutron stars in the GW170817 event led to the generation of gravitational waves, accompanied by the electroMAGNETic counterpart known as a kilonova (KN). Since then, it has been a prime topic of interest, as it has provided much insight into multi-messenger astronomy. Apart from existing methods for parameter estimation, we propose an alternative technique for it, utilizing the strength and flexibility of a conditional variational autoencoder. Publicly available light curves are used as training data, conditioning on the corresponding physical parameters for a chosen model; after training, we carry out rapid parameter inferences. As this approach approximates the likelihood through variational inference, it yields results more efficiently. Through this innovative approach, we demonstrated that the total time, from training to parameter inference, is under $\approx3$h. We showed that for a given KN light curve, we can rapidly perform parameter inference based on the required model.
[abstract 60 / 72] (score: 2) - Title: Diffuse gamma-ray emission in the vicinity of open cluster Berkeley 87Authors: Ziwei Ou, Xiaolong Yang,Comments:Subjects: astro-ph.HECreated: 2026-05-17; Updated: 2026-05-19; Datestamp: 2026-05-19
We report the detection of diffuse gamma-ray emission toward the young massive star cluster Berkeley 87 using FERMI data. The emission has an angular extension of 0.36 degree and a photon index of 2.68. The hadronic scenario is favored given the dense gas and the cluster's strong stellar winds.
[abstract 61 / 72] (score: 2) - Title: Four-Body Gravitational Microlensing Events Involving Both a Binary Lens and a Binary SourceAuthors: Cheongho Han, Chung-Uk Lee, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Youn Kil Jung, Kyu-Ha~Hwang, Yoon-Hyun Ryu, Yossi Shvartzvald, In-Gu Shin, Jennifer C. Yee, Weicheng Zang, Hongjing Yang, Doeon Kim, Dong-Jin Kim, Seung-Lee Kim, Dong-Joo Lee, Sang-Mok Cha, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymańskim Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Mateusz J. Mróz,Comments: 11 pages, 6 figuresSubjects: astro-ph.SRCreated: 2026-05-17; Updated: 2026-05-19; Datestamp: 2026-05-19
We present detailed analyses of three anomalous microlensing events--KMT-2021-BLG-0209, KMT-2021-BLG-0901, and OGLE-2025-BLG-0356--identified from a systematic re-examination of KMTNet light curves for which previous modeling attempts failed or left persistent residuals. Although all three events show caustic-related features consistent with binary-lens microlensing, we find that their full light-curve structures can be described by four-body configurations that required four-body configurations involving a binary lens and a binary source. In KMT-2021-BLG-0209, weak caustic-exit residuals arise from a faint companion source undergoing an additional caustic interaction. In KMT-2021-BLG-0901, a late-time re-brightening is produced when the secondary source encounters the resonant caustic long after the primary. For OGLE-2025-BLG-0356, we test the degeneracy between 3L1S and 2L2S interpretations of a short isolated anomaly and find that the 2L2S model provides a significantly better fit. Source colors and magnitudes indicate binary sources composed of (G8V, M3V), (G8V, K2V), and (G6V, G8V) stars for the three events, respectively. Bayesian inference suggests that the lenses are predominantly low-mass binaries, including one system (KMT-2021-BLG-0901) with a companion consistent with a brown dwarf. These events add to the growing sample of well-characterized 2L2S systems and underscore the importance of systematically testing complex models, particularly in anticipation of the high-precision microlensing data expected from the Roman Space Telescope survey.
[abstract 62 / 72] (score: 2) - Title: BISTRO Survey: Gravity-Dominated and Magnetically Regulated Star Formation in M17 SWAuthors: Mengke Zhao, Keping Qiu, Ji-hyun Kang, Xindi Tang, Anthony Whitworth, Derek Ward-Thompson, Takashi Onaka, Chang Won Lee, Tyler L. Bourke, Jihye Hwang, David Eden, Thiem Hoang, Motohide Tamura, Jungmi Kwon, Felix Priestley, Kee-Tae Kim, Doris Arzoumanian, James Di Francesco, Chakali Eswaraiah, Doug Johnstone, Nguyen Bich Ngoc, Zhiwei Chen, Sarah Sadavoy, Archana Soam, Ray S. Furuya, Shih-Ping Lai, Woojin Kwon, Pierre Bastien, Kate Pattle, David Berry,Comments: 19 pages, 16 figures, accepted by ApJSubjects: astro-ph.GACreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
We present high-resolution MAGNETic field maps of the M17 SW molecular cloud using JCMT 850 $μ$m dust POLARIZATION at a scale of 14$''$. The MAGNETic field exhibits a distinct arc-like structure that encircles three dense clumps (C1, C2, and C3). By combining POLARIZATION data with ammonia line observations, the plane-of-sky MAGNETic field strength, measured using the Skalidis-Tassis method to minimize angle dispersion errors, ranges from 0.1 to 2.4 mG (mean: 0.54 mG). Energy budget analysis reveals a hierarchy dominated by gravity ($e_G \approx 10^{-7.8}$ erg cm$^{-3}$), which exceeds both MAGNETic ($e_B \approx 10^{-8.3}$ erg cm$^{-3}$) and turbulent ($e_k \approx 10^{-8.7}$ erg cm$^{-3}$) energies. Since all three energy densities lie within one order of magnitude, gravitational dominance acts primarily as the global driver, while the system remains in a state of near-equipartition. Structurally, the northeastern boundary shows MAGNETic field lines perpendicular to the shock front, consistent with compression from the adjacent HII region. Within the cloud, MAGNETic field lines generally align with gravity to assist collapse, but turn perpendicular to gravity within curved accretion bridges. This configuration provides support against radial collapse while guiding gas flow. Kinematic evidence suggests that these channels transport material from Clump C3 onto the massive Clump C2. Star formation in M17 SW is globally driven by gravity but locally regulated by the MAGNETic field structure.
[abstract 63 / 72] (score: 2) - Title: Higher-order statistics of the stochastic gravitational wave background from supermassive BLACK HOLE binariesAuthors: Hinano Hisamamtsu, Koutarou Kyutoku,Comments: 15 pages, 10 figuresSubjects: astro-ph.HE astro-ph.GA gr-qcCreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
Recent progress in gravitational wave observations has positioned Pulsar Timing Arrays as a key tool for detecting the stochastic gravitational wave background in the nanohertz band. It is widely believed that this background is primarily attributed to the cosmic ensemble of inspiraling supermassive BLACK HOLE binaries. While traditional analyses have predominantly focused on the spectral amplitude and frequency dependence of the gravitational wave background, higher-order statistics such as variance, skewness, and kurtosis could potentially be useful for extracting further physical information. However, these statistical moments are known to diverge when the redshift integration is extended down to z=0. In this study, we propose a strategy to resolve this issue by introducing a physically motivated lower integration limit, z_min, defined by the sensitivity for detecting individual sources. Since higher-order statistics are primarily determined by local sources, we may adopt the lowest-order approximation with respect to redshift in their computations. Under this approximation, we demonstrate that all higher-order statistics beyond the expectation value depend on the mass function only through a weighted average of the chirp mass, <\mathcal{M}^{10/3}>, irrespective of the redshift evolution model. We show that the ratio of the variance to the expectation value provides information on <\mathcal{M}^{10/3}>/<\mathcal{M}^{5/3}> independently of the total number of mergers. We also find a consistency relation between the kurtosis and the squared skewness, paving the way for testing the binary-origin hypothesis of the gravitational wave background. Our findings demonstrate that higher-order statistics provide a new window for interpreting the gravitational wave background, offering a methodology to break existing degeneracies and refine our understanding of the mass function.
[abstract 64 / 72] (score: 2) - Title: Undulator Radiation from a Single Electron: A Temporal Double-Slit ExperimentAuthors: Shaukat Khan, Yuya Asai, Zohair Usfoor, Tatsuo Kaneyasu, Carsten Mai, Hiroshi Miyauchi, Yasuaki Okano, Arjun Radha Krishnan, Wael Salah, Miho Shimada, Vivek Vijayan, Masahiro Katoh,Comments:Subjects: physics.acc-phCreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
Double-slit diffraction studies with photons or massive particles rank among the most beautiful experiments in physics. In particular, measurements at very low intensities demonstrate the particle-wave duality and the coherent superposition of states very clearly. In this paper, low-intensity double-slit experiments in the time domain are presented measuring the spectral distribution of SYNCHROTRON light from a single RELATIVISTIC electron in a storage ring. In two consecutive radiation sources (so-called undulators) with a MAGNETic detour between them, electrons emit two temporally separated light pulses leading to a spectrum with interference fringes, very much like the angular distribution of light behind two spatially separated slits. Independent experiments at two SYNCHROTRON light sources (DELTA in Germany and UVSOR-III in Japan) directly demonstrate that the spectral distribution of accumulated SYNCHROTRON light from a single electron is essentially the same as the spectrum from a beam of many electrons. While the latter is usually explained as interference between electroMAGNETic waves from the two undulators, the single-electron experiments demonstrate that coherent photon emission is delocalized over several meters and the accumulated spectral distribution exhibits a deterministic interference pattern at small wavelengths. The experiments presented here were conducted with near-ultraviolet light to avoid an elaborate in-vacuum setup, but the very wide spectral range of SYNCHROTRON radiation, from infrared light to X-rays, enables access to regimes not available in LASER-based quantum optics experiments.
[abstract 65 / 72] (score: 2) - Title: Time Series Extrinsic Regression of Ion Cyclotron Emission Spectra Trained on Particle-In-Cell SimulationsAuthors: Ethan Attwood, J. W. S. Cook, Peter Hill,Comments: 8 page letter including references; 4 figures. Submitted to Physical Review LettersSubjects: physics.plasm-phCreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
Ion Cyclotron Emission (ICE) is a ubiquitous MAGNETised plasma phenomenon previously detected on virtually all large MAGNETic fusion devices and whose diagnostic potential for future power plants rests upon an accurate mapping of plasma parameters to spectra. This work demonstrates that the inverse problem is solved by training Time-Series Extrinsic Regression (TSER) models on synthetic ICE spectra from oblique propagation angle sweeps of nonlinear fully kinetic 1D3V particle-in-cell simulations of the MAGNEToacoustic cyclotron instability. Using datasets from a systematically constructed scan over reactor-relevant ranges of background MAGNETic field strength, density, and alpha-particle velocity pitch ($v_\parallel/|v|$) and concentration, we show that these bulk and fast ion parameters may be recovered from a JET ICE spectrum via TSER models with near real-time capability.
[abstract 66 / 72] (score: 2) - Title: Polarization Observations of a Sample of 6.7 GHz Methanol MasersAuthors: Paul Fallon, Derck P. Smits,Comments: 26 pages, 14 figuresSubjects: astro-ph.GA astro-ph.SRCreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
Spectra of 6.7 GHz methanol masers from 21 pointings of known star-forming regions are reported. The C-band observations, using the Green Bank Telescope in full Stokes mode, have measured how POLARIZATION properties vary across the maser profiles in each spectrum and vary between different epochs of observation. Two-thirds of the sources are observed to have 6.7 GHz methanol masers, including one new detection (G240.316+0.071). Linear POLARIZATION is in the range 0 to 15% and circular POLARIZATION 0 to $\pm$9%, in line with previously reported values. The only instances where POLARIZATION is not observed is when these POLARIZATION ranges are below 3$σ$ detection limits. Zeeman splitting is observed in several sources, with splitting values derived from velocity separation between RCP and LCP components via Gaussian fitting. These values are seen to change with time and appear to correspond to changes in the linear and circular POLARIZATION. The POLARIZATION properties varying across the spectra and changing with time are most likely due to variations in the MAGNETic fields.
[abstract 67 / 72] (score: 2) - Title: A Three-Dimensional Exploration of Magnetic Fields, Rotation, and Shock Revival in a $39 M_\odot$ Core-Collapse Supernova ProgenitorAuthors: Liubov Kovalenko, Evan O'Connor, Haakon Andresen, Sean M. Couch,Comments: Submitted to Astronomy & Astrophysics (A&A), 24 pages, 23 figures, 2 videos (https://nextcloud.fysik.su.se/s/77ogas6CrTcsKwe) Comments are welcomeSubjects: astro-ph.HECreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
We present three-dimensional hydrodynamic and MAGNETohydrodynamic core-collapse SUPERNOVA simulations of a rapidly rotating, high-compactness $39 M_\odot$ progenitor to investigate the roles of rotation and MAGNETic fields in shock revival and outflow morphology. This study is designed to separate neutrino-driven expansion, rotation-induced deformation, and MAGNETically aided polar outflow within the same progenitor. We evolve three models: a non-rotating hydrodynamic baseline, a rotating hydrodynamic model, and a rotating MAGNETized model. All three models reach runaway shock expansion within the simulated interval, but with markedly different morphologies and timescales. The MAGNETized model revives first and develops the clearest bipolar outflow. The rotating non-MAGNETized model undergoes the latest shock revival and remains comparatively compact at the end of the simulation. The non-rotating model also undergoes shock revival, but subsequently collapses to a BLACK HOLE about one second after core bounce. In the MAGNETized model, Maxwell stresses redistribute angular momentum and extract energy from the differential rotation of the protoneutron star, reducing the inner-core spin and helping channel rotational free energy into the emerging polar outflow. Neutrino emission provides an additional, though smaller, angular-momentum sink in both rotating models. We find that rapid rotation and strong MAGNETic fields can launch an early MAGNETically aided polar outflow in 3D, while the resulting dynamics remain intrinsically non-axisymmetric. In this extreme progenitor, rotation also provides significant support against prompt black-hole formation, although the longer-term remnant stability remains uncertain beyond the simulated interval.
[abstract 68 / 72] (score: 2) - Title: Dyonic Black Holes in Lorentz-Violating Gravity with a Background Kalb--Ramond FieldAuthors: Yu-Xuan Lin, Jia-Zhou Liu, Yu-Xiao Liu,Comments: 30 pages, 5 figuresSubjects: gr-qcCreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
By introducing a nonminimal coupling between the Kalb--Ramond field and the electroMAGNETic field, we construct an exact four-dimensional static, spherically symmetric dyonic BLACK HOLE solution in Lorentz-violating gravity with a background Kalb--Ramond field. The curvature invariants show that the spacetime retains a genuine curvature singularity at $r=0$. We then analyze the geodesic motion of null and timelike particles and obtain the photon-sphere radius, the shadow radius, and the innermost stable circular orbit, demonstrating that both the Lorentz-violating parameter and the dyonic charges can appreciably modify the shadow size and the domain of stable circular motion. In the extended phase space, we derive the thermodynamic quantities and verify the first law of BLACK HOLE thermodynamics together with the Smarr relation. The system also exhibits a first-order phase transition between small and large BLACK HOLEs, and its phase structure is strongly influenced by the Lorentz-violating parameter and the dyonic charges.
[abstract 69 / 72] (score: 2) - Title: Probing (sub-)solar-mass BLACK HOLEs and superspinars with current and next-generation gravitational-wave observatoriesAuthors: K. S. Sruthy, N. V. Krishnendu, Chandrachur Chakraborty, Nami Uchikata,Comments: 14 pages, 4 figuresSubjects: gr-qc astro-ph.HECreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
Gravitational-wave observations provide a powerful probe of compact objects and strong-field gravity. In this work, we investigate the detectability of binaries containing (sub-)solar-mass BLACK HOLEs and superspinars with current and next-generation gravitational-wave observatories. Such objects may arise from primordial formation channels or from more exotic high-energy scenarios, and their detection would provide important insights into the population of low-mass compact objects and the physics of extreme gravitational fields. We model the gravitational-wave signals using the frequency-domain post-Newtonian inspiral waveform model TaylorF2, and truncate the signal at the innermost stable circular orbit (ISCO) to avoid contamination from the post-inspiral regime. We assess the observability of these systems using the sensitivities of current detectors such as Advanced LIGO and upcoming third-generation observatories including the Einstein Telescope and Cosmic Explorer. Our results show that while current detectors have limited reach for very low-mass binaries, third-generation observatories can enhance both detection capability and parameter-estimation precision. Their improved strain sensitivity and extended low-frequency coverage allow these observatories to track the inspiral phase over a substantially larger number of gravitational-wave cycles. As a result, they achieve considerably higher signal-to-noise ratios and provide dramatically improved constraints on binary parameters. In particular, it is possible to measure the primary spin parameter with precision $Δχ_{1z}~\sim~10^{-4}-10^{-3}$, potentially allowing clear observational discrimination between near-extremal BLACK HOLEs and superspinars in the mass range $0.1~M_\odot-2~M_\odot$ and with signal-to-noise ratio of $\sim 100-350$.
[abstract 70 / 72] (score: 2) - Title: An explicit, energy-conserving particle-in-cell scheme for RELATIVISTIC plasmasAuthors: Lee Ricketson, Jingwei Hu,Comments:Subjects: physics.plasm-ph cs.NA math-ph math.MP math.NACreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
We extend the recently-developed explicit, energy-conserving particle-in-cell (PIC) scheme of [1] to the RELATIVISTIC Vlasov-Maxwell system. As in the non-RELATIVISTIC case, the method is built on an optimization problem that is analytically solvable, local to each particle, and designed to enforce exact energy conservation. Although the solution to this optimization problem is not guaranteed to be real, we show that such instances are rare enough for practical simulation parameters to permit dramatic improvements in energy conservation over traditional explicit PIC schemes. We show that, as in the non-RELATIVISTIC case, the scheme is compatible with popular field-solvers for electroMAGNETic PIC schemes, including the Yee/FDTD and pseudo-spectral analytic time-domain (PSATD) methods. The scheme is verified on standard RELATIVISTIC test problems, where its conservation properties are confirmed.
[abstract 71 / 72] (score: 2) - Title: Towards the Deployment of the First NectarCAM, a Medium-Sized-Telescope Camera for the Cherenkov Telescope Array ObservatoryAuthors: Pablo Correa, CTAO NectarCAM Collaboration,Comments: 4 pages, 2 figures, contribution to the 2026 Very High Energy Phenomena in the Universe session of the 60th Rencontres de MoriondSubjects: astro-ph.IM astro-ph.HECreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
NectarCAM is a Cherenkov camera designed to detect gamma rays with energies between 80 GeV and 50 TeV. It will equip nine medium-sized telescopes (MSTs) of the Cherenkov Telescope Array Observatory. NectarCAM consists of 1855 pixels distributed over 265 modules. Each pixel consists of a photomultiplier tube that is connected to a NECTAr3 chip. This NECTAr3 chip contains a 12-bit digitizer with a GHz sampling rate, and has a typical readout deadtime of ${\sim}0.7$ $μ$s. In these proceedings, we highlight the performance of the NectarCAM in terms of time resolution and charge resolution. We also present the latest calibration techniques that were recently implemented for the camera. Finally, we briefly present the current status and plans of the NectarCAM production; the first production-line NectarCAM will be ready for shipment by Summer 2026, and it is planned to equip one of the MST pathfinders of CTAO.
[abstract 72 / 72] (score: 2) - Title: A universal framework to identify eccentric binary mergers: GW200105 case studyAuthors: Teagan A. Clarke, Isobel M. Romero-Shaw, Charlie Hoy, Jakob Stegmann, Paul D. Lasky, Eric Thrane,Comments: 10 pages, 4 figures, 1 tableSubjects: astro-ph.HE gr-qcCreated: 2026-05-18; Updated: 2026-05-19; Datestamp: 2026-05-19
Orbital eccentricity in gravitational-wave signals from merging compact object binaries is a powerful indicator of their formation channel. Several binary BLACK HOLE mergers and a neutron star--BLACK HOLE merger have been reported to exhibit signs of eccentricity, but which events are identified and the significance of the eccentricity differs between studies. Measurements of eccentricity can change depending on the choice of prior. The choice of prior is subtle: eccentricity is commonly measured at an arbitrary reference frequency, which varies from study to study. We use the candidate eccentric neutron star--BLACK HOLE merger GW200105_162426 as a case study, employing a range of priors and reference frequencies, and find the results to be strongly prior-driven. We show that the varied results reported across different studies can be partially reconciled by accounting for the evolution of eccentricity with reference frequency. In order to make conclusive statements about eccentricity, we propose a detection statistic that does not depend on reference frequency, and which marginalises over astrophysically-motivated distributions in eccentricity. Using this detection statistic, we find reduced support for the eccentric hypothesis for GW200105_162426: we obtain a natural log Bayes factor ln B $\leq$ 0.9 comparing the eccentric, aligned-spin hypothesis to the quasi-circular, precessing hypothesis. Our results cast doubt on the eccentric interpretation of GW200105_162426 and underscore the importance of modelling the astrophysical distributions of eccentricity in nature.
arXiv:2605.17397 [pdf, ps, other]
arXiv:2605.17460 [pdf, ps, other]
arXiv:2605.16495 [pdf, ps, other]
arXiv:2605.18283 [pdf, ps, other]
arXiv:2605.17060 [pdf, ps, other]
arXiv:2507.10276 [pdf, ps, other]
arXiv:2601.07928 [pdf, ps, other]
arXiv:2602.09102 [pdf, ps, other]
arXiv:2603.28666 [pdf, ps, other]
arXiv:2605.16698 [pdf, ps, other]
arXiv:2605.17441 [pdf, ps, other]
arXiv:2605.17455 [pdf, ps, other]
arXiv:2605.17735 [pdf, ps, other]
arXiv:2605.18050 [pdf, ps, other]
arXiv:2605.18122 [pdf, ps, other]
arXiv:2605.03019 [pdf, ps, other]
arXiv:2605.05429 [pdf, ps, other]
arXiv:2605.16766 [pdf, ps, other]
arXiv:2605.17195 [pdf, ps, other]
arXiv:2605.17344 [pdf, ps, other]
arXiv:2605.17547 [pdf, ps, other]
arXiv:2605.17993 [pdf, ps, other]
arXiv:2605.18266 [pdf, ps, other]
arXiv:2605.18513 [pdf, ps, other]
arXiv:2605.18731 [pdf, ps, other]
arXiv:2601.11780 [pdf, ps, other]
arXiv:2605.16485 [pdf, ps, other]
arXiv:2605.16734 [pdf, ps, other]
arXiv:2605.16898 [pdf, ps, other]
arXiv:2605.16924 [pdf, ps, other]
arXiv:2605.17138 [pdf, ps, other]
arXiv:2605.17280 [pdf, ps, other]
arXiv:2605.18129 [pdf, ps, other]
arXiv:2605.18161 [pdf, ps, other]
arXiv:2605.18671 [pdf, ps, other]
arXiv:2408.04878 [pdf, ps, other]
arXiv:2504.20992 [pdf, ps, other]
arXiv:2511.22641 [pdf, ps, other]
arXiv:2512.18281 [pdf, ps, other]
arXiv:2601.19104 [pdf, ps, other]
arXiv:2602.15953 [pdf, ps, other]
arXiv:2602.19186 [pdf, ps, other]
arXiv:2603.19505 [pdf, ps, other]
arXiv:2604.26763 [pdf, ps, other]
arXiv:2605.02796 [pdf, ps, other]
arXiv:2605.05265 [pdf, ps, other]
arXiv:2605.16425 [pdf, ps, other]
arXiv:2605.16461 [pdf, ps, other]
arXiv:2605.16483 [pdf, ps, other]
arXiv:2605.16488 [pdf, ps, other]
arXiv:2605.16498 [pdf, ps, other]
arXiv:2605.16506 [pdf, ps, other]
arXiv:2605.16670 [pdf, ps, other]
arXiv:2605.16760 [pdf, ps, other]
arXiv:2605.16792 [pdf, ps, other]
arXiv:2605.17048 [pdf, ps, other]
arXiv:2605.17319 [pdf, ps, other]
arXiv:2605.17321 [pdf, ps, other]
arXiv:2605.17377 [pdf, ps, other]
arXiv:2605.17636 [pdf, ps, other]
arXiv:2605.17654 [pdf, ps, other]
arXiv:2605.17708 [pdf, ps, other]
arXiv:2605.17983 [pdf, ps, other]
arXiv:2605.18244 [pdf, ps, other]
arXiv:2605.18268 [pdf, ps, other]
arXiv:2605.18275 [pdf, ps, other]
arXiv:2605.18347 [pdf, ps, other]
arXiv:2605.18371 [pdf, ps, other]
arXiv:2605.18428 [pdf, ps, other]
arXiv:2605.18542 [pdf, ps, other]
arXiv:2605.18596 [pdf, ps, other]
arXiv:2605.18742 [pdf, ps, other]