Current date: 2026-09-11
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Datestamp limit: 2026-09-11 (0 days ago)
Created/updated limit: 2026-09-04 (7 days ago)
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Suggested sets: physics, physics:astro-ph, physics:gr-qc, physics:physics
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Scoring abstracts
Number of records retrieved: 835
Keyword score statistics
score 7 -- 1 abstracts
score 6 -- 1 abstracts
score 5 -- 5 abstracts
score 4 -- 4 abstracts
score 3 -- 8 abstracts
score 2 -- 21 abstracts
in total -- 40 abstracts
Articles that appeared on 2026-09-11
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[abstract 1 / 40] Wow! (score: 7)
- Title: Probing the details of RELATIVISTIC electrons with multifrequency observations of M87 BLACK HOLEAuthors: J. G. J. Keuper, M. Moscibrodzka,Comments: 20 pages, 23 figures. Submitted to Monthly Notices of the Royal Astronomical SocietySubjects: astro-ph.HECreated: 2026-09-10; Updated: 2026-09-11; Datestamp: 2026-09-11
Beginning in March 2026, the Event Horizon Telescope (EHT) conducted a two-month observing campaign aimed at obtaining the first time-resolved sequence of images of the BLACK HOLE M87* at the center of the Virgo A galaxy. The primary scientific objectives of this campaign are to constrain the BLACK HOLE spin and to investigate the temporal variability of the MAGNETic field and plasma properties within the horizon-scale JET-launching region. In this work, we present theoretical predictions for the spectral index maps expected from these observations. Our predictions are based on Magnetically Arrested Disk simulations performed with the EBHLIGHT code and post-processed using the IPOLE general RELATIVISTIC ray-tracing code. We investigate the temporal evolution of the spectral index for a range of electron distribution models and five different BLACK HOLE spin values. The analysis includes both frequency bands currently present within the EHT and neighboring frequencies proposed for future extensions of the EHT array. In addition to extending previous studies to a broader range of observing frequencies, our work systematically investigates the time variability of the predicted spectral index maps. In purely thermal electron models, the temporal variability of the spectral index maps closely traces variations in the MAGNETic field strength and electron temperature in the immediate vicinity of the event horizon. By contrast, models incorporating a non-thermal electron population exhibit substantially weaker spectral index variability, owing to the contribution of a power-law component with a fixed spectral slope. Our numerical results are consistent with theoretical expectations. Finally, a comparison with the recently measured integrated spectral index of the M87* enables us to place preliminary constraints on the model parameters.
[abstract 2 / 40] Yes (score: 6) - Title: Deciphering the IceCube Diffuse Neutrino Observations via AGN VariabilityAuthors: Caijin Xie, Zijian Qiu, Yudong Cui, Sujie Lin, Lili Yang,Comments: 29 pages, 10 figuresSubjects: astro-ph.HECreated: 2026-09-10; Updated: 2026-09-11; Datestamp: 2026-09-11
The physical origin of the diffuse neutrino background and its spectral break at $\sim$ 30 TeV remain a major puzzle in multi-messenger astrophysics. In this work, we demonstrate that this spectral feature is a natural consequence of AGN activity cycles and the resulting COSMIC RAY (CR) propagation. We present a unified model coupling the active and quiescent phases of AGNs, where CRs accelerated in the active core undergo subsequent diffusion and hadronic interactions in the host galaxy during the quiescent phase. The superposition of these distinct evolutionary phases yields dual spectral breaks, particularly the one at tens of TeV. Under realistic energetics, our model simultaneously accounts for the IceCube diffuse flux and fits the neutrino emissions of diverse sources, ranging from the BLAZAR TXS 0506+056 to the Seyfert galaxies NGC 7469, CGCG 420-015, and the Circinus Galaxy. Our findings reveal that temporal variability is essential for deciphering the cosmic neutrino landscape and tracking high-energy CR escape.
[abstract 3 / 40] Yes (score: 5) - Title: Unveiling the population of massive quenched galaxies at $z\ge2$ in the COLIBRE simulations - II. The role of AGN feedback and environment on their emergenceAuthors: Ángel Chandro-Gómez, Claudia del P. Lagos, Chris Power, Willian M. Baker, Alejandro Benítez-Llambay, Evgenii Chaikin, Harry G. Chittenden, Camila Correa, Carlos S. Frenk, Filip Huško, Kei Ito, Robert J. McGibbon, Themiya Nanayakkara, Sylvia Ploeckinger, Alexander J. Richings, Matthieu Schaller, Joop Schaye, James W. Trayford, Francesco Valentino,Comments: Accepted for publication in MNRAS (after minor changes). This work is Part II of a two-paper series (Part I: arXiv:2512.16208). 24 pages (17 of main body and 7 of appendices)Subjects: astro-ph.GACreated: 2026-09-10; Updated: 2026-09-11; Datestamp: 2026-09-11
Early ($z \gtrsim 2$) Massive ($M_{\star} \gtrsim 10^{10}\,\mathrm{M_{\odot}}$), Quenched Galaxies (MQGs) challenge current galaxy formation models. In this series, we study these systems using the new COLIBRE cosmological hydrodynamical simulations. Following the broad agreement between their predictions and observations found in the first paper, this second paper explores the processes driving galaxies to become massive and quenched in COLIBRE, identifying Active Galactic Nucleus (AGN) feedback as the primary quenching mechanism in both the thermal (L200m6 simulation) and hybrid (thermal+JET, L200m7h simulation) AGN feedback models implemented. However, the two models behave differently: while the thermal model efficiently quenches massive galaxies at $z>3$, the hybrid model is less effective because BLACK HOLEs (BHs) grow more slowly in the early Universe, and the JET component, which dominates the feedback energy, acts on longer timescales to impact galaxies. Both models predict QUASAR-like MQGs (AGN with $L_{\rm bol}\gtrsim10^{45}\,\mathrm{erg\,s^{-1}}$), with the most luminous systems associated with more recently quenched galaxies. Compared to star-forming galaxies of similar mass, MQGs host more massive BHs and exhibit higher STAR FORMATION efficiencies. These differences arise primarily from their environments before quenching, particularly at local ($\rm 0.3\,cMpc$) to intermediate scales ($\rm 1.0\,cMpc$), where overdense regions are associated with enhanced gas inflows, higher BH accretion and, hence, feedback power. We find that about $54\%$ ($20\%$) of the $z=3$ MQGs survive as the main progenitors of $z=0$ galaxies, although up to $56\%$ ($60\%$) experience rejuvenation episodes at a given redshift $z<3$ in L200m6 (L200m7h). Our results highlight the central role of BH growth, AGN feedback and environment in driving rapid quenching in the early Universe.
[abstract 4 / 40] Yes (score: 5) - Title: Wave optical imaging of an oscillating electric dipole orbiting a BLACK HOLEAuthors: Filipe Nazaré, João S. Santos, Vitor Cardoso, José Natário,Comments: 18 pages, 13 figuresSubjects: gr-qc astro-ph.HE physics.class-phCreated: 2026-09-09; Updated: 2026-09-11; Datestamp: 2026-09-11
We study the electroMAGNETic radiation and wave-optical imaging of an oscillating electric dipole orbiting a Kerr BLACK HOLE. We derive the effective 4-current associated with a pointlike oscillating electric dipole in curved spacetime, and use BLACK HOLE perturbation theory to compute the resulting radiation field at future null infinity, from first principles. We then develop a wave-optical imaging framework for a moving electroMAGNETic source in curved spacetime. We obtain images of an orbiting electric dipole, displaying RELATIVISTIC beaming, gravitational lensing, and Einstein rings. We study POLARIZATION-dependent scattering by comparing the images produced by spinning dipoles with opposite helicities, finding a displacement that roughly decreases with the inverse of the radiation frequency, as expected for a beyond-geometric-optics effect. Our results provide a first-principles benchmark for beyond-geometric-optics descriptions of electroMAGNETic radiation in Kerr spacetime.
[abstract 5 / 40] Yes (score: 5) - Title: Strong Black Hole Natal Kicks in Magnetized Accretion-Powered ExplosionsAuthors: Sean E. Li, Ore Gottlieb, Brian D. Metzger,Comments: Submitted to ApJ. 39 pages, 15 figures, 4 tables. Comments welcomeSubjects: astro-ph.HECreated: 2026-09-09; Updated: 2026-09-11; Datestamp: 2026-09-11
Asymmetric stellar explosions impart an impulse, or natal kick, to their compact remnants by linear momentum conservation. Black hole (BH) natal kicks are often assumed to be weaker than neutron star kicks because of greater mass accretion, and they are harder to constrain observationally because isolated BHs are electroMAGNETically faint. Using 3D general-RELATIVISTIC MAGNETohydrodynamic simulations lasting up to ~30 s, we show that BHs formed from the collapse of rapidly rotating massive stars (collapsars) threaded by strong large-scale MAGNETic fields can acquire large natal kicks 10^2--10^3 km/s. Asymmetric electroMAGNETic outflows, MAGNETic-flux eruptions, and the gravitational pull of aspherical ejecta shape the kick magnitude, and their relative contributions depend on the progenitor structure, MAGNETic-flux history, and BH spin. More rapidly spinning BHs receive stronger, more nearly spin-aligned kicks, primarily through the gravitational pull of asymmetric JET-driven ejecta. Delayed transitions to the MAGNETically arrested state produce more asymmetric outflows and can generate even stronger recoils. Because the large-scale MAGNETic flux required in our models is also a key ingredient of RELATIVISTIC GAMMA-RAY BURST JETs and their associated energetic, JET-driven SUPERNOVAe, natal kicks may be a natural consequence of MAGNETized collapsars. Such kicks could substantially alter BH retention in dense stellar environments, binary survival, spin-orbit misalignment, and the viability of MAGNETized collapsars in producing highly spinning BHs within the pair-instability mass gap.
[abstract 6 / 40] Yes (score: 5) - Title: Detection of hard X-ray pulsations in non-ULX X-ray pulsar 3X J0042 in M31Authors: Ketan Rikame, Biswajit Paul,Comments: 11 pages, 7 figures, Submitted to ApJSubjects: astro-ph.HECreated: 2026-09-09; Updated: 2026-09-11; Datestamp: 2026-09-11
We report the detection of hard X-ray pulsations from the M31 accreting non-ULX X-ray pulsar 3X J0042 (3XMM J004232.1+411314) using archival NUSTAR observations. The source has a spin period of ~3 s and an orbital period of ~4.15 hr, with coherent pulsations previously detected only in XMM-Newton observations. We reanalyse all five publicly available NUSTAR observations by correcting the photon arrival times for binary motion and optimizing the orbital epoch and projected semi-major axis. Coherent pulsations are detected in all five observations. The broad-band pulse profiles show similar morphology across the five observations spanning ~2.3 yr, with no significant long-term evolution. The pulse profile also shows energy dependence, with structured, non-sinusoidal profiles below ~20 keV and a less structured profile at higher energies. The pulse periods show an overall decrease over the ~2.3 yr NUSTAR baseline, continuing the long-term spin-up trend observed in the ~16 yr of XMM-Newton observations, but with a faster average spin-up rate of ~-1.1e-10 s/s compared to the earlier reported ~-6e-11 s/s. The short orbital period and inferred low-mass companion star shows it to be a low-mass X-ray binary containing a MAGNETized neutron star, with systems such as Her X-1, 3A 1822-371, and XMM J174457-2850.3 providing closer Galactic comparisons. This work represents the first detection of hard X-ray pulsations from a non-ULX extragalactic accreting pulsar.
[abstract 7 / 40] Yes (score: 5) - Title: Hbeta Spicules, Small-scale Jets, and Hbeta Microflashes: Sub-arcsecond Dynamic Events and their Magnetic Origins in the Lower Solar Chromosphere Observed by DKISTAuthors: Navdeep K. Panesar, V. Aparna, Sanjiv K. Tiwari, Alphonse C. Sterling, Ronald L. Moore, J. M. da Silva Santos,Comments: 17 pages, 9 figures, 1 table, accepted for publication in ApJ LettersSubjects: astro-ph.SRCreated: 2026-09-09; Updated: 2026-09-11; Datestamp: 2026-09-11
We examine an on-disk solar quiet region of enhanced MAGNETic network using Hbeta images from Daniel K. Inouye Solar Telescopes (DKISTs) Visible Broadband Imager (VBI) and line-of-sight MAGNETograms from DKISTs Visible Spectro-Polarimeter (ViSP). We also compare the ViSP MAGNETograms with co-aligned co-temporal line-of-sight MAGNETograms from the Solar Dynamics Observatory (SDO)/Helioseismic and Magnetic Imager (HMI). We find:(i) Two types of chromospheric JET-like features: Hbeta spicules, and small-scale JETs. Both are rooted near edges of MAGNETic network lanes. Several sit close to ViSP-detected tiny islands of either minority-polarity flux or dips in majority-polarity flux. Hence, those several plausibly stem from mixed-polarity MAGNETic flux, and are caused by chromospheric MAGNETic RECONNECTion. For H\b{eta} spicules, the average width, length, lifetimes, and speeds are 420$\pm$400 km, 2600$\pm$1600 km, 4.3$\pm$0.25 min, and 12$\pm$4.7 kms. For small-scale JETs, those are 385$\pm$100 km, 620$\pm$40 km, 5$\pm$3min, and 4.4$\pm$1.5 kms. (ii) H$β$ microflashes sit in evidently unipolar flux. Their widths, lengths, lifetimes, and speeds are 180$\pm$65 km, 365$\pm$100 km, 4.3$\pm$2.6 min, and 3.1$\pm$0.2 kms. (iii) At the base of a coronal plume, due to its higher spatial resolution than HMI, ViSP shows both some very strong (>800 G) majority-polarity flux not shown by HMI and some sub-arc-second minority-polarity-flux inclusions not shown by HMI. These sub-arcsecond chromospheric transients carry sufficient energy (10^{24}erg) to transiently heat the local chromosphere and corona and potentially contribute to solar-wind acceleration. They may represent the small-scale end of a continuum of MAGNETic-RECONNECTion-driven activity, highlighting the importance of DKIST's high-resolution MAGNETic-field measurements for understanding small-scale chromospheric dynamics.
[abstract 8 / 40] Yes (score: 4) - Title: Statistical evidence for massive BLACK HOLE recoils in ACTIVE GALACTIC NUCLEiAuthors: Bence Bécsy, Peter Raffai, Zoltán Haiman, Andor Budai, Zsolt Frei,Comments: 11 pages, 8 figures, 2 tables, version matching published paperSubjects: astro-ph.GACreated: 2026-09-10; Updated: 2026-09-11; Datestamp: 2026-09-11
We search for a population-level signature of gravitational-wave recoiling supermassive BLACK HOLEs: a positive correlation between dust obscuration and the magnitude of the line-of-sight velocity offset of broad emission lines relative to the host. Using the SDSS DR16 QUASAR catalogue, we estimate the velocity offset, $Δv$, as the difference between the broad H$β$ redshift and a noise-weighted redshift from narrow lines ([O III] 5007, [O II] 3728, and Ca II 3934). We adopt the redshift-relative colour excess $Δ(g-i)$ as a proxy for dust column density. Analysing $\sim10^{5}$ QUASARs that meet basic spectral quality requirements, we find a modest but highly significant positive correlation between $|Δv|$ and $Δ(g-i)$ (Spearman $r\simeq0.12$ and Pearson $r\simeq0.13$, with $p\ll10^{-10}$ in both cases). The fraction of highly obscured QUASARs increases with $|Δv|$, indicating that the correlation is driven by a dust-reddened subpopulation. The result is robust to the choice of minimum $|Δv|$ threshold and to the line redshift estimator (peak vs. centroid). As expected, the correlation is largely absent when velocity offsets are computed between narrow emission lines. We find systematic differences between redshifted and blueshifted subsamples, which may point to residual velocity biases or additional physical effects (e.g. winds, inflows, orientation-dependent obscuration, or asymmetric broad-line regions). Recoiling massive BLACK HOLEs provide a natural explanation for the observed correlation, but alternative scenarios should be explored. If confirmed, this would enable population-level constraints on massive BLACK HOLE merger rates, recoil dynamics, and ACTIVE GALACTIC NUCLEi disc properties.
[abstract 9 / 40] Yes (score: 4) - Title: Nonbirefringent model of orthogonal POLARIZATION modes in radio pulsars - New view on S swing and mode structure in pulsar beamAuthors: J. Dyks, A. Frankowski,Comments: 6 pages, 5 figures, submitted to AandA on 9 Jul 2026Subjects: astro-ph.HECreated: 2026-09-10; Updated: 2026-09-11; Datestamp: 2026-09-11
Two orthogonal POLARIZATION modes observed in radio pulsar signals have long been attributed to proper modes of wave oscillation in strongly MAGNETized plasma. Yet it has been shown recently that they show up readily for extended emission regions that produce incoherently-superposed POLARIZATION signal. In this paper we present a two-dimensional POLARIZATION model based on incoherent superposition of radio signals. The model involves a single proper mode, say the O mode, but leads to the appearance of two orthogonal POLARIZATION tracks and naturally produces the triple form of POLARIZATION mode segregation in averaged profiles (central mode flanked on boths sides by another mode), as well as the displacement of modes in latitude, previously inferred from beam mapping. In the case of conal emission regions, the modelled POLARIZATION tends to mimic general POLARIZATION properties of the rotating vector model (RVM). However, the reason for this is the symmetry of the emission region - not the usual projection of dipolar MAGNETic azimuths. Thus the emerging RVM parameters reveal geometry of the emission region, not of the dipolar MAGNETic field. The results strongly support the vital role of nonbirefringent modal effects in radio pulsar profiles. Two proper modes may not be needed to explain observations of two orthogonal POLARIZATION tracks.
[abstract 10 / 40] Yes (score: 4) - Title: Spin-down of the accreting MAGNETar candidate 4U 0114+65: possible first evidence for a strong coupling regimeAuthors: Graciela Sanjurjo-Ferrín, Jose Miguel Torrejón, Konstantin Postnov, Jose Joaquín Rodes-Roca, Lida Oskinova, Jessica Planelles-Villalva,Comments:Subjects: astro-ph.HECreated: 2026-09-10; Updated: 2026-09-11; Datestamp: 2026-09-11
4U~0114+65 is a high-mass X-ray binary composed of the B1\,Ia supergiant V*~V662~Cas and one of the slowest known accreting neutron stars, with a spin period of $\sim$9.4 ks. In 2025, its long X-ray pulsations became undetectable in \textit{SWIFT}/BAT monitoring, motivating a Director's Discretionary Time observation with \textit{XMM-Newton}. We compare this observation with a 2015 \textit{XMM-Newton} observation, when the source was brighter and clearly pulsed, and analyze the long-term spin evolution using \textit{SWIFT}/BAT data. We performed average and pulse-phase-resolved spectroscopy using the same model as in previous work. The 2025 observation still reveals weak pulsations, with a period of about 9.3 ks, despite their non-detection in \textit{SWIFT}/BAT. The overall spectral shape remains similar in both epochs, but the luminosity decreased by about one order of magnitude, mainly due to strong suppression of the bulk-motion Comptonization component. Although the absorbing column is higher in 2025, the inferred wind properties remain broadly compatible with those from 2015, suggesting that no major global change in the donor wind is required. Instead, the results point to a substantial reduction in accretion efficiency close to the neutron-star MAGNETosphere. We propose that 4U~0114+65 may be evolving toward partial centrifugal inhibition in the strong-coupling regime, where the toroidal MAGNETic-field component is comparable to the poloidal one. If confirmed, this would represent the first observational evidence of this state. Accretion would become progressively less efficient and more intermittent without reaching a fully developed propeller regime. The apparent disappearance of the pulse in long-term hard X-ray monitoring would then result from the lower luminosity and reduced absolute pulsed flux, rather than from the loss of the underlying spin modulation.
[abstract 11 / 40] Yes (score: 4) - Title: Experimental Plasma Density Profiles Determined Through Measurements of the Magnetosonic Wave SpeedAuthors: Cameron Kuchta, Jan Egedal, Abhishek Mhatre, Paul Gradney, Joseph Olson, Xinyu Yu, Cary B. Forest,Comments: submitted to Physics of Plasmas on 09/08/2026Subjects: physics.plasm-phCreated: 2026-09-10; Updated: 2026-09-11; Datestamp: 2026-09-11
Information on plasma density in laboratory plasmas is commonly acquired using either Langmuir probes or optical diagnostics. Here, we present an alternative approach, inferring the density profile from MAGNETic measurements of a plasma wave. In particular, during the process of creating a RECONNECTing current layer for MAGNETic RECONNECTion experiments in the Big Red Ball, the RECONNECTion drive first launches a large amplitude fast MAGNETosonic wave. The propagation of the wavefront is measured with high spatial and temporal resolutions by in situ MAGNETic diagnostics. Given a known uniform background MAGNETic field strength and the known dispersion relation of the wave, we here show how the characteristics of the wavefront can be applied to determine the initial plasma density profile.
[abstract 12 / 40] (score: 3) - Title: Laboratory measurements of energy partitioning and anomalous electron heating in MAGNETized, perpendicular collisionless shocksAuthors: V. Valenzuela-Villaseca, S. Totorica, J. Griff-McMahon, L. -J. Chen, S. Malko, P. V. Heuer, P. Pongkitiwanichakul, W. Fox, D. B. Schaeffer,Comments: Main body: 8 pages, 5 Figures. Supplemental material: 12 pages, 5 figuresSubjects: physics.plasm-ph astro-ph.HE astro-ph.SRCreated: 2026-09-10; Updated: 2026-09-11; Datestamp: 2026-09-11
We present laboratory results on energy partitioning from supercritical, MAGNETized collisionless shock experiments ($\rm{M_A} \sim 8$, $\rm{M_{ms}}\sim 4$). We report the first observation of fully-developed laboratory shocks that evolve for more than seven upstream ion gyration periods and have a downstream region that extends more than four shocked ion gyroperiods. Thomson scattering measurements are used to measure electron and ion temperatures, plasma density, and flow speeds. We directly measure a compression ratio of $3.6\pm0.3$, consistent with shock jump conditions. A foot ahead of the shock exhibits super-adiabatic electron and ion heating. The downstream electron temperature has an $\approx 30\%$ excess above adiabatic and collisional electron-ion heating, implying significant collisionless anomalous electron heating. We find a downstream electron-ion temperature ratio $T_e^{(d)}/T_i^{(d)} = 0.8 \pm 0.3$, consistent with spacecraft observations but outside the range of predictions from theory and numerical simulations.
[abstract 13 / 40] (score: 3) - Title: A Population of Little Red Dot-like Quasars in SDSSAuthors: Quinn O. Casey, Ryan C. Hickox, Nikko J. Cleri, Jonathan H. Cohn, David M. Alexander, Emmanuel Durodola, Kelly E. Whalen, Raphael E. Hviding, Tonima Tasnim Ananna,Comments: 22 pages, 7 figures (+2 appendix figures), 4 tables. Accepted for publication in The Astrophysical JournalSubjects: astro-ph.GACreated: 2026-09-09; Updated: 2026-09-11; Datestamp: 2026-09-11
Compact and red sources in the high redshift ($z\sim5$) Universe, known as "Little Red Dots" (LRDs), are among JWST's most intriguing discoveries. These sources have broad Balmer emission lines, weak X-ray emission, and unique spectral energy distributions (SEDs) poorly fit by either stellar or AGN templates. Local LRD-like objects allow for detailed studies of the underlying physical processes with archival multi-wavelength datasets unavailable in the high-$z$ Universe. We show that the SDSS $ugriz$ filters at $z\approx0.4, 0.8$ overlap well with the JWST filters used to select LRDs at $z\sim5$. We use SDSS QUASARs to define a sample of $\sim1300$ Local Red Dots (LoRDs) which share the same photometric colors of LRDs. A subset of the LoRD sample selected to have V-shaped continua ($N=244$) show prominent higher-order Balmer absorption features and [NeV]$λ$3426 emission, both of which would likely be missed in JWST/PRISM observations given the low spectral resolution. A composite SED of the LoRDs differs from a typical QUASAR SED in the rest-frame UV/optical, but the two agree with each other in the NIR. The LoRD SED matches well with a stack of LRDs and can be modeled either as a reddened AGN combined with a host galaxy, or as a reddened AGN combined with a host galaxy and a cool blackbody. Interestingly, the LoRDs are X-ray detected at a rate comparable to typical QUASARs. However, the probability that LoRDs and typical QUASARs would go undetected, if subject to the LRD X-ray upper limits, is $>50\%$.
[abstract 14 / 40] (score: 3) - Title: Vacuum Cherenkov radiation in supercritical MAGNETic fieldsAuthors: Daniel Gálvez-García, Nora Bretón,Comments: 16 pages, 5 figuresSubjects: gr-qcCreated: 2026-09-09; Updated: 2026-09-11; Datestamp: 2026-09-11
In the presence of very intense electroMAGNETic fields, the refractive index of vacuum is modified such that light velocity is less than $c$ and ultraRELATIVISTIC charged particles can be faster than light and can induce Cherenkov radiation. We present the comparison of the Cherenkov radiation produced by the Euler-Heisenberg theory for critical and supercritical MAGNETic fields. We also make the comparison between the Cherenkov and the SYNCHROTRON radiation produced by the charged particles.
[abstract 15 / 40] (score: 3) - Title: The NOvA Test Beam ExperimentAuthors: NOvA Collaboration, S. Abubakar, M. A. Acero, B. Acharya, P. Adamson, N. Anfimov, A. Antoshkinaf, E. Arrieta-Diaz, L. Asquith, A. Aurisano, N. Balashov, P. Baldi, B. A. Bambah, E. F. Bannister, A. Barros, J. Barrow, A. Bat, T. J. C. Bezerra, V. Bhatnagar, B. Bhuyan, J. Bian, S. Block, A. C. Booth, B. Brahma, C. Bromberg, N. Buchanan, J. Burns, A. Butkevich, T. J. Carroll, E. Catano-Mur, J. P. Cesar, C. Chang, S. Chaudhary, H. Chen, S. Choate, B. C. Choudhary, O. T. K. Chow, A. Christensen, M. F. Cicala, T. E. Coan, T. Contreras, A. Cooleybeck, L. Cremonesi, G. S. Davies, P. F. Derwent, K. Dever, Z. Djurcic, K. Dobbs, D. Dueñas Tonguino, E. C. Dukes, A. Dye, R. Ehrlich, E. Ewart, P. Filip, W. Flanagan, M. J. Frank, H. R. Gallagher, F. Gao, A. Giri, R. A. Gomes, M. C. Goodman, R. Group, A. Gusmão, A. Habig, F. Hakl, J. Hartnell, R. Hatcher, J. M. Hays, M. He, A. Heggestuen, K. Heller, V Hewes, A. Himmel, T. Horoho, J. Huang, X. Huang, T. Huynh, A. Ivanova, C. Joe, K. Kaess, I. Kakorin, A. Kalitkina, D. M. Kaplan, A. Khanam, B. Kirezli, J. Kleykamp, O. Klimov, L. W. Koerner, L. Kolupaeva, R. Kralik, G. Kufatty, A. Kumar, C. D. Kuruppu, V. Kus, T. Lackey, K. Lang, A. Lister, J. Liu, J. A. Lock, S. Magill, R. C. Mandujano, W. A. Mann, M. T. Manoharan, M. Manrique Plata, A. Marathe, M. L. Marshak, M. Martinez-Casales, V. Matveev, T. McGuire, A. Medcalf, A. Medhi, B. Mehta, M. D. Messier, H. Meyer, T. Miao, S. Mishra, R. Mohanta, A. Moren, A. Morozova, W. Mu, L. Mualem, M. Muether, C. Murthy, D. Myers, J. Nachtman, D. Naples, J. K. Nelson, O. Neogi, R. Nichol, E. Niner, G. Nissan, M. Nixon, A. Norman, A. Norrick, D. Northacker, H. Oh, A. Olshevskiy, T. Olson, Y. Onel, A. Pal, J. Paley, L. Panda, R. B. Patterson, G. Pawloski, R. Petti, D. D. Phan, R. K. Pradhan, L. R. Prais, S. Puhan, J. Rabaey, A. Rafique, M. Rajaoalisoa, B. Ramson, B. Rebel, C. Reynolds, P. Roy, D. Sagar, O. Samoylov, M. C. Sanchez, S. Sãnchez Falero, P. Shanahan, P. Sharma, A. Sheshukov, S. Shukla, I. Singh, P. Singh, V. Singh, P. Snopok, E. Sobimpe, N. Solomey, A. Sousa, K. Soustruznik, M. Strait, C. Sullivan, L. Suter, A. Sutton, K. Sutton, S. K. Swain, A. Sztuc, N. Talukdar, P. Tas, J. Thomas, E. Tiras, M. Titus, Y. Torun, D. Tran, J. Trokan-Tenorio, J. Urheim, B. Utt, P. Vahle, Z. Vallari, K. J. Vockerodt, A. V. Waldron, M. Wallbank, B. Wang, C. Weber, M. Wetstein, D. Whittington, D. A. Wickremasinghe, J. Wolcott, W. Wu, Y. Xiao, B. Yaeggy, A. Yahaya, A. Yallappa Dombara, A. Yankelevich, K. Yonehara, S. Zadorozhnyy, J. Zalesak, L. Zhao, R. Zwaska,Comments:Subjects: hep-exCreated: 2026-09-09; Updated: 2026-09-11; Datestamp: 2026-09-11
NOvA is a long-baseline neutrino oscillation experiment designed to study the neutrino mixing parameters, mass ordering, and CP violation in the lepton sector. A key component of the success of the experiment is a robust understanding of the systematic uncertainties associated with detector response and calibration. To address this, NOvA deployed a Test Beam experiment at the FERMIlab Test Beam Facility, which collected data from April 2019 through July 2022. The NOvA Test Beam experiment used a 30-ton segmented liquid scintillator detector functionally identical to the NOvA Near and Far Detectors to analyze tagged particles produced from p-Cu collisions, with instrumentation capable of selecting and identifying electrons, muons, pions, kaons, and protons with momentum ranging from 0.4-1.5GeV/c. Analysis of the collected data provides a better understanding of the largest systematic uncertainties impacting NOvA's analyses, which include the detector response, energy calibration, and hadronic and electroMAGNETic energy resolutions.
[abstract 16 / 40] (score: 3) - Title: Magnetising the quokka code with fast, second-order accurate, error-correcting schemes for MAGNETohydrodynamics on GPUsAuthors: Neco Kriel, Elizabeth Cole-Kodikara, Benjamin Wibking, Mark R. Krumholz, Chong-Chong He, Anish Sarkar, Pak Shing Li,Comments: 28 pages, 23 pages, submitted to MNRASSubjects: astro-ph.IMCreated: 2026-09-09; Updated: 2026-09-11; Datestamp: 2026-09-11
We implement a second-order accurate constrained transport (CT) MAGNETohydrodynamics (MHD) module with first-order flux correction in the open-source, adaptive mesh refinement (AMR), GPU-accelerated code quokka, supporting both ideal and resistive (constant Ohmic) regimes. For computing and averaging the electromotive forces (EMFs) at cell edges, the basis of any CT-MHD method, we experiment with a wide range of recent, state-of-the-art schemes, together with different reconstruction schemes. Alongside these, we develop a new EMF compute scheme that requires fewer reconstruction steps than existing approaches. We evaluate these scheme combinations on the basis of accuracy, stability, and GPU throughput, and demonstrate that our new scheme achieves accuracy comparable to the best-in-class existing methods, together with greater stability in RECONNECTion-dominated flows and roughly 25--60% higher GPU throughput. Using this scheme, quokka achieves excellent results across a wide range of MHD flow regimes, reaching >50 million cell updates per GPU per second, with >70% parallel efficiency out to >500 GPUs. Finally, we confirm that our CT implementation preserves divergence-free MAGNETic fields (to machine precision) under AMR.
[abstract 17 / 40] (score: 3) - Title: Nitrogen-Loud Quasars from the Dark Energy Spectroscopic Instrument. I. Sample Selection and Basic PropertiesAuthors: Shuo Zhai, Wei-Jian Guo, Yong-Jie Chen, Zhi-Qiang Chen, Haining Li, Jian-Min Wang, Gang Zhao,Comments: Submitted to ApJSSubjects: astro-ph.GACreated: 2026-09-10; Updated: 2026-09-11; Datestamp: 2026-09-11
We present the largest sample to date of nitrogen-loud (N-loud) QUASARs with strong broad N IV] $\lambda1486$ and/or N III] $\lambda1750$ emission lines over the redshift range $1.6 < z < 4.3$, selected from the Dark Energy Spectroscopic Instrument (DESI) Data Release 1. The final sample contains 1,993 N-loud QUASARs, corresponding to about 1.2% of the parent QUASAR sample. The $L_{1450}$ distribution of the N-loud QUASARs is broadly similar to that of the DESI parent sample, but their redshift distribution is distinct, with a stronger concentration around $z \sim 2.5$--3. Their composite spectrum displays a broadly similar UV continuum shape to that of the parent QUASARs, while showing significantly enhanced broad nitrogen emission features, including N V, N IV], and N III]. Other metal emission features also show a moderate enhancement. Relative to a control sample matched in redshift and UV continuum luminosity, the N-loud QUASARs show systematically narrower broad C IV and Mg II emission lines, lower single-epoch virial BLACK HOLE masses, and higher Eddington ratios, suggesting that N-loud QUASARs may preferentially appear during a relatively rapid BLACK HOLE accretion phase. The radio-loud fraction is 10.1%, with the highest fraction among objects exhibiting both N III] and N IV] emission. The catalog provides a statistical baseline for future studies of nitrogen enhancement and its physical origin.
[abstract 18 / 40] (score: 3) - Title: Evidence for plasmoid formation related to a hot UV burst in the solar atmosphereAuthors: Mats Ola Sand, Luc Rouppe van der Voort, Souvik Bose, Daniel Nobrega-Siverio, Jonas Thoen Faber, Reetika Joshi, Ignasi Josep Soler Poquet,Comments: main article 13 pages, appendix 6 pages, includes links to movies associated with figuresSubjects: astro-ph.SRCreated: 2026-09-10; Updated: 2026-09-11; Datestamp: 2026-09-11
Magnetic RECONNECTion in the solar atmosphere drives energetic phenomena such as Ellerman bombs, UV bursts, and surges. We used coordinated observations from the Swedish 1-m Solar Telescope (SST), IRIS, SDO, and the Hinode/X-ray Telescope (XRT) to analyze an active region with strong MAGNETic flux emergence. This region displayed long duration UV burst activity, occurrence of multiple Ellerman bombs, and recurrent ejection of surges. Chromospheric imaging show sthe presence of a dome-like structure that overarched the region where MAGNETic flux was emerging. The curved chromospheric fibrils were closely associated with bright and similarly curved extensions from a UV burst in the IRIS 1400 A channel. We observed an episode of formation of a bright sheet along the curved fibrils in H-beta that subsequently fragmented into plasmoid-like blobs with peak emission at a Doppler offset of +43 km/s. IRIS Si IV lines in the same region show complex and non-Gaussian line profiles that display asymmetric extensions to high Doppler offsets. Some profiles have clear components with Doppler offsets in excess of 150 km/s on both sides of the nominal line center. The optically thin SDO/AIA channels, including 94 A, show intermittent and repeated occurrences of the burst. Emission measure and filter ratio analysis indicate that the burst is multi-thermal and can attain temperatures beyond 1 MK. AIA and Hinode/XRT observations reveal a localized EUV and soft-X-ray counterpart of the burst/dome system, supporting the presence of intrinsically multithermal plasma that reaches coronal, and likely multi-MK, temperatures.
[abstract 19 / 40] (score: 3) - Title: Relativistic Magnetohydrodynamics from Myers-Pospelov Lorentz-Violating ElectrodynamicsAuthors: Matheus Duarte, Vitor de Souza,Comments:Subjects: astro-ph.HECreated: 2026-09-10; Updated: 2026-09-11; Datestamp: 2026-09-11
We derive the equations of RELATIVISTIC MAGNETohydrodynamics from Lorentz-violating Myers-Pospelov electrodynamics. Starting from the modified fermionic and electroMAGNETic equations of motion, we employ the covariant Wigner formalism to establish the semiclassical spectral constraints and distribution function, which, combined with Noether's theorem, yield the energy-momentum tensor, particle current, and corresponding conservation laws in the presence of Lorentz violation. The resulting hydrodynamic description contains Lorentz-violating corrections to the thermodynamic quantities and to the fluid currents. In the purely timelike sector, these corrections can be absorbed into effective thermodynamic quantities, preserving the isotropic structure of the fluid equations. In contrast, spacelike backgrounds introduce explicit contributions along the preferred direction, which cannot be absorbed into the standard hydrodynamic variables and give rise to anisotropic forces and torques. These effects lead to departures from standard RELATIVISTIC MAGNETohydrodynamics and provide a direct macroscopic manifestation of the Lorentz-violating background. Our results provide a first-principles derivation of Lorentz-violating RELATIVISTIC MAGNETohydrodynamics and establish a framework for investigating the macroscopic consequences of Lorentz violation in MAGNETized RELATIVISTIC fluids.
[abstract 20 / 40] (score: 2) - Title: First flow harmonic of net baryon from directed diffusion of stopped baryonsAuthors: Tribhuban Parida, Sandeep Chatterjee,Comments:Subjects: nucl-thCreated: 2026-09-10; Updated: 2026-09-11; Datestamp: 2026-09-11
We propose a new ansatz for baryon deposition that incorporates salient features from the baryon junction picture. The deposited baryon is coupled to a tilted fireball and deployed to study the directed flow of identified hadrons in Au+Au collisions at $\sqrt{s_{NN}}=7.7-200$ GeV. We find a parameter space in the model where the resulting hydrodynamic evolution generates a suitable flow to describe the directed flow $v_1$ of identified hadrons including the observed double sign change between $\sqrt{s_{NN}}=7.7-39$ GeV of the rapidity slopes of the net proton and the net lambda $v_1$. Our model that includes stopping of baryons and their consequent diffusion within a RELATIVISTIC hydrodynamic framework along with a crossover equation of state as obtained from lattice QCD calculations provides a noncritical baryonic baseline that is crucial in our ongoing searches for the QCD critical point and the initial strong electroMAGNETic field.
[abstract 21 / 40] (score: 2) - Title: Dark matter interpretation of GRB 221009A: a singlet scalar explains LHAASO dataAuthors: S. Peyman Zakeri,Comments:Subjects: hep-ph astro-ph.HECreated: 2026-09-10; Updated: 2026-09-11; Datestamp: 2026-09-11
In this work, we propose a DARK MATTER (DM) interpretation of the intensive gamma ray burst GRB 221009A. This indirect detection approach devotes to the decay of DM particles into high energy (HE) photons. In this context, a singlet scalar DM generated at the redshift of GRB 221009A is up-scattered by the high energy COSMIC RAYs (HECRs) during its propagation to Earth. This highly boosted DM then possesses a high flux and undergoes a dominant di-photon decay before reaching the detector. The Large High Altitude Air Shower Observatory (LHAASO) probes such energetic gamma rays whereby has recorded a $\sim$13 TeV event for the aforementioned GRB.
[abstract 22 / 40] (score: 2) - Title: A Geometric Reinitialization for Conservative Level-Set Methods in the Context of Capillary FlowsAuthors: Helene Papillon-Laroche, Amishga Alphonius, Magdalena Schreter-Fleischhacker, Jean-Philippe Harvey, Bruno Blais,Comments:Subjects: physics.flu-dynCreated: 2026-09-09; Updated: 2026-09-11; Datestamp: 2026-09-11
Simulations of immiscible two-phase flows involving surface tension (ST) require a robust high-fidelity framework. State-of-the-art multi-phase models, such as the Conservative Level-Set (CLS) approach, use Eulerian representations of the fluids and their interface, and require reinitialization methods to ensure volume conservation and accurate ST force modeling. This work proposes a new geometric reinitialization strategy for CLS formulations as an alternative to the typical PDE-based reinitialization methods. Building on the geometric reinitialization developed in context of level-set frameworks, the proposed method is an extension to the CLS approach within an open-source finite element framework that allows for fully distributed and adaptively refined, two- and three-dimensional meshes. This extension enables application of the geometric reinitialization method to large-scale three-dimensional problems with strongly deforming interfaces, including breakup. The method is quantitatively compared to two established reinitialization approaches: the PDE-based reinitialization proposed in the original CLS method and a simple projection-based approach. The assessment comprises three 3D application cases of increasing complexity: the capillary migration of a droplet, the rise of a bubble, and the Rayleigh-Plateau instability development in a capillary JET. The geometric method leads to high-quality, spatially-converged results in good agreement with benchmark and reference solutions. It robustly and accurately recovers expected interface topology-based metrics (e.g., the volume, surface area and sphericity), and relevant flow quantities. In addition, the proposed method has only two parameters and is robust across parameter choices and cases.
[abstract 23 / 40] (score: 2) - Title: Cosmological Constraints from Gravitational Wave-Fast Radio Burst Associations without Redshift Measurements for LIGO-Virgo and Cosmic ExplorerAuthors: Jiaming Zhuge, Marios Kalomenopoulos, Carl-Johan Haster, Bing Zhang,Comments:Subjects: astro-ph.CO astro-ph.HECreated: 2026-09-10; Updated: 2026-09-11; Datestamp: 2026-09-11
The potential association between gravitational waves (GWs) and fast radio bursts (FRBs) offers a unique multi-messenger probe for cosmology. In this paper, we develop a redshift-independent framework to constrain cosmological parameters using the luminosity distance - dispersion measure relation, accounting for realistic astrophysical uncertainties. We perform a comprehensive comparative analysis across different GWs detector sensitivities and modeling assumptions. Specifically, we investigate the performance of the current LIGO-Virgo (LV) network (at $z < 0.2$) versus the future Cosmic Explorer (CE). Our study further evaluates the impact of different dispersion measure (DM) distributions---specifically the corrected Macquart's PDF (Zhuge+2025) and the log-normal distribution---and explores the influence of including or excluding host galaxy DM contributions. Using realistic simulated observations, we find that while the current LV network lacks the precision to provide meaningful constraints, CE will enable high-precision cosmology. Even without spectroscopic redshifts, CE observations can effectively break parameter degeneracies and robustly constrain both cosmology and host galaxy parameters. These results highlight the necessity of next-generation detectors.
[abstract 24 / 40] (score: 2) - Title: Mass-Ratio Reversal as an Alternative to Hierarchical Mergers for GW241011Authors: Rui-Chong Hu, Ying Qin, Bing Zhang,Comments: 10 pages, 5 figures, accepted for publication in ApJLSubjects: astro-ph.HE astro-ph.SRCreated: 2026-09-10; Updated: 2026-09-11; Datestamp: 2026-09-11
Recent gravitational-wave (GW) observations have revealed binary BLACK HOLE (BBH) mergers with both extreme mass ratios and large effective spin parameters ($χ_{\rm{eff}}$). GW241011 is a notable example that shows these properties. Although hierarchical mergers (second-generation + first-generation BHs) can naturally produce high spins and become more prevalent than first-generation + first-generation mergers at mass ratios $q \lesssim 0.6$, they are negligible at the extreme mass ratio $\sim 0.3$ and are further limited by gravitational recoil kicks that can eject the second-generation BH from the host environment. Moreover, recent studies have argued against a dynamical origin for GW241011. Here, we investigate the formation of GW241011-like systems through the mass-ratio reversal (MRR) channel in isolated binary evolution. By quantifying the probability of producing such systems across a range of binary-evolution models, we identify the key dependencies on stellar-evolution and binary-interaction physics. Our results demonstrate the conditions under which the MRR channel can provide a viable alternative to hierarchical mergers for GW241011-like events, although its predicted merger rate density remains relatively low.
[abstract 25 / 40] (score: 2) - Title: Interstellar Complex Organic Molecules and Molecular Outflows in NGC 1333 IRAS 4B and 4B' Observed Using NOEMAAuthors: C. C. Sarver, M. M. Giese, D. C. Lis, S. L. Widicus Weaver,Comments: 43 pages, submitted to ApJSubjects: astro-ph.GA astro-ph.SRCreated: 2026-09-09; Updated: 2026-09-11; Datestamp: 2026-09-11
We present interferometric observations with the Northern Extended Millimeter Array (NOEMA) of NGC 1333 IRAS 4B and 4B', two young stellar objects (YSOs) within the Perseus molecular cloud. YSOs, especially Class 0 protostars, are rich in gas-phase interstellar complex organic molecules (iCOMs), but relatively little is known about the spatial distribution of these important prebiotic molecules. Various molecules were imaged within IRAS 4B and the surrounding area in the 145 GHz spectral range, revealing hundreds of molecular transitions within the warm inner envelope of IRAS 4B. This work provides derived physical parameters (rotational temperature, column density, velocity shift with respect to local standard of rest, and full-width at half-maximum spectral line width) for 11 molecules toward IRAS 4B including methanol (CH$_3$OH and isotopologues), methyl formate (HCOOCH$_3$), dimethyl ether (CH$_3$OCH$_3$), acetaldehyde (CH$_3$CHO), ethanol (C$_2$H$_5$OH), glycolaldehyde (CH$_2$OHCHO), acetone (CH$_3$COCH$_3$), and isocyanic acid (HNCO). Out of these molecules, 10 are iCOMs (excluding HNCO) that trace the inner envelope of IRAS 4B and mark it as a rich source of organic material. There is a strong spatial correlation between the continuum emission of IRAS 4B and iCOM molecular emission and among various iCOMs with each other. Physical parameter and integrated intensity maps show that IRAS 4B is a binary protostar system that drives a JET in a north-south orientation and an outflow in a northwest-southeast orientation. IRAS 4B' also drives a west-east outflow but shows no evidence of molecular emission cospatial with its continuum emission.
[abstract 26 / 40] (score: 2) - Title: Open Clusters as Laboratories for Cool Star Evolution: Highlights from the Cool Stars 23 Splinter SessionAuthors: Deepak Chahal, Beatrice Caccherano, Edward Gillen, Dario J. Fritzewski, Robin D. Jeffries, Kevin R. Covey, Andrew Boyle, Lyra Cao, Federica Chiti, Alexander Hughes, Leslie Moranta, Natalie R. Myers, Emily K. Pass, Phil Van-Lane, Fábio C. Wanderley, Mackenna L. Wood, Stephanie T. Douglas, David Montes, Loredana Prisinzano,Comments: 13 pages, 3 figuresSubjects: astro-ph.SR astro-ph.GACreated: 2026-09-10; Updated: 2026-09-11; Datestamp: 2026-09-11
Open clusters remain among the most powerful laboratories for calibrating how fundamental stellar properties such as rotation, MAGNETic activity, surface chemistry, and internal structure evolve over the pre-main-sequence to main-sequence and post-main-sequence stellar lifetime. Because cluster members share a common age, galactic environment, and initial composition, they provide empirical anchors upon which age-dating techniques such as gyrochronology, activity-age relations, and chemical clocks are built. This paper summarizes the Cool Stars 23 splinter session - Open Clusters as Laboratories for Cool Star Evolution, held on 15 June 2026 in Tokyo, Japan. The session comprised one invited review, ten contributed talks, and ten poster pop-up presentations, organized around three themes: the evolution of rotation, MAGNETic activity, and chemical abundances (Li-depletion, [C/N], [Y/Mg], and neutron-capture elements). We close with a summary of the open questions identified in the panel discussion and the observational and theoretical work that new surveys (e.g. Gaia DR4, 4MOST, WEAVE) and missions (e.g. PLATO, Roman) will enable over the coming years. Together, these efforts will help assess the current state of the field and shape its future directions.
[abstract 27 / 40] (score: 2) - Title: On modelling the 2017 galactic COSMIC RAY depressionAuthors: O. P. M. Aslam, D. MacTaggart, M. S. Potgieter, M. D. Ngobeni, I. I. Ramokgaba,Comments: Total 18 pages, 7 Figures, Accepted, Astrophysical JournalSubjects: astro-ph.SR astro-ph.HE physics.space-phCreated: 2026-09-08; Updated: 2026-09-11; Datestamp: 2026-09-11
In the second half of 2017, as Solar Cycle 24 approached its minimum, a pronounced and rigidity-dependent depression in the galactic COSMIC RAY (GCR) proton flux was observed using AMS-02. This event was driven by a sequence of strong coronal mass ejections (CMEs). In this work, we model the modulation of GCR protons during this period using a steady-state Parker transport framework with parameters constrained by AMS-02 observations. Treating the event as a purely long-term modulation interval yields excellent agreement with the observed proton intensities, but implies an inferred rigidity dependence of particle mean free paths that is inconsistent with basic turbulence theory, corresponding to an effective inversion of the scattering regime. We argue that this behaviour arises from the ability of highly flexible transport parameterizations to reproduce integrated modulation signatures through correlated adjustments of diffusion coefficients during transient events. To address this inconsistency, we relax the commonly adopted assumption of a time-independent ratio of perpendicular to parallel diffusion coefficients and introduce a physically motivated reduction of this ratio during the CME-dominated interval. This modification preserves the quality of the spectral fits whilst restoring the expected rigidity ordering of mean free paths. Our results indicate that allowing the perpendicular-to-parallel diffusion ratio to vary in time provides an effective means of constraining transport solutions during the 2017 depression and may help to resolve similar inconsistencies reported in other GCR modulation studies.
[abstract 28 / 40] (score: 2) - Title: Dilaton gravity can enhance quantum coherence and reduce entanglementAuthors: Zejun Wang, Zhihong Liu, Yu-Xuan Wang, Xiao-Li Huang,Comments:Subjects: gr-qcCreated: 2026-09-09; Updated: 2026-09-11; Datestamp: 2026-09-11
We investigate the influence of the Garfinkle-Horowitz-Strominger (GHS) dilaton BLACK HOLE on different quantum resources of Dirac fields beyond the single-mode approximation. By employing the negativity to characterize quantum entanglement and the $l_1$-norm and the relative entropy of coherence to characterize quantum coherence, we demonstrate that these resources exhibit remarkably different responses to the gravitational field. Specifically, increasing the dilaton parameter continuously suppresses quantum entanglement, leaving only a finite residual amount in the strong-gravity regime, whereas quantum coherence is enhanced, indicating that the dilaton-induced spacetime affects nonlocal quantum correlations and local quantum superposition in fundamentally different ways. Furthermore, we show that an initially maximally entangled state does not always possess the largest negativity after propagating in the GHS dilaton spacetime; instead, under appropriate conditions, certain non-maximally entangled states can retain stronger entanglement than the maximally entangled one. These findings reveal the resource-dependent nature of gravitational effects in dilaton BLACK HOLE backgrounds and provide new insights into the manipulation and protection of quantum resources for RELATIVISTIC quantum information processing in curved spacetime.
[abstract 29 / 40] (score: 2) - Title: Energy deposition in planetary and exoplanetary atmospheres induced by COSMIC RAYsAuthors: Jesse Polman, Ingo Leya,Comments: Accepted to A&A. 14 pages, 11 figuresSubjects: astro-ph.EP astro-ph.HECreated: 2026-09-09; Updated: 2026-09-11; Datestamp: 2026-09-11
Cosmic rays can significantly alter the abundances of certain species in the upper layers of planetary atmospheres, especially in terms of their biosignatures. To fully understand the extent of this effect, it is essential to accurately model the interactions of COSMIC RAYs with planetary MAGNETic fields. We used the CosmicTransmutation code to study the effect of a planetary MAGNETic field on the flux of galactic COSMIC RAYs and stellar energetic particles. We found that both particle sources are significantly affected by MAGNETic fields, even though the effects are different due to the varying energy ranges that characterize each source. The stellar energetic particle energy flux is significantly higher for an Earth-like planet with no MAGNETic field, but with a MAGNETic field of 30\,$μ$T or higher, the energy flux of the two sources becomes comparable. We find that the atmospheric pressures the COSMIC RAYs reach are significantly lower than those found in previous studies using simpler models and that the effect of the atmospheric composition on this outcome is small. We found similar results using the model for the exoplanet K2-18b, even though the radius is significantly larger than Earth's. Because the two COSMIC RAY sources cover different energy ranges and are affected by the MAGNETic field in different ways as a result, both sources should be considered. Future studies should focus on combining an accurate modelling procedure of the interaction between COSMIC RAYs and planetary MAGNETic fields with atmospheric chemistry models. This will require general circulation models to capture the latitudinal and longitudinal dependencies in full.
[abstract 30 / 40] (score: 2) - Title: Teglon: A Pixel-Level Pipeline for Galaxy-Informed Gravitational-Wave Follow-up Planning and Efficiency AnalysisAuthors: D. A. Coulter, P. Darc, C. D. Kilpatrick, R. J. Foley, P. McGill, S. D. Wyatt, R. Hausen,Comments: 21 pages, 6 figures, 3 tables; submitted to PASPSubjects: astro-ph.HE astro-ph.IMCreated: 2026-09-09; Updated: 2026-09-11; Datestamp: 2026-09-11
We describe Teglon, an open-source database and analysis pipeline engineered to optimize the search for electroMAGNETic (EM) counterparts to gravitational wave (GW) sources. Teglon constructs a 3D galaxy completeness metric from an input galaxy catalog and convolves it with the 3D localization volume of a GW event, producing an updated posterior map informed by known galaxy distributions. Using Teglon, users can ingest arbitrary instrument footprints --- or download them directly from the Treasure Map --- to generate dynamic observation plans that seamlessly interpolate between targeted galaxy pointing and region tiling. By focusing efforts on high-probability volumes, Teglon significantly reduces the predicted search area to find EM counterparts and increases observational efficiency, especially for small field-of-view (<= 1 deg^2) instruments like the Nancy Grace Roman Space Telescope. Furthermore, Teglon integrates with Redback to calculate pixel-level model detection efficiencies, enabling custom, event-specific observing strategies or retrospective detection efficiencies on an arbitrary grid of EM transient models. Teglon also supports custom science cases, such as prioritizing Active Galactic Nuclei searches for EM counterparts to binary BLACK HOLE mergers. Having supported Gravity Collective and related programs from the LIGO-Virgo-KAGRA third observing run (O3) through O4, Teglon is being continuously developed to support O5 and beyond. We document the public repository lineage and packaging, and provide Version 2.0 as an open-source tool for the community.
[abstract 31 / 40] (score: 2) - Title: Binary-BLACK HOLE spin population results may be driven by prior degeneraciesAuthors: Noah E. Wolfe, Asad Hussain, Jack Heinzel, Salvatore Vitale,Comments: 5 pages, 4 figures. Comments welcome!Subjects: gr-qc astro-ph.HECreated: 2026-09-09; Updated: 2026-09-11; Datestamp: 2026-09-11
Gravitational waves carry information on the spins of merging binary-BLACK HOLEs. The orientations of their spins relative to their orbits ("tilts")---while challenging to measure---differentiate the astrophysical formation mechanisms by which merging BLACK HOLE binaries may form. Multiple analyses have reported tentative evidence that BLACK HOLE spins are preferentially oriented in the plane of the binary orbit. We show that these results are likely extrapolated from more easily measurable "effective spin" parameters which characterize the gravitational-wave inspiral of BLACK HOLE binaries but may not uniquely constrain their astrophysical formation. In particular, we reproduce a peak in the spin tilt distribution with information about the marginal effective spin distributions alone. We propose a geometric picture to compare constraints on effective spins to standard population modeling assumptions, suggesting that current inferences of a preferred spin orientation are spurious.
[abstract 32 / 40] (score: 2) - Title: Low-Mass Magnetic Monopoles in the Galaxy: Simulations and Comparison with Ultra-High-Energy Cosmic-Ray DataAuthors: Ala'a AL-Zetoun, Igor Ostrovskiy, Peiwen Mi, Daniele Perri,Comments: 32 pages, 19 figuresSubjects: astro-ph.HE hep-ex hep-phCreated: 2026-09-09; Updated: 2026-09-11; Datestamp: 2026-09-11
Origin and composition of ultra-high energy COSMIC RAYs are still uncertain, particularly the rare events exceeding the Greisen-Zatsepin-Kuzmin cutoff and whose apparent arrival directions point to the Local Void. This work is an in-depth investigation of the possibility that such COSMIC RAYs contain low-mass MAGNETic monopoles predicted in several recent theoretical models. Using a custom extension to CRPropa, a state-of-the-art code for modeling COSMIC RAY propagation, monopoles are tracked in the galactic environment under realistic assumptions on mass, MAGNETic charge, and initial phase-space distributions. Our simulations demonstrate that relic MMs follow filamentary ``Galactic MAGNETic funnels'', producing anisotropic arrival directions at Earth. The expected arrival directions are concentrated in a small region of the sky, which has significant implications for the design and interpretation of future searches. A comparison of the simulated arrival directions with the Pierre Auger Observatory dataset shows that the null hypothesis - no monopole contribution - is statistically preferred for the majority of cases. Using a profile-likelihood analysis that incorporates both directional and energy information, we set 90% C.L. upper limits on the integral MM flux of $< 2.1\times10^{-23}$ $\mathrm{cm^{-2}s^{-1}sr^{-1}}$.
[abstract 33 / 40] (score: 2) - Title: The THRILS Factor: Investigating the properties of Little Red Dots (LRDs) at 3[abstract 34 / 40] (score: 2)Authors: Ananya Ganapathy, Rebecca L. Larson, Erini Lambrides, Guillermo Barro, Taylor A. Hutchison, Pablo Arrabal Haro, Anthony J. Taylor, Dale Kocevski, Casey Papovich, Steven L. Finkelstein, Anton M. Koekemoer, Jonathan R. Trump, Pablo G. Pérez-González, Weida Hu, Volker Bromm, Dan Coe, Kelcey Davis, Michaela Hirschmann, Nikko J. Cleri, Ray A. Lucas, Stephan R. McCandliss, L. Y. Aaron Yung, Jorge A. Zavala,Comments: 21 pages, 14 Figures, submitted to ApJSubjects: astro-ph.GACreated: 2026-09-09; Updated: 2026-09-11; Datestamp: 2026-09-11
JWST has uncovered a class of objects called LRDs, whose nature is still widely debated. In this work, we present a comprehensive spectroscopic analysis of nine LRDs in the Extended Groth Strip (EGS) field studied as part of THRILS and C3PO, both JWST Cycle 3 programs. These targets, photometrically selected based on their compact red appearance, are observed with deep spectroscopic exposures ($\geq8$ hours), enabling robust detections of broad Balmer lines, He I emission, and other spectral features characteristic of AGN activity. Using the [SII] $λ\lambda6716,6731$ doublet, we find electron densities ($n_e$) between $2.33 < \log (n_e) < 2.97 \ \mathrm{cm^{-3}}$, comparable to those in narrow line regions (NLR) of local AGN and high-$z$ galaxies. The spectroscopic depth further enables detailed characterization of broad Balmer line profiles. We fit both Gaussian and convolved exponential models to each source and find that five LRDs are statistically better described by the latter model. We measure optical depths $τ_{\rm sc} = 0.56-0.91$, scattering fractions $f_{\rm SC} = 0.40-0.82$ which correspond to column densities log(N$_e$) $\sim$ 23.93-24.14 cm$^{-2}$, and covering fractions $c_f = 0.43-0.59$. These results indicate a clumpier broad line region (BLR) geometry that deviates from conventional LRD models, which predict covering fractions close to unity. Furthermore, these Compton-thick gas columns may explain the X-ray weakness of LRDs. We also find that THRILS LRDs are narrow-line dominated compared to literature AGN-dominated LRDs, and show that exponential profile fitting corrects for systematic overestimation of BLACK HOLE masses from Gaussian-based measurements.
arXiv:2609.10845 [pdf, ps, other]XRISM has mapped gas velocities across the core of the Perseus cluster, separating the kinematic effects of mergers and AGN feedback. The physical properties of these motions remain unclear: are they a superposition of bulk flows, predominantly random/turbulent motions, or a mixture of both? Without resolving this question, constraints on the nonthermal pressure fraction and heating rate remain uncertain, as both assume predominantly random motions. Unlike emission line broadening, resonant scattering is most sensitive to small-scale, random motions rather than coherent bulk flows. Taking advantage of the extensive XRISM coverage of the Perseus cluster, we detect the full effects of resonant scattering on the Heα w line for the first time. This includes flux suppression in the cluster center, enhancement in the outer regions, and non-Gaussianity in the emission line. We employ radiative transfer simulations to constrain the amplitude of small-scale ICM velocities in the inner 60 kpc of Perseus, finding them to be consistent with the line broadening measurements within the uncertainties. This indicates the observed velocity dispersion is primarily due to small-scale random motions in the central Perseus regions rather than coherent bulk flows. We further explore potential anisotropy of these motions, showing that they are consistent with isotropic or radial motions rather than tangential ones. Longer XRISM observations are required to improve these anisotropy constraints. Finally, we explore azimuthal variations between the two complete radial arms observed by XRISM.
arXiv:2609.11068 [pdf, ps, other]Long-period transients are a class of periodic pulsed radio source repeating on the minute to hour timescale. Recently, an increasing number of them are being identified as binary systems, specifically white dwarfs with low-mass main-sequence companions. In this work we analyse the most luminous long-period transient discovered to date, ASKAP/DART J1832-0911, with two years of radio data, and propose that it, too, may be a white dwarf system, although in a far more compact orbit than the aforementioned. The pulses are composed of quasi-periodic components which evolve in a systematic way over days and months. The source is highly linearly or elliptically polarised and its brightness enabled very high signal-to-noise measurement of the time-resolved Faraday rotation measure, which was found to vary across pulse phase. The linear polarisation position angle, circular polarised fraction, and spectral index also varied systematically in ways not typical of pulsars and MAGNETars. We show that an ultra-compact asynchronous polar explains much of the phenomenology of ASKAP/DART J1832-0911, in particular the evolution of the pulse morphology, rotation measure variation, and periodic X-ray emission, although we cannot conclusively prove a binary nature. However, our model makes testable predictions.
arXiv:2609.11487 [pdf, ps, other]The C IV $λ\lambda1548,1551$ resonance doublet is a key tracer of warm gas ($T\sim10^5\,{\rm K}$) within and around galaxies. Recent observations have detected this line in both absorption and emission, revealing asymmetric profiles in galaxies and spatially extended haloes around ACTIVE GALACTIC NUCLEi (AGNs). Resonance scattering can strongly modify the emergent spectra and spatial distributions, complicating their interpretation. Using 3D Monte Carlo radiative transfer simulations, we study C IV resonance scattering over a broad range of column densities, intrinsic emission-line widths, and outflow velocities. We find that multiple scattering broadens the line profile and, in outflowing media, modifies the doublet ratio, $R_{\rm CIV}$, defined as the flux ratio of the K and H components at 1548 and 1551 $\mathrm{\mathring{A}}$, respectively. When the outflow velocity approaches or exceeds the doublet separation ($\simeq500\,{\rm km\,s^{-1}}$), K-line photons are redistributed around the H component, driving $R_{\rm CIV}$ below its intrinsic value and, in optically thick fast outflows, even below unity. We also combine photoionization models with resonance scattering to investigate extended C IV haloes around AGNs and compare them with He II $\lambda1640$ emission. Simple photoionization models do not produce C IV emission more extended than He II, whereas resonance scattering redistributes locally produced and central-source C IV photons to larger radii. These results demonstrate that the C IV doublet ratio and spatial distribution provide complementary diagnostics of warm gas.
arXiv:2609.11629 [pdf, ps, other]We produce a diverse set of observed core-collapse SUPERNOVA (CCSN)-type morphologies using a precessing pair of opposite JETs within the jittering-JETs explosion mechanism (JJEM) framework. We conduct a three-dimensional hydrodynamical simulation of a precessing pair of JETs that explode a massive star, and find that a single precessing pair of opposite JETs can generate S-shaped structures, pipe-spout-blowout features as observed in the Cygnus Loop, multiple apparent pairs of opposite protrusions similar to some morphological features in S147, and H-shaped structures with a prominent bar, similar to the one observed in the 3C 397 remnant. At small scales, the JETs form clumps and filaments, resulting from instabilities and vortices that the JETs induce in the ejecta as they interact with the stellar material. We did not aim the simulation to reproduce any particular CCSN remnant, but rather to explore the resulting morphological features. Our finding of simulated features similar to observed ones supports the role of JETs in exploding CCSNe and, in turn, supports the claim that the JJEM is the primary explosion mechanism of CCSNe.
arXiv:2609.11738 [pdf, ps, other]Quantum field theory on curved and non-inertial backgrounds contains background- and foliation-dependent quantities in the canonical Lagrangian, the hypersurface inner product and bilinear form, as well as in the equal-time anti-commutation relations. In this work, we determine a local fermion-field redefinition that brings these canonical structures into their standard-Minkowski forms, i. e., the forms they assume in Cartesian inertial coordinates on Minkowski spacetime, where the zeroth world coordinate is identified as the coordinate of time. Starting from the generally covariant Dirac action minimally coupled to a spin-1 gauge field, we derive the corresponding Lagrangian, fermionic inner product, and quantization rule in an Arnowitt-Deser-Misner decomposition, formulated in arbitrary world coordinates. We identify the generalized temporal gamma matrix as the common geometric factor governing the canonical temporal structure of all three quantities. Using a field redefinition, we transform this generalized temporal gamma matrix to its standard-Minkowski form, thereby mapping the fermionic inner product and the equal-time anti-commutation relation to their standard-Minkowski expressions, while transferring the explicit background and foliation dependence to the transformed Lagrangian and fermion-field operators. We show that such a field redefinition necessarily consists of a local rescaling and a fixing of the local Lorentz frame. This procedure restores the conventional canonical normalization from standard-Minkowski spacetime used for fermionic mode quantization and occupation-number operators. The transformed Lagrangian consequently assumes a generalized first-order Schrödinger form, leading to the familiar rest-energy term and spacetime-MAGNETic couplings, as well as to the leading non-RELATIVISTIC limit, in which temporal derivatives are separated from spatial ones.
arXiv:2609.11902 [pdf, ps, other]We compute the energy gained by accretion onto a compact star due to matter falling from the inner edge of a thin accretion disk. We employ a controlled slow-rotation expansion based on the Hartle-Thorne metric and find that in neutron stars in general only leading order rotational corrections to the metric, describing frame dragging, are sizable. However, for accretion onto a MAGNETized neutron star, where the disk roughly extends to the co-rotation radius, even frame dragging effects are minor. Based on general conservation laws we then derive simple, equation-of-state-independent expressions for the spin-up and heating energy, consistently including the relevant rotational, RELATIVISTIC and nuclear effects, and find that in observed accreting millisecond sources the results can strongly deviate from presently employed estimates.
arXiv:2609.11921 [pdf, ps, other]Title: Teleparallel torsion and white dwarf structure in \(f(T)=T+ΞT^2\) gravityAuthors: Edson Otoniel, Jonathan A. Reboucas, Iarley P. Lobo,Comments:Subjects: astro-ph.SR astro-ph.HECreated: 2026-09-10; Updated: 2026-09-11; Datestamp: 2026-09-11We investigate how quadratic torsion modifies the equilibrium structure of white dwarfs in covariant $f(T)=T+ΞT^2$ gravity. Static spherical configurations are calculated with a fixed equation of state for cold carbon matter, including RELATIVISTIC electron degeneracy and Coulomb lattice corrections. The stellar interior is matched to a vacuum exterior, and the mass is determined from the asymptotic geometry. At fixed central density, negative couplings produce more massive and more compact configurations than general relativity, whereas positive couplings give smaller masses and larger radii. The deviations increase with central density and are more pronounced in mass than in radius. The first limiting feature of each sequence depends on the coupling. For $Ξ=-10^{18}\,\mathrm{cm}^{2}$, the sequence remains monotonic up to the electron capture density and reaches $1.508\,M_\odot$. General relativity and $Ξ=+10^{18}\,\mathrm{cm}^{2}$ instead reach mass turning points at $1.385\,M_\odot$ and $1.366\,M_\odot$, respectively. The positive extreme can be continued as an equilibrium solution to the capture density, where its mass decreases to $1.24\,M_\odot$, but this configuration lies beyond the turning point and is not the maximum mass along that sequence. These results identify a density dependent structural response to torsion that changes the stellar mass scale without modifying the matter equation of state.
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