Current date: 2026-10-16
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Scoring abstracts
Number of records retrieved: 806
Keyword score statistics
score 10 -- 1 abstracts
score 8 -- 1 abstracts
score 7 -- 1 abstracts
score 6 -- 1 abstracts
score 4 -- 9 abstracts
score 3 -- 9 abstracts
score 2 -- 21 abstracts
in total -- 43 abstracts
Articles that appeared on 2026-10-16
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[abstract 1 / 43] Wow! (score: 10)
- Title: mm-JETs in the multi-messenger eraAuthors: Karri I. I. Koljonen, Thomas D. Russell, Britton Jeter, Lauren Rhodes, Alexandra J. Tetarenko, María Díaz Trigo, Talvikki Hovatta, Pau Bosch-Cabot, Mamta Pandey-Pommier, Alessio Marino, Jakob van den Eijnden, Dieu D. Nguyen, Melania Del Santo, Thomas Maccarone, Anna Y. Q. Ho, Maria C. Baglio, Sera Markoff, the ALMA2040 Transient, Time-Domain Astronomy working group,Comments: Part of the ALMA2040 White Paper Series. 10 pages, 2 figuresSubjects: astro-ph.HE astro-ph.IMCreated: 2026-10-14; Updated: 2026-10-16; Datestamp: 2026-10-16
Jets and outflows operate across the full cosmic mass scale from young stellar objects (YSOs) and X-ray binaries (XRBs) to ACTIVE GALACTIC NUCLEi (AGN), GAMMA-RAY BURSTs (GRBs), and tidal disruption events (TDEs), shaping many time-domain and multi-messenger transients. Key questions concern on how JETs are launched, accelerated and collimated; where and how they dissipate energy and accelerate particles; and how they couple to their environments to set electroMAGNETic counterpart diversity and feedback. Millimeter and sub-millimeter observations uniquely address these questions by tracking the evolving SYNCHROTRON turnover for robust calorimetry and Lorentz-factor constraints, providing full-Stokes POLARIZATION and Faraday diagnostics close to the JET base, and enabling high-resolution imaging from Galactic ejecta to event-horizon-scale AGN JET bases via global Very Long Baseline Interferometry (VLBI). We describe the JET and outflow science enabled by ALMA2040, a next-generation mm/sub-mm interferometer combining an order-of-magnitude sensitivity gain with rapid-response observing, simultaneous multi-band coverage, full-Stokes polarimetry, and integration with global VLBI networks. These capabilities will enable statistically controlled, trigger-driven samples spanning XRB outbursts, early GRB afterglows, protostellar disk winds and JET launching, AGN JET bases, and JETted TDEs, establishing mm/sub-mm astronomy as a cornerstone of time-domain and multi-messenger JET physics in the 2040s and beyond.
[abstract 2 / 43] Wow! (score: 8) - Title: FUGUE: A New GPU-accelerated General Relativistic Magnetohydrodynamics Code with Weak-Field Multipole Self-Gravity and Quasi-Stationary Kerr Black Hole EvolutionAuthors: Piotr Plonka, Agnieszka Janiuk,Comments: 25 pages; 19 figures; In press in ApJ Supplement Series; comments welcomeSubjects: astro-ph.HECreated: 2026-10-14; Updated: 2026-10-16; Datestamp: 2026-10-16
We present FUGUE, a new GPU-accelerated code for general RELATIVISTIC MAGNETohydrodynamics (GRMHD). The code supports an optional quasi-stationary update of the Kerr BLACK HOLE mass and spin, as well as weak-field multipole self-gravity computed with a spherical harmonic Poisson solver. The calculations using high-order multipoles in the Poisson solver are expensive, so the self-gravity solver is well suited for GPU acceleration. The code uses shock-capturing methods and a second-order Runge--Kutta (RK2) scheme for time integration. We validate the code with hydrodynamic, MAGNETohydrodynamic, general RELATIVISTIC, and convergence tests for the self-gravity module. We present an application of the code to a simulation of a self-gravitating, Toomre-unstable, MAGNETized accretion disk with a mass of 1,M-Sun around a Kerr BLACK HOLE. In our demonstration model, gravitational instabilities are associated with changes in the mass accretion rate and the Blandford--Znajek luminosity, and may contribute to GAMMA-RAY BURST variability.The performance of the code is equivalent to or exceeds that of the current state-of-the-art GRMHD codes, achieving more than 470 million zone-cycles per second on a single NVIDIA GH200 GPU with linear reconstruction.
[abstract 3 / 43] Wow! (score: 7) - Title: A model for the image structure and spectral energy distribution of RELATIVISTIC JETsAuthors: Dominic W. Pesce, Ramesh Narayan, Yuh Tsunetoe,Comments: 37 pages, 12 figures, submitted for publication in ApJSubjects: astro-ph.HECreated: 2026-10-14; Updated: 2026-10-16; Datestamp: 2026-10-16
Upcoming advances in high-frequency VLBI promise to enable spatially resolved studies of astrophysical JETs across an increasingly large source population. We present here a Python implementation of the semi-analytic model from Tsunetoe et al. (2025) for self-consistently interpreting the spatial and spectral structure of the SYNCHROTRON emission from such JETs. The model is based on an axisymmetric force-free JET solution supplemented with a prescription for nonthermal electron heating, SYNCHROTRON cooling, pitch-angle anisotropy in the electron distribution, and radiative transfer along straight rays. We use this model to explore how the predicted spectral energy distribution depends on the model parameters, identifying approximately self-similar scalings with BLACK HOLE mass, accretion rate, and electron heating efficiency. We also compare the model predictions against observations of M87 and Sgr A*. For M87, a single fiducial parameter set qualitatively reproduces VLBI images across multiple frequencies and matches the observed longitudinal intensity profile, while also yielding a broadband SED that is quantitatively consistent with the observed radio through X-ray measurements. For Sgr A*, a fit to the quiescent-state SED demonstrates that emission from a collimated JET with comparable nonthermal heating efficiency to M87's is quantitatively consistent with the observed radio through X-ray measurements, predicting a compact JET whose radio size decreases inversely with frequency, consistent with VLBI constraints.
[abstract 4 / 43] Yes (score: 6) - Title: Are $E>B$ regions essential for particle injection in RELATIVISTIC MAGNETic RECONNECTion?Authors: Omar French, Fan Guo, Xiaocan Li, Qile Zhang, Yi-Hsin Liu, William Daughton, Hui Li,Comments: 10 pages, 6 figures, 2 tables, submitted to MNRASSubjects: astro-ph.HE physics.plasm-phCreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
During RELATIVISTIC MAGNETic RECONNECTion, X-points ($E>B$ regions at vanishing guide field) have been proposed to play an essential role in injecting particles into the nonthermal population. Using fully kinetic particle-in-cell simulations at a range of MAGNETizations $σ\equiv B_0^2/(4πn_0 m_e c^2) = 12$--$800$, we study in detail how the particle energy gains up to the injection threshold $γ_{\rm inj} = σ/4$ are partitioned into work done inside $E>B$ regions (unMAGNETized), within one gyration after exit (re-MAGNETizing), and at all other times (MAGNETized). The MAGNETized channel supplies the largest part of the energy gain for $\sim 95\%$ of injected tracers at $σ= 12$ and $\sim 65\%$ at $σ= 800$. Most of the tracers in this MAGNETized majority never enter an $E>B$ region before injection. We also compare these injection shares with the earlier studies that proposed an essential role for $E>B$ regions. We conclude that $E>B$ regions are neither necessary for injection nor the dominant direct contributors to pre-injection work by injection share in two-dimensional, nonradiative pair-plasma RECONNECTion at vanishing guide field.
[abstract 5 / 43] Yes (score: 4) - Title: Multi-phase investigation of outflows in the circumgalactic and interstellar media of luminous QUASARs at z~5Authors: Matilde Brazzini, Valentina D'Odorico, Manuela Bischetti, Chiara Feruglio, Guido Cupani, George Becker, Roberta Tripodi,Comments: 19 pages, 14 figures. Published in A&ASubjects: astro-ph.GACreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
Aims. Outflows from ACTIVE GALACTIC NUCLEi are invoked as the principal feedback process regulating the co-evolution of supermassive BLACK HOLEs and their host galaxies. Because of their multi-phase and multi-scale nature, an exhaustive description of these winds should exploit multiple tracers. However, connecting various outflow features remains a challenge. The aim of this work is to provide a complete characterisation of outflows in a sample of z~5 QUASARs, by exploiting the combination of different emission and absorption tracers. Methods. We analysed the UV/optical and FIR continuum, line emission, and absorption in a sample of 39 z~5 QUASARs observed with VLT/X-Shooter and ALMA (available for six objects). We identified broad and narrow absorption lines associated with the QUASAR and emission lines to determine BLACK HOLE masses and bolometric luminosities. Results. Our sample encompasses massive (log(M_BH,MgII / M_sun) = 8.5-10) and luminous (log(L_bol/(erg/s)) = 46.9-48) QUASARs at redshift 5.0-5.7. They display powerful ionised outflows detected in both emission and absorption, with velocities exceeding 48,000 km/s in some cases, and lie above the local BLACK HOLE-host galaxy mass relation, exhibiting a behaviour similar to that of z~6 QUASARs. These findings suggest a phase of efficient BLACK HOLE feedback occurring at redshift z~6 and likely persisting down to z~5, characterised by rapid BLACK HOLE growth exceeding that of the host galaxy. The fraction of QUASARs with outflow detections in absorption is higher for larger CIV-MgII velocity shifts, suggesting that while the physical mechanisms powering the two outflow phenomena detected in emission and absorption may differ, a correlation exists between them.
[abstract 6 / 43] Yes (score: 4) - Title: A grid of fast-rotating, chemically-homogeneous, SUPERNOVA and/or long-GRB progenitorsAuthors: M. Renzo, O. Gottlieb, H. S. Chan, J. A. Goldberg, A. Grichener, K. Sen, N. Shah, E. Farag, Matteo Cantiello,Comments: accepted by ApJS, data available at https://zenodo.org/records/14286306, reproducible at https://github.com/mathren/CHE_LGRB_progenitorsSubjects: astro-ph.HE astro-ph.SRCreated: 2026-10-14; Updated: 2026-10-16; Datestamp: 2026-10-16
The understanding of the mechanism(s) by which massive stars collapse and possibly explode is rapidly maturing. Uncertainties in the structure of the stellar core at the onset of collapse are often dominant in numerical simulations, and a limited number of progenitor grids are available. This is especially true for explosions where rotation and MAGNETic fields play a significant or primary role. We present a grid of 113 single-star models with initial masses $M_{\rm ZAMS}=30-90\,M_{\odot}$ and initial rigid rotation $ω_{\rm ZAMS}=0.5-0.99\,ω_{\rm crit}$ computed at $Z=0.001$ with the open-source stellar evolution code \textsc{MESA}. We adopt a 128-isotope nuclear reaction network capable of following the weak reactions deleptonizing the core during and after silicon core burning. By construction, these models experience rotationally-induced chemically-homogeneous evolution, and reach the onset of collapse ($v_{\rm infall}\lesssim -300\,\mathrm{km\ s^{-1}}$) with large and structured amounts of angular momentum, possibly sufficient to form accretion disks on a proto-compact object. Therefore, these progenitor structures provide a homogeneous set of models with updated input physics and improved algorithmic accuracy to understand stellar explosions of (some types of) stripped-envelope SUPERNOVAe, possibly JETted and/or broad-lined, collapsars or MAGNETar-powered, and/or long $γ$-ray bursts.
[abstract 7 / 43] Yes (score: 4) - Title: The energetic atmosphere of the SunAuthors: Sven Wedemeyer, Mats Kirkaune, Miroslav Barta, Astrid M. Veronig, Stanislav Gunar, Roman Brajsa, Manuela Temmer, Valery Nakariakov, Stephen White, Bart De Pontieu, Maryam Saberi, Atul Mohan, Masumi Shimojo, Davor Sudar, Galina Motorina, Maria Loukitcheva, Paulo Simoes, Stefaan Poedts, Raghavendra Sahai,Comments: Part of the ALMA2040 White Paper SeriesSubjects: astro-ph.IM astro-ph.SRCreated: 2026-10-14; Updated: 2026-10-16; Datestamp: 2026-10-16
Understanding the mechanisms that heat the Sun's chromosphere and corona to temperatures far exceeding those of the solar photosphere below remains one of the central challenges in solar physics. Small-scale, rapidly evolving processes - including shocks, turbulence, MAGNETohydrodynamic waves, RECONNECTion-driven JETs, and nano-flares - are thought to contribute significantly to the heating budget. However, direct observational constraints on their spatial, temporal, and spectral signatures remain hard to obtain. At millimeter wavelengths, optically thick thermal emission provides a comparatively direct measure of gas temperature. While the Atacama Large Millimeter/submillimeter Array (ALMA) already provides unique diagnostic capabilities, offering temperature diagnostics and high-cadence imaging, the current capabilities are still limiting the study of such dynamic, small-scale phenomena. Improved spatial resolution, enhanced uv-coverage, and simultaneous multi-band observations, as proposed for ALMA2040, would enable transformative progress in capturing dynamic processes across multiple heights and enable time-dependent three-dimensional thermal and MAGNETic tomography of the chromosphere. Combined with complementary diagnostics and simulations, these measurements would test how small-scale processes contribute to atmospheric heating.
[abstract 8 / 43] Yes (score: 4) - Title: JWST reveals a highly ionized nebula powered by an ultraluminous X-ray source with a massive BLACK HOLE in the metal-poor galaxy Holmberg IIAuthors: F. A. Fogantini, P. Zeidler, L. M. Oskinova, T. Bao, W. -R. Hamann, P. Marchant, D. M. -A. Meyer, D. Pauli, S. Reyero Serantes, A. A. C. Sander, T. Shenar, R. Soria,Comments: 9 pages, 5 figuresSubjects: astro-ph.GA astro-ph.HECreated: 2026-10-14; Updated: 2026-10-16; Datestamp: 2026-10-16
Recent James Webb Space Telescope (JWST) observations have revealed fine-structure lines of ions with ionization potentials ${\gtrsim}50$\,eV, such as [Ne\,{\sc v}] and [O\,{\sc iv}], in nebular spectra of some low-metallicity galaxies, raising questions about the nature of the ionizing sources. Ultraluminous X-ray sources (ULXs) have been considered as potential contributors, but direct evidence linking individual ULXs to highly ionized nebulae is limited. Here we present JWST IFU spectroscopy of the nebula surrounding the template ULX Ho\,II\,X--1 in the low-metallicity galaxy Holmberg\,II, already known to emit He\,{\sc ii}\,$\lambda4686$ and [O\,{\sc iv}]\,25.89\,$μ$m lines. We resolve the infrared nebula on spatial scales of ${\sim}15-25$\,pc and report the first detections of [Ne\,{\sc v}] and [Ne\,{\sc vi}] in this source. We find anisotropic ionizing conditions: emission from the highest-ionization species arises from compact regions offset from the ULX toward the previously detected radio knots, whereas lower-ionization species trace the wider nebula. The preferential alignment of the highest-ionization emission with the radio axis suggests anisotropic escape of the ionizing continuum and a physical connection with JET-ejection activity. Spectral lines across the nebula are narrow and consistent with the instrumental resolution, indicating kinematically quiescent gas and disfavoring shocks as the dominant ionization mechanism. Together, these results provide direct evidence linking an individual ULX to a highly ionized nebula in a low-metallicity galaxy. These JWST observations of Ho~II~X--1 show that an accreting BLACK HOLE in a low-metallicity galaxy is responsible for the extreme ionization of the surrounding nebula on ${\sim}100$\,pc scales.
[abstract 9 / 43] Yes (score: 4) - Title: Detecting and Identifying Supernovae in AGN Accretion DisksAuthors: Zhi-Peng Ma, Kai Wang,Comments:Subjects: astro-ph.HE astro-ph.GACreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
Stars may become embedded in ACTIVE GALACTIC NUCLEus (AGN) accretion disks and eventually explode as SUPERNOVAe (SNe), whose detection would provide direct evidence for the existence and evolution of stars in AGN disks. We investigate the electroMAGNETic emission of such disk SNe using an analytic shock dynamics model coupled with a one-zone radiation model. Applying this framework to four progenitor types over a range of AGN BLACK HOLE masses and Eddington ratios, we find that disk SNe around lower-mass BLACK HOLEs (BHs) or at lower Eddington ratios are more readily detectable against the underlying AGN emission and can remain detectable over a broader range of electroMAGNETic bands, from the infrared to soft X-rays. However, detectability against the AGN background does not guarantee that disk SNe can be distinguished from isolated SNe with CSM interaction. We therefore further compare disk SNe with isolated SNe with and without CSM interaction and find substantial degeneracies in their macroscopic observables. Nevertheless, we identify distinctive signatures that are robust across progenitor types. The characteristic emission shifts from the EUV for \(M_{\rm BH}\lesssim10^7\,M_\odot\) toward the UV/optical for \(M_{\rm BH}=10^8\,M_\odot\), with the visibility timescale increasing from less than a day to \(\sim3\text{--}70\) days and \(T_{\rm peak}\sim3\text{--}8\) eV in the latter case. The UV/optical regime around \(10^8\,M_\odot\) BHs therefore offers particularly promising prospects for detecting disk SNe.
[abstract 10 / 43] Yes (score: 4) - Title: Neutrino production at the extreme vicinity of supermassive BLACK HOLE in NGC 1068Authors: Zhi-Peng Ma, Kai Wang,Comments:Subjects: astro-ph.HECreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
The identification of NGC~1068 as an extragalactic high-energy neutrino source raises the question of the physical conditions required for neutrino production. Motivated by the newly updated IceCube data (down to $\sim 0.2 \,\rm TeV$) for NGC 1068, we present a statistical, model-independent inference primarily constrained by the multi-messenger observations. We calculate neutrino production from hadronic channels (including hadronuclear and photomeson processes) and the accompanying cascade gamma rays, and then employ the Latin hypercube sampling (LHS) method to explore the parameter space comprehensively, constrained by observational data. According to our results, the emission region is tightly limited: $R \gtrsim 10\,R_{\rm s}$ is excluded at $\sim 5σ$, and $R \gtrsim 6\,R_{\rm s}$ at $\sim 3σ$, where $R_{\rm s}$ is Schwarzschild radius of supermassive BLACK HOLE (SMBH). Furthermore, reproducing $\gtrsim 80\%$ of the observed neutrino flux further restricts the emission to $R \lesssim 3R_{\rm s}$. Finally, we explore the possible particle acceleration mechanisms and find that stochastic acceleration naturally satisfies all constraints, whereas alternative mechanisms require extreme, fine-tuning parameters. We therefore identify stochastic acceleration as the most viable origin of the neutrino emission from NGC~1068.
[abstract 11 / 43] Yes (score: 4) - Title: A ${}^{13}$CO Detection in a Massive Molecular Gas Flow in Abell 1795's Central GalaxyAuthors: J. A. Gray, H. R. Russell, F. Combes, O. Almaini, P. E. J. Nulsen, A. C. Fabian, B. R. McNamara, T. Rose, P. Salomé,Comments: 11 pages, 4 figures, accepted for publication in MNRASSubjects: astro-ph.GACreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
We present new ALMA ${}^{13}$CO(2-1) observations of the central galaxy in the cool-core cluster Abell 1795, targeting the origin of extended molecular filaments. The filaments extend for 5--7 kpc and are closely drawn up around large radio bubbles inflated by JETs from the central ACTIVE GALACTIC NUCLEus (AGN). Smooth velocity gradients along their lengths are consistent with entrained flows lifted by the expanding bubbles. Here we detect the northern molecular filament in the low-opacity molecular tracer ${}^{13}$CO(2-1), which can provide a more reliable measure of the molecular gas mass and conditions than ${}^{12}$CO. The velocity structure in ${}^{13}$CO(2-1) is consistent with that of the ${}^{12}$CO(2-1) emission. Using a range of plausible excitation temperatures and covering fractions, we thereby determine a filament molecular gas mass of (0.1--2) $\times \ 10^9 \ \text{M}_\odot$, or down to an order of magnitude below previous estimates. This implies a CO-to-H$_2$ conversion factor of $α_\text{CO} =$ 0.4--5 $\ \text{M}_\odot $ (K km s$^{-1}$ pc$^2)^{-1}$ in the filament, or $\sim$ 0.1--1 times the standard assumption of the Milky Way value. Direct entrainment by the N radio bubble is now plausible, as it can provide sufficient mechanical energy and buoyant support for the molecular gas flow. Similarly, measured X-ray cooling rates are also now consistent with in-situ condensation of uplifted, low-entropy hot gas. Both formation mechanisms require multiple generations of bubbles at higher filament masses.
[abstract 12 / 43] Yes (score: 4) - Title: X-ray point sources towards the giant radio lobes of Centaurus AAuthors: Karthik Balasubramaniam, Hsiang-Kuang Chang, Łukasz Stawarz, Volodymyr Marchenko,Comments: 15 pages, 8 figures, 8 tables. Submitted to A&A. The 185-source catalogue is provided as ancillary filesSubjects: astro-ph.HECreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
Centaurus A (NGC 5128) is the nearest RADIO GALAXy (d = 3.8 Mpc), so individual X-ray point sources can be resolved against its giant radio lobes. We test whether a compact X-ray source population over the lobes exceeds the expected field population, once the selection function, foreground stars and the cosmic X-ray background (CXB) are accounted for. From five Chandra/ACIS-I lobe pointings we build a 0.5-7 keV catalogue of 185 sources, with Bayesian hardness ratios, Gaia DR3 and AllWISE counterparts, and spectral fits to the eight brightest. The hardness-ratio distribution (median -0.17; 80% of sources below N_H = 10^22 cm^-2) is that of background AGN plus a few foreground stars. Above the flux at which half the footprint is covered, the good sample holds 83 sources, 9 of them foreground stars, against 101 expected background sources: 27% below the expectation (-1.5 sigma including a 15% normalisation uncertainty), with no excess. The 90% upper limit on a lobe-associated excess above 6.9x10^36 erg/s is N_lobe < 18, or < 38 for a conservative 30% normalisation uncertainty. With the usual resolved-source masking and CXB subtraction, no additional lobe-associated correction to diffuse-emission or inverse-Compton measurements is indicated.
[abstract 13 / 43] Yes (score: 4) - Title: High-frequency water megamasers as precision probes of BLACK HOLEs, galaxies and cosmology: A case for a next-generation sub-mm/mm interferometerAuthors: Ingyin Zaw, C. M. Violette Impellizzeri, Dominic W. Pesce, Elizabeth Humphreys, Hannah R. Stacey, Sophie Venselaar, Chengyu Kuo, Jack Gallimore, Yoshiaki Hagiwara, Satoki Matsushita, Jim Braatz,Comments: Part of the ALMA2040 White Paper SeriesSubjects: astro-ph.IM astro-ph.CO astro-ph.GACreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
Water megamasers in the circumnuclear disks of ACTIVE GALACTIC NUCLEi are among the most precise probes of supermassive BLACK HOLEs. VLBI imaging of 22 GHz disk masers has provided geometric distances to independently constrain $H_0$, accurate BLACK HOLE mass measurements, and sub-parsec views of accretion disk geometry. ALMA has opened a new window into water maser transitions in the sub-mm/mm regime, which trace temperatures, densities and disk regions that are inaccessible at 22 GHz, and can be observed at higher spatial resolution and with less free-free absorption. However, current detections are limited to a few bright extragalactic masers in nearby galaxies. We present the case for a next-generation sub-mm/mm interferometer - ALMA2040 - that would open a new parameter space for maser studies. We show that a 10-fold increase in line sensitivity and three times longer baselines compared to ALMA would transform sub-mm maser studies from a few bright detections into a population-level probe, delivering BLACK HOLE masses and geometric distances from sub-mm masers alone, independent of and complementary to 22 GHz measurements. Integrated into a VLBI array, ALMA2040 would resolve maser disks out to $>$160 Mpc, extend maser BLACK HOLE masses into the largely untested intermediate-mass regime, reveal MAGNETic field structure in accretion disks through POLARIZATION studies, and test systematics in $H_0$ measurements.
[abstract 14 / 43] (score: 3) - Title: Gravitational light deflection and shadows in a warm plasmaAuthors: Barbora Bezděková, Volker Perlick,Comments: 30 pages, 22 figuresSubjects: gr-qcCreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
Analytical studies of light bending in a dispersive medium near compact objects, e.g., BLACK HOLEs or neutron stars, are most challenged by a suitable definition of the medium. The most realistic model would be a hot MAGNETized plasma. In such a medium, however, an analytical description of light rays is very difficult. Therefore, usually an isotropic dispersive medium is assumed in analytical calculations. While it is possible to formulate equations for a general refractive index, which some studies do, most attention in the literature is given to the particular case of a cold, non-MAGNETized electron-ion plasma. Whereas this model covers many astrophysically relevant situations, there are indications that in some cases the plasma temperature is so high that the approximation of a cold plasma is no longer valid. For this reason, we consider in this paper a warm, non-MAGNETized electron-ion plasma, where the temperature is not set equal to zero but assumed to be small enough, such that relevant equations can be linearized with respect to it. After discussing the general equations for light rays in such a medium on a general-RELATIVISTIC spacetime, we specify to the axially symmetric and stationary case which includes the spherically symmetric and static case. In particular, we calculate the influence of a warm plasma on the bending angle. In the spherically symmetric and static case, we also calculate the shadow in a warm plasma. We illustrate the general results with a static (respectively corotating) and an infalling warm plasma on Schwarzschild and Kerr spacetimes.
[abstract 15 / 43] (score: 3) - Title: FERMI Acceleration Mechanisms Beyond Lorentz SymmetryAuthors: Gilson A. Ferreira, Erick Aguiar, A. A. Araújo Filho, Edson Otoniel, Valdir B. Bezerra, Iarley P. Lobo,Comments: 23 pages. Matches published versionSubjects: gr-qcCreated: 2026-10-14; Updated: 2026-10-16; Datestamp: 2026-10-16
We construct models for first- and second-order FERMI acceleration of particles, incorporating generic frame transformations, dispersion relations, and conservation laws. Within this framework, we study deformations of Lorentz symmetry via the $κ$-Poincaré algebra in the bicrossproduct and classical bases, which respectively deform and preserve the RELATIVISTIC dispersion relation. We also examine explicit Lorentz symmetry violation and compare the results with deformed relativity and special relativity. The energy spectra present different shapes when one considers deformation or violation of Lorentz symmetry in superluminal or subluminal scenarios. One of the possible outcomes is an intense decay of the spectrum for higher energies. We also gather the predictions of all the scenarios considered, comparing the spectra produced at the source in the energy domain, which is the variable in which COSMIC RAY observatories report their measurements.
[abstract 16 / 43] (score: 3) - Title: The impact of nonlinear Landau damping on COSMIC RAY streaming and the role of external turbulenceAuthors: Rouven Lemmerz, Mohamad Shalaby, Ellen Zweibel, Christoph Pfrommer, Timon Thomas,Comments:Subjects: astro-ph.HE astro-ph.GA physics.plasm-phCreated: 2026-10-14; Updated: 2026-10-16; Datestamp: 2026-10-16
Cosmic rays (CRs) streaming faster than the Alfvén speed generate Alfvén waves that scatter them. The saturated wave amplitude is regulated by a damping mechanism. This damping controls the CR scattering rate and drift velocity, and thus the rate at which CRs transfer momentum and energy to the ambient plasma, which sets the strength of CR feedback. In the ionized interstellar medium, nonlinear Landau damping (NLLD) is commonly invoked as the dominant damping mechanism for Alfvén waves. We test this assumption with fluid-PIC simulations in which thermal ions and electrons are modeled as fluids with optional Landau closures, allowing us to compare otherwise identical runs with and without NLLD. When waves are self-generated by monoenergetic CRs, runs with and without Landau closures are indistinguishable: NLLD is inefficient and the CRs isotropize in the wave frame. Once high-amplitude Alfvén waves mimicking external turbulence are seeded, NLLD curbs wave growth and equalizes forward- and backward-propagating waves. We show that the saturated drift velocity, which falls below the Alfvén speed, can be accurately predicted from the wave spectra alone. If the CR distribution is undersampled, a numerical instability corrupts the largest resonant scales: unphysical, unresolved pitch-angle gradients resonantly generate backward-propagating waves, driving an inverse cascade that should be absent from purely streaming-driven waves. While power-law CR distributions may permit stronger NLLD, our results indicate that NLLD is unlikely to be an intrinsic saturation mechanism of the streaming instability; instead, its effectiveness hinges on the interplay of streaming-generated modes with those of external origin.
[abstract 17 / 43] (score: 3) - Title: Understanding cosmic explosionsAuthors: Karri I. I. Koljonen, Tomek Kamiński, Anna Y. Q. Ho, Thomas Maccarone, Aneurin Evans, María Díaz Trigo, Thomas D. Russell, Dieu D. Nguyen, Dirk Petry, Jakob van den Eijnden, Tanmoy Laskar, Laura Chomiuk, the ALMA2040 Transient, Time-Domain Astronomy working group,Comments: Part of the ALMA2040 White Paper Series. 10 pages, 2 figures, 1 tableSubjects: astro-ph.IM astro-ph.HECreated: 2026-10-14; Updated: 2026-10-16; Datestamp: 2026-10-16
Millimeter-wavelength observations provide a uniquely sensitive window into the physics of cosmic explosions, from SUPERNOVAe (SNe) and tidal disruption events (TDEs) to nova eruptions, stellar mergers and electroMAGNETic counterparts to gravitational wave (GW) sources. Over the past decade, discoveries across the transient sky have revealed that many of the most informative phases of shock interaction, particle acceleration and JET formation unfold at frequencies above the traditional cm-wave domain, where SYNCHROTRON self-absorption weakens and thermal, nonthermal and dust components can be disentangled. Upcoming wide-field mm surveys will detect a new population of short-lived transients but will be limited by coarse localization and limited spectral characterization. ALMA2040, with dramatically improved sensitivity, wide instantaneous spectral coverage, rapid-response and sub-arraying modes, polarimetry and extended baselines, is essential for converting these discoveries into robust physical constraints. Here we outline the scientific context, key open questions and the ALMA2040 capabilities required to unlock the full potential of millimeter time-domain astrophysics in the 2040s.
[abstract 18 / 43] (score: 3) - Title: Aluminum wide-range EOS sensitivity in Z-pinch dynamic-hohlraum liner-foam impact and outgoing radiationAuthors: Cong Wang, Zi Li, Weijie Li, Xianjue Peng,Comments:Subjects: physics.plasm-phCreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
In a Z-pinch dynamic hohlraum, an aluminum liner collides with a central foam and converts kinetic energy into radiation, and the liner-foam response depends on the aluminum equation of state (EOS). We construct a wide-range aluminum equation-of-state table from density functional theory (DFT) simulations over solid-liquid-plasma regions, denoted DFT-eos. Mixed deterministic-stochastic finite-temperature DFT (mDFT) gives the electron thermal contribution; quantum molecular dynamics (QMD) with classical calibration gives the ion part. We perform one-dimensional cylindrical radiation MAGNETohydrodynamics (MHD) simulations at a peak current of 50 MA and rise times of 220-300 ns on a single-layer light foam load. Opacity and electrical conductivity are fixed; only the liner Al EOS is changed between DFT-eos and the quotidian EOS (QEOS). Impact time and peak liner kinetic energy change little between the two tables. Larger differences appear in flight-segment density, the contact state at impact, and the time history of outgoing radiation power at the outer interface.
[abstract 19 / 43] (score: 3) - Title: Numerical simulations of low-mass BLACK HOLE-neutron star mergers with moderate eccentricitiesAuthors: Ivan Markin, Gonzalo Morrás, Tim Dietrich,Comments: 24 pages, 8 figures, to be submitted to PRDSubjects: gr-qc astro-ph.HECreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
A confident detection of orbital eccentricity in gravitational-wave signals from BLACK HOLE-neutron star systems would be a strong indicator of their dynamical formation origin. While eccentric waveform models have recently been developed, their validity for analyzing BLACK HOLE--neutron star signals has yet to be tested against numerical-relativity simulations. Building upon our previous study of quasicircular BLACK HOLE--neutron star mergers, we perform simulations of a subset of these systems with orbital eccentricities around five times larger than those inferred for GW200105_162426. Additionally, we perform simulations with MAGNETized matter to assess whether trapped $g$-mode oscillations persist in strongly MAGNETized disks. Regarding the emitted gravitational-wave signal, we find that the effective one-body waveform model SEOBNRv5EHM shows reasonable agreement unless tidal contributions become important, and the inspiral-only post-Newtonian models pyEFPE/pyEFPEHM show larger disagreement in the late inspiral. For the equal-mass system, which has the largest effective tidal deformability, eccentric tidal corrections have a small but noticeable impact on the phase, $\sim0.1$ rad. We find an almost negligible impact of eccentricity on the properties of the remnant BLACK HOLE, and differences of up to a factor of two in the remnant disk mass. Trapped $g$ modes in the accretion disks have the same frequency regardless of the eccentricity, confirming that they depend mainly on the properties of the remnant BLACK HOLE. We find that when accretion disks are strongly MAGNETized, they become less dense and have less pronounced structure, and that the trapped $g$ modes previously identified in the unMAGNETized cases are efficiently damped.
[abstract 20 / 43] (score: 3) - Title: A Shell Collision Scenario for EP251222b/GRB 251222A: Connecting Prompt Emission and Double-Peaked AfterglowAuthors: Run Shi, Di Xiao, Brajesh Kumar, Yifang Liang, Guowang Du, Jinjun Geng, Wenlong Zhang, Yuan Fang, Chenlei Guo, Dingfang Hu, Jie Hu, Qiuju Huang, Yanlong Hua, Yongfeng Huang, HongGuang Li, Xiangkun Liu, Xiaowei Liu, Yuan Liu, Jirong Mao, Xuan Mao, Bao Wang, Yuanpei Yang, Shiyan Zhong, Dan Zhu, Xuefeng Wu, Weimin Yuan,Comments: 26 pages, 9 figures. Submitted to The Astrophysical Journal (ApJ)Subjects: astro-ph.HECreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
GRB 251222A is a long-duration GAMMA-RAY BURST at a spectroscopic redshift of $z=3.171$. It was detected by the EP as the soft X-ray transient EP251222b before and during the gamma-ray emission. We performed a multi-wavelength (EP/WXT, fermi/GBM, swift/XRT and optical/NIR) investigation of this event. Its prompt soft X-ray and gamma-ray features, together with two afterglow rebrightenings, allow us to examine a possible connection between the prompt ejecta and the afterglow. We consider a multiple-shell scenario in which a faster, narrower shell catches up with a slower, wider shell. We assume that the selected pulse groups trace different ejecta and that the late X-ray flare marks their collision. Under these assumptions, we represent the post-collision outflow by an effective merged core and an outer annular component. A joint fit to the multi-band afterglow gives a Lorentz factor of $Γ_c\approx293$ for the merged core and $Γ_{1,w}\approx228$ for the outer component. The sample-wise collision mapping gives an energy release of $E_{\rm diss}=(1.6^{+2.1}_{-0.9})\times10^{52}$ erg and a dynamical dissipation efficiency of $0.37^{+0.07}_{-0.14}\%$. EP251222b can therefore be used to test a prompt--afterglow connection through shell collisions, although it does not uniquely establish this interpretation.
[abstract 21 / 43] (score: 3) - Title: AGN Feeding and Feedback: Resolving the TorusAuthors: M. Pereira-Santaella, F. Combes, A. Alonso-Herrero, S. Garcia-Burillo, A. Audibert, E. Bertola, M. Bischetti, R. Decarli, I. Garcia-Bernete, I. Lamperti, I. Ruffa, F. Salvestrini, H. R. Stacey, M. V. Zanchettin, V. Casasola, D. Espada, D. Nguyen, M. Pandey-Pommier, S. Thater,Comments: Part of the ALMA2040 White Paper Series. 9 pages, 4 figuresSubjects: astro-ph.IM astro-ph.GACreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
Active Galactic Nuclei (AGN) play a key role in galaxy evolution by regulating STAR FORMATION within their host galaxies. It is therefore crucial to understand how the central supermassive BLACK HOLEs (SMBH) are fueled by material from the galactic disk, and how AGN feedback impacts the surrounding gas. Most information so far comes from very nearby active galaxies (z < 0.008; D < 35 Mpc), providing the best spatial resolution and revealing randomly oriented dusty molecular tori that fuel SMBHs. A facility such as ALMA2040, offering significantly higher sensitivity and better angular resolution than current ALMA, would enable progress in two fundamental areas that remain beyond the capabilities of all existing and planned observatories: (i) probing the dynamics of the material feeding the AGN down to the accretion disk in nearby galaxies; and (ii) spatially resolving the tori and circum-nuclear regions of more energetic and cosmologically significant AGN, such as local QUASARs (z ~ 0.1 and Lbol > 10^45 erg/s).
[abstract 22 / 43] (score: 3) - Title: Investigation of an X-class Flare and Quasi-Periodic Pulsations in NOAA AR 13842 using SDO, Aditya-L1 and Solar OrbiterAuthors: Pawan Kumara, Sanjay Kumara, Sushree S. Nayak, Sadashiv, Sachin Rajkapoor Kanaujiyac, Ramesh Chandrad,Comments: 23 Pages, 14 Figures, Accepted in Advances in Space Research (ASR)Subjects: astro-ph.SRCreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
We investigate an X9.0 class flare (SOL2024-10-03T12:08) and associated quasi-periodic pulsations (QPPs) in NOAA active region (AR) 13842 using observations from the Solar Dynamics Observatory (SDO), Aditya-L1 and Solar Orbiter (SO). To explore the role of MAGNETic configuration in the flare, we employ non-force-free-field extrapolation technique for reconstructing a sequence of the coronal MAGNETic field throughout the flare. The observations reveal the emergence of intricate flare brightenings and ribbons. QPPs are observed with periods of $\approx$ 2 and $\approx$ 6 minutes in EUV, $\approx$ 7 minutes in UV, and $\approx$ 1 minute in X-rays. The extrapolation documents the presence of a flux rope, a sheared arcade, and a hyperbolic flux tube (HFT) enveloping the rope and the arcade. The sequence of the extrapolation illustrates an increase in the twist of the rope as it ascends towards a torus-unstable region, thereby rendering the rope a viable candidate for eruption. The sheared arcade appears to generate electric current through its foot-point's motion, which explains the sigmoidal brightening observed at the flare onset. The motion also seems to drive the non-parallel field lines closer together, heightening gradient in the MAGNETic field beneath the rope. Consequently, recurrent MAGNETic RECONNECTion is anticipated within the sheared arcade --- explaining the ascent of the rope with its twist increment. The formation of parallel flare ribbons is attributed to these RECONNECTions. Furthermore, RECONNECTion at the HFT is proposed to lead the remote and quasi-circular ribbons. Crucially, repeated RECONNECTions inside the arcade as well as at the HFT are speculated to cause the QPPs.
[abstract 23 / 43] (score: 2) - Title: A linear model of synergetic current drive with lower-hybrid wave and electron cyclotron waveAuthors: J. N. Chen, S. Y. Chen, M. L. Mou, C. J. Tang,Comments: 30pages,13figuresSubjects: physics.plasm-phCreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
A linear model of synergetic current drive (SCD) with lower-hybrid wave (LHW) and electron cyclotron wave (ECW) is developed to quickly calculate the quantitative SCD efficiency and reveal the conditions for the occurrence of the synergy effect. In this model, the response function dominated by collisions in the presence of LHW is derived from the adjoint equations by using perturbation and Green-Function techniques, where the RELATIVISTIC and trapping effects are considered. The SCD results compared to Lin-Liu's ECW current drive (ECCD) efficiency show two features of the synergy effect, one is that it is inclined to occur at smaller $y = 2ω_{c}/ω$ with the fixed ECW parallel refractive index $n_{\parallel}$, and the other is that the threshold values of $y$, at which the synergy effect becomes sufficiently significant, shift towards higher values with a decreasing $n_{\parallel}$; the SCD results without the trapping effect and the response function without the RELATIVISTIC effect have been provided. The quasilinear simulation on ECCD and SCD efficiency with a two-dimensional Fokker-Planck code is consistent with the results of the linear model in trends. Given considerable parameter improvements nowadays, the SCD efficiencies with parameters of current mainstream reactors are calculated in this work. We provide the current profile of ECCD and SCD by combining them with GENRAY, showing the potential application of integrating SCD into a ray-tracing code. Criteria for the occurrence and the sufficient significance of the synergy effect are suggested, which indicate that the synergy effect is dependent on the power factor that quantifies the degree of the overlap of the two waves quasilinear domains, the LHW power, and synergy electrons.
[abstract 24 / 43] (score: 2) - Title: Jittering JETs in stripped-envelope core-collapse SUPERNOVAeAuthors: Nikki Yat Ning Wang, Dmitry Shishkin, Noam Soker,Comments: Accepted for publication in ApJSubjects: astro-ph.HE astro-ph.SRCreated: 2026-10-14; Updated: 2026-10-16; Datestamp: 2026-10-16
We compare the expected explosion time of core-collapse SUPERNOVAe (CCSNe) in the jittering JETs explosion mechanism (JJEM) to that in the neutrino-driven (the delayed neutrino) mechanism, and conclude that for most, but not all, stellar models, even when the neutrino-driven mechanism might have led to an explosion, the JJEM starts to operate before the neutrino mechanism fully revives the stalled shock. To achieve this goal, we conduct comprehensive one-dimensional stellar evolution simulations using the code \textsc{mesa} to determine the expected explosion time according to the JJEM, which corresponds to the time when the inner convective layer of the core is accreted onto the newly born neutron star (NS). We present results for many hydrogen-rich, hydrogen-stripped, and helium+hydrogen-stripped envelope CCSN progenitor models. We find that most, but not all, of our models in the initial mass range of $M_{\rm ZAMS}=12M_\odot$ to $M_{\rm ZAMS}=40M_\odot$, have at least one strong convective zone inside the mass coordinate that is the maximum baryonic mass of an NS, $m \simeq 2.65\ M_\odot$, which can facilitate the JJEM. This study contributes to establishing the JJEM as a viable explosion mechanism of CCSNe.
[abstract 25 / 43] (score: 2) - Title: The formation of merging BLACK HOLEs via stable mass transfer in massive binary starsAuthors: Xiao-Tian Xu, Norbert Langer, Jakub Klencki, Chen Wang, Xiang-Dong Li,Comments: Published in Nature Astronomy. Link to the paper https://www.nature.com/articles/s41550-026-03000-7 . This is a pre-review version with a title matching the published version (old title: "Stable mass transfer in massive binaries leading to merging black holes")Subjects: astro-ph.SR astro-ph.HE gr-qcCreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
The vast majority of massive binary systems in the universe is evidently unsuited to produce merging binary BLACK HOLEs. However, several narrow evolutionary paths of isolated massive binaries towards this goal have recently been identified. Due to the high degree of simplification and assumptions applied in previous modelling of these paths, conclusions remained vague so far. For one of these paths, the stable mass transfer channel, we now construct detailed binary evolution models which include internal differential rotation as well as mass and angular momentum transfer between the stars, all the way from the zero-age main sequence to the formation of the BLACK HOLEs, only skipping the rapid late burning stages. This allows us to follow the mass and chemical structure evolution of the mass accreting component, which turns out to have a key influence on the phase of reverse mass transfer, that allows the obtained BLACK HOLE spins and mass ratios to naturally fall into the regime observed for the gravitational-wave source in the 10--25$M_\odot$ primary BLACK HOLE mass range. As for this channel, also a large number of progenitor binaries are known, we conclude that it likely contributes to the observed population of gravitational wave sources.
[abstract 26 / 43] (score: 2) - Title: Modeling the merger-ringdown of an eccentric test-mass inspiral into a Kerr BLACK HOLE using the effective-one-body frameworkAuthors: Guglielmo Faggioli, Alessandra Buonanno, Maarten van de Meent, Gaurav Khanna,Comments: 39 pages, 19 figures, 3 ancillary filesSubjects: gr-qcCreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
We characterize and phenomenologically model the merger-ringdown of gravitational waves emitted by a small compact object that plunges and merges into a Kerr BLACK HOLE from equatorial-eccentric inspirals. The waveforms are generated employing a time-domain Teukolsky code sourced with trajectories computed using the effective-one-body framework. We span values of the Kerr spin $a\in[-0.9, 0.9] $, eccentricity at the last stable orbit (LSO) $ e_{\rm LSO} \in [0,0.9] $, and RELATIVISTIC anomaly $ ξ_{\rm LSO} \in [0 , 2 π]$. We characterize the last peak of the waveform and ringdown features across the parameter space, finding that the eccentricity mainly affects the last peak features, while it has a smaller impact on the ringdown signal. In contrast, the RELATIVISTIC anomaly measured at the LSO influences the morphology of the last peak in a restricted portion of the parameter space and has no impact on the ringdown part. We perform the analysis for all the spin-weighted spherical harmonic modes normally included in the $\texttt{SEOBNR}$ family of models, $(\ell,m)\in\{ (2,2), (3,3), (4,4), (5,5), (2,1), (3,2), (4,3)\}$. Finally, we introduce a merger-ringdown model for $\texttt{SEOB-TMLE}$, a forthcoming inspiral-merger-ringdown waveform model for eccentric spin-aligned binary BLACK HOLEs in the test-mass limit, whose features can be extended to comparable-mass regimes. The model also accounts for quasinormal mode mixing during the ringdown. It provides a first step toward incorporating the impact of residual eccentricity close to merger into spin-aligned effective-one-body merger-ringdown models for binary BLACK HOLEs.
[abstract 27 / 43] (score: 2) - Title: Lacunarity in a Two-Dimensional Atomizing Liquid JetAuthors: Guangnian Ji, Yash Kulkarni, Stéphane Zaleski,Comments: 6 pages, 5 figuresSubjects: physics.flu-dynCreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
Atomization stretches and folds the liquid--gas interface before fragmenting it into ligaments and droplets, making fractal measures a natural descriptor of the lacunarity of the final breakup state. We examine this idea in two-dimensional (2D) VOF-DNS of a liquid JET with adaptive mesh refinement in Basilisk. Box-counting of the full resolved interface does not yield a single scale-independent exponent. Instead, two scaling ranges appear, separated by a crossover near the box-counting level \(L_{\mathrm{box}}\simeq7\): coarser boxes measure the folded connected JET envelope, whereas finer boxes increasingly sample ligaments, droplets, and nearly smooth local interface segments. Decomposing the interface into detached droplets, ligaments, and the connected main body shows that the relevant effective dimension is structure dependent. Droplets are most lacunar with dimension below one, ligaments occupy an intermediate level, and the main body carries the largest coarse-scale dimension. This hierarchy persists over $Re_l=100$--$10^4$ at fixed $\We_g=200$. The lacunarity of droplets is reminiscent of that of the object positions in the night sky hypothesized by de Vaucouleurs.
[abstract 28 / 43] (score: 2) - Title: Linear causality and stability constraints on RELATIVISTIC second-order MAGNETohydrodynamicsAuthors: Yiwei Qiu, Duan She, Defu Hou,Comments: 62 pages, 10 figuresSubjects: physics.flu-dyn astro-ph.HE hep-phCreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
In this work, we construct a theoretical framework for RELATIVISTIC second-order MAGNETohydrodynamics based on entropy current analysis. The formalism consistently incorporates finite relaxation dynamics of the dissipative fluxes, providing a transient framework suitable for analyzing linear stability and short-wavelength causality. Utilizing linear mode analysis, we investigate the constraints imposed by causality and stability on this anisotropic system. By linearizing the theory around a homogeneous equilibrium state, we identify the MAGNETosonic, Alfvén, and charge-diffusion sectors, together with their coupling terms. For each sector, we derive asymptotic dispersion relations in both the long-wavelength (small-$k$) and short-wavelength (large-$k$) regimes, validating them against exact numerical roots. Our numerical analysis confirms the accuracy of these asymptotic solutions and uncovers a nontrivial angular dependence, especially near special propagation directions where the ordinary momentum expansion becomes less reliable. By evaluating the large-$k$ behavior of the propagating branches alongside the damping properties of non-hydrodynamic modes, we delineate the corresponding causality constraints. We find that the admissible linear causal domain is governed by the interplay between propagation direction, anisotropic transport coefficients, and relaxation times, with the resulting bounds being intrinsically mode-dependent. These findings provide a systematic theoretical basis for investigating linear stability and short-wavelength causality in RELATIVISTIC MAGNETohydrodynamics beyond the first-order approximation.
[abstract 29 / 43] (score: 2) - Title: Mock Catalogs of Strongly Lensed Gravitational Waves via a Halo Model Approach with Space-borne DetectorsAuthors: Mingqi Sun, Kai Liao, Youkai Li, Tonghua Liu, Hengyu Wu, Shaoqi Hou, Tao Yang, Xilong Fan, Marek Biesiada,Comments: 20 pages, 13 figures, 11 tables, to appear in ApJSSubjects: astro-ph.CO astro-ph.GA astro-ph.HECreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
Future space-borne gravitational-wave (GW) detectors, such as LISA and DECIGO, are expected to detect a large number of GW events, a fraction of which may be strongly lensed by intervening galaxies or galaxy clusters. In this work, we develop a comprehensive framework to simulate strongly lensed GWs in the context of space-borne detectors. Based on realistic astrophysical models for both the source population and the lens distribution, we construct mock catalogs of lensed GW events, referred to as \textbf{GW-LMC-Space}. Our results show that, for a four-year LISA observation, the expected number of lensed events ranges from $0$ to $131$, depending on the adopted formation model of massive BLACK HOLE binaries (MBHBs). The corresponding lensing probability for MBHBs can reach up to $\sim 0.3\%$. For DECIGO, we find that the number of lensed events in a one-year observation is expected to lie in the range of $0$--$44$, with a lensing probability of $\sim 0.15\%$ for stellar-mass binary BLACK HOLEs (BBHs), binary neutron stars (BNSs), and neutron star--BLACK HOLE binaries (NSBHs). We further show that the overlap of lensed signals is a common feature in space-borne detectors, which can significantly affect both the signal-to-noise ratio (SNR) estimation and event identification. These results highlight the importance of accounting for signal overlap in the analysis of strongly lensed GW events in future space-borne GW observations.
[abstract 30 / 43] (score: 2) - Title: Quadrupole and quadratic-in-spin effects in quasicircular, spinning, asymmetric binariesAuthors: Mostafizur Rahman, Misbah Shahzadi, Adam Pound, Josh Mathews,Comments: 24 pages, 7 figures, 3 tables. Minor modifications. Matches the version published in Phys. Rev. DSubjects: gr-qcCreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
Next-generation gravitational-wave detectors will require significant improvements in current theoretical waveform models, particularly in the case of asymmetric-mass binaries. Here we provide one such improvement by calculating fully RELATIVISTIC finite-size effects for small mass ratios -- primarily, fluxes of energy -- including quadratic-in-secondary-spin terms, spin-induced quadrupole terms, and tidally induced quadrupole terms, for quasicircular inspirals of a small companion into a Kerr BLACK HOLE. We formulate these calculations within a multiscale waveform-generation framework in self-force theory, which could be used, with an energy-balance law we derive, to develop self-contained waveform models for asymmetric binaries involving stars orbiting BLACK HOLEs. Our results could additionally be used to improve other families of waveform models across all mass ratios. We present results both as complete numerical data sets on a Chebyshev grid and as analytical post-Newtonian expansions (to sixth PN order relative to the leading term in each contribution to the flux).
[abstract 31 / 43] (score: 2) - Title: Analysis of collisional and facility effects in a MAGNETic nozzle plasma expansionAuthors: Manuel Cortés-Hernán, Mario Merino, Diego García-Lahuerta, Eduardo Ahedo,Comments: 36 pages, 10 figuresSubjects: physics.plasm-phCreated: 2026-10-14; Updated: 2026-10-16; Datestamp: 2026-10-16
An axisymmetric, quasineutral three-fluid model is proposed to study the plasma expansion in a MAGNETic nozzle under the presence of neutrals coming either from the plasma source or as an homogeneous background. As a difference with other models, electron cooling in the plume is achieved by treating the electron energy flux as mainly convective and without the need to postulate any anomalous resistivity. Solutions are presented for the electron high-MAGNETization limit, in which the electron main magnitudes can be integrated along MAGNETic lines. Ionization, elastic and charge-exchange collisions with neutrals do not change the main qualitative features of the plasma expansion, known from previous collisionless models. Ionization enhances the plasma flow in the nozzle, and leads to additional electron cooling, which decreases the electric potential fall along the nozzle. The efficiency of the nozzle is quantified in terms of the gain of MAGNETic thrust and the plume divergence angle. Two types of boundary conditions are discussed for the electron flow: local current ambipolarity conditions at the nozzle throat and global current-free conditions at the outer boundary (i.e., metallic vacuum chamber walls). These last ones are shown to be physically more reliable: they introduce the influence of the chamber walls on the plasma expansion by shaping the ambipolar electric field; they permit the extrapolation to undisturbed free space conditions; and they approximate better experimental trends with the background pressure.
[abstract 32 / 43] (score: 2) - Title: Electrically charged regular BLACK HOLEs in higher dimensions: Maxwellian limit, branch point of the Lagrangian, and thermodynamicsAuthors: Bobir Toshmatov, Bobomurat Ahmedov, Nozima Isamadinova, Ozodbek Rahimov, Chengxun Yuan,Comments: 17 pages, 6 figuresSubjects: gr-qcCreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
Electrically charged regular BLACK HOLEs in general relativity coupled to nonlinear electrodynamics are known to require a double-valued Lagrangian density $L(F)$, with a branch point at the radius where the electroMAGNETic invariant attains its extremum. We extend the construction of such BLACK HOLEs to an arbitrary number of spacetime dimensions $D\geq4$ and obtain a new family of solutions that unifies the Bardeen and Hayward BLACK HOLEs in a single analytic form, with a single nonlinearity parameter $γ$. We show that the Maxwellian weak-field limit is recovered if and only if $γ=D-3$, so that the Bardeen and Hayward BLACK HOLEs, which lack this limit in four dimensions, become Maxwellian in five and six dimensions, respectively. The matter sector is written in the dual $P$ framework as a Hamiltonian density $H(P)$ that contains only fixed coupling constants, so that the mass and the charge of the BLACK HOLE appear as integration constants of a fixed theory; the regular solutions form a one-parameter subfamily in which the mass is tied to the charge. We locate the branch point of $Ł(F)$ in closed form and find that it is always hidden inside the event horizon in four dimensions, whereas for $D\geq5$ it emerges from the horizon for near-extremal charges and becomes visible to a distant observer. The null and weak energy conditions are satisfied everywhere, the strong energy condition is violated only inside the horizon, and the dominant energy condition is violated at large distances only for $γ>D-3$. Finally, since the theory is fixed, the first law of BLACK HOLE thermodynamics holds in its standard form; we derive the horizon potential in closed form, the extended first law with the couplings as thermodynamic variables, and the corresponding Smarr formula.
[abstract 33 / 43] (score: 2) - Title: Thermochemically Constrained Multiscale Laplace Neural Operator to Learn Stiff Chemical Kinetics with Conditional Diffusion Model SamplingAuthors: Dong Yang, Xiongbo Duan, Min Zhang, Yuqiang Li,Comments: Main text: 14 pages, 13 figures. Supplementary Materials: 3 pages, 3 figuresSubjects: physics.comp-ph physics.flu-dynCreated: 2026-10-09; Updated: 2026-10-16; Datestamp: 2026-10-16
Stiff chemical kinetics is a major computational bottleneck in reacting-flow simulations, while data-driven solvers remain sensitive to training-state coverage and chemical dynamics. This work combines conditional diffusion sampling with a thermochemically constrained multiscale Laplace neural operator (TC-MLNO) for chemistry ODE integration. The diffusion model learns the equivalence-ratio-conditioned joint distribution of temperature and species from low-dimensional flame data, augmenting the state space without independent perturbations. TC-MLNO represents transient, non-periodic responses through pole-residue Laplace layers and assigns fast, medium, and slow species to separate branches. Thermochemical constraints are imposed through losses for mass and elemental conservation and heat release rate. The framework is evaluated in 1D premixed flames, a 2D developing JET, and a 3D turbulent burner flame. With equal-sized datasets, diffusion sampling reduces the 95th-percentile distance to the base flame manifold by up to 37.5% and the a posteriori full-species macro-average error by up to 92.7% versus random sampling, especially for minor species and radicals. TC-LNO yields smaller errors than the DeepONet baseline for 84.9% of retained modes and reduces the 95th-percentile error for the most attenuated modes from 0.372 to 0.081. In multidimensional flames, TC-MLNO better preserves reaction-zone locations, heat-release structures, and chemically sensitive species than DeepONet. Errors of representative radical and nitrogen-containing species in the 3D flame decrease by 88.0%-88.9%. Compared with direct CVODE integration, TC-MLNO reduces mean chemistry and total solution times by 90.1% and 62.6%, respectively. These results show that distribution-aware sampling and Laplace neural operator learning provide an accurate and efficient alternative for stiff chemical ODE integration.
[abstract 34 / 43] (score: 2) - Title: On MAGNETic-field consistency in the sideways force calculation of Phys. Plasmas 27, 012508 (2020)Authors: Denis Mironov,Comments: 10 pages, 2 figuresSubjects: physics.plasm-phCreated: 2026-10-09; Updated: 2026-10-16; Datestamp: 2026-10-16
We examine the consistency of the equilibrium MAGNETic field $\mathbf{B}_0$ used in the analytical calculation of the sideways wall force by A. A. Martynov and S. Yu. Medvedev [Phys. Plasmas 27, 012508 (2020)] and the subsequent reformulation presented in [Phys. Plasmas 27, 054702 (2020)]. In these attempts, the current density $\mathbf{j}_0 = \nabla \times \mathbf{B}_0$ must vanish in the vacuum regions adjacent to the wall, making $\mathbf{B}_0$ curl-free as a complement to the natural $\nabla \cdot \mathbf{B}_0 = 0$. Since the cited works incorporate selected toroidal corrections without explicitly specifying the corresponding differential operators, we test $\mathbf{B}_0$ adopted in these models against Maxwell's equations using both toroidal and quasi-cylindrical formulations. We show that the divergence-free requirement is violated in the toroidal interpretation, while the curl-free condition is not satisfied in the quasi-cylindrical limit. The reformulation likewise fails to define a self-consistent equilibrium field with toroidal effects because the accompanying field corrections required for consistency with Maxwell's equations are not specified. Since the sideways force calculations are built upon these inconsistent field prescriptions, their analytical derivations are consequently compromised. The resulting arguments therefore cannot serve as a valid basis for revising either the earlier results established by D. V. Mironov and V. D. Pustovitov [Phys. Plasmas 24, 092508 (2017)] or those obtained within the single-harmonic analysis [Phys. Plasmas 22, 052502 (2015)].
[abstract 35 / 43] (score: 2) - Title: The Impact of High-Mass Clusters on the Binary Black Hole Merger Rate over Cosmic TimeAuthors: Aidan Mai, Kyle Kremer, Fulya Kıroğlu,Comments: 16 pages, 11 figures. Submitted to ApJ. Comments welcome!Subjects: astro-ph.GA astro-ph.HECreated: 2026-10-14; Updated: 2026-10-16; Datestamp: 2026-10-16
We present a cosmological calculation of the binary BLACK HOLE merger rate from dense star clusters, using a $\texttt{Cluster Monte Carlo}$ ($\texttt{CMC}$) model grid spanning the full observed parameter space of cluster mass, metallicity, and virial radius. For the first time, we incorporate $N=10^{7}$-particle $\texttt{CMC}$ models into this calculation, including a new solar-metallicity model, extending the $\texttt{CMC Cluster Catalog}$ to the most massive clusters observed in the local Universe. Using an analytic cluster formation model which convolves the cluster formation rate with delay-time distributions from our model suite, we find that the local cluster BBH merger rate is dominated by low-mass ($M_1 \lesssim 20\,M_\odot$) mergers originating from recently formed, high-metallicity clusters. While high-mass clusters are the primary sites of hierarchical (second-generation and higher) mergers, their contribution to the overall merger rate is suppressed by the exponential cutoff of the cluster initial mass function. The hierarchical merger rate is therefore highly sensitive to the exact value of the Schechter mass, $M_S$, suggesting that gravitational wave constraints on the hierarchical merger fraction can independently constrain the high-mass end of the cluster initial mass function. Our cluster formation model reproduces the observed present-day GC number density without fine tuning, and we find $M_S = 10^7\,M_\odot$ provides the best match to the observed Virgo GC mass distribution. For this value, $27\%$ of local dynamical mergers are hierarchical, compared to $18\%$ for the canonical value of $M_S = 10^{6.26}\,M_\odot$. Our merger weights, which we make publicly available, can be used for direct comparison with LVK distributions and other formation models.
[abstract 36 / 43] (score: 2) - Title: Wandering intermediate-mass BLACK HOLEs and off-nuclear tidal disruption events from early star clustersAuthors: Claire E. Williams, Smadar Naoz, Yihao Zhou, Tatsuya Akiba-Lewis, Mark Vogelsberger, Blakesley Burkhart, Naoki Yoshida, Avi Chen, Kyle Kremer, William Lake, Federico Marinacci, Shyam H. Menon,Comments: 27 pages, 11 figuresSubjects: astro-ph.GA astro-ph.HECreated: 2026-10-14; Updated: 2026-10-16; Datestamp: 2026-10-16
Off-nuclear tidal disruption events (TDEs) reveal evidence for massive BLACK HOLEs outside galactic centers, but the origins of this wandering population remain uncertain. We investigate wandering intermediate-mass BLACK HOLEs (IMBHs) formed through runaway stellar collisions in dense, high-redshift star clusters and predict their TDE signatures across cosmic time. Our semi-analytic model samples clusters associated with low-mass subhalos at $7
[abstract 37 / 43] (score: 2) - Title: Axial gravitational quasinormal modes of MAGNETically charged BLACK HOLEsAuthors: De-Cheng Zou, Xufen Zhang, Chao-Ming Zhang, Ming Zhang, Rui-Hong Yue,Comments: Published in Chinese Physics C 49 (2025) 125109Subjects: gr-qcCreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
In this paper, we consider axial perturbations on the MAGNETically charged string-inspired Euler-Heisenberg BLACK HOLE. Since axial metric perturbation decouples from axial electroMAGNETic perturbation, here we mainly focus on axial gravitational perturbation. By using WKB approximation and AIM methods, we make a detailed analysis of the gravitational quasinormal frequencies by varying the characteristic parameters of gravitational perturbation and BLACK HOLEs. It is found these results obtained through the AIM method are in good agreement with those of obtained by WKB method, including these results extracted from the time-domain profiles. The greybody factor is calculated by WKB method. The effects of these parameters $Q_m$, $ε$ and multipole number $l$ on the greybody factor are also studied.
[abstract 38 / 43] (score: 2) - Title: Probing fundamental physics with ALMA2040 mm-wavelength observations of neutron starsAuthors: Kuo Liu, Marilyn Cruces, Gregory Desvignes, Michael Kramer, Mariafelicia De Laurentis, Natalia Lewandowska, Nutnicha Masoongnoen, Dieu D. Nguyen, Lijing Shao, Pablo Torne, Jompoj Wongphechauxsorn,Comments: 8 pages, 3 figures, Part of the ALMA2040 White Paper SeriesSubjects: astro-ph.HECreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
Bursty or (rotation-induced) pulsed coherent radio emission from pulsars, MAGNETars, and fast radio transients originates in some of the most extreme environments in the Universe. However, the exact physical mechanism behind the scenes remains poorly understood. ALMA2040 will allow for systematic exploration of the millimeter-wavelength spectral window for pulsars and fast radio transients for the very first time, offering unprecedented opportunities to discover new observational phenomena and advance our understanding of emission physics. Beyond this, ALMA2040 provides a unique means to unveil the neutron-star population in the Galactic Centre (GC), enable novel tests of fundamental physics in the vicinity of the supermassive BLACK HOLE Sgr A*, probe the potential existence of DARK MATTER in the GC, and investigate the dense, highly dynamic interstellar and MAGNETic environment of this region.
[abstract 39 / 43] (score: 2) - Title: From Cosmic Bounces to Primordial Black Holes: The Role of Primordial Magnetic FieldsAuthors: Ajeet Singhal, Shreya Banerjee,Comments: 33 pages, 12 figuresSubjects: gr-qc astro-ph.COCreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
We investigate primordial BLACK HOLE (PBH) formation from primordial MAGNETic fields generated during a non-singular ekpyrotic bounce. A time-dependent coupling between the electroMAGNETic field and a scalar background breaks conformal invariance and amplifies gauge field fluctuations during contraction, generating MAGNETic fields whose anisotropic stress dominates during radiation domination. By retaining finite-wavenumber cutoffs, we compute the ultraviolet-dominated curvature spectrum, evaluate density-perturbation variance, and determine PBH abundances using both monochromatic and critical-collapse prescriptions. For benchmark parameters, the critical collapse mass spectrum peaks at $M\simeq 2.0\times10^{-3}M_\odot$ , with a total PBH DARK MATTER fraction of $f_{PBH}\approx 10^{-5}$, forming a subdominant subsolar PBH population. Enforcing the cosmological overclosure bound ($f_{\mathrm{PBH}} \le 1$) constrains the primary background parameters, namely the end-of-contraction Hubble scale ($H_{\mathrm{end}} \le 1.6 \times 10^3~\mathrm{GeV}$) and the contraction exponent ($q \le 0.247$), establishing a physical boundary consistent with the electroMAGNETic backreaction limit. Shifting to asteroid-mass PBHs or a larger DARK MATTER fraction requires modifying the ultraviolet cutoff and contraction duration. This analysis highlights the essential role of finite-wavenumber cutoffs and assumed-collapse prescriptions in linking bounce MAGNETogenesis to the predicted PBH abundance.
[abstract 40 / 43] (score: 2) - Title: Secular Evolution of Quasiperiodic Eruptions: eRO-QPE2Authors: Zirui Zhang, Cong Zhou, Zhen Pan,Comments: 13 pages, 8 figuresSubjects: astro-ph.HECreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
Quasi-periodic eruptions (QPEs) are recurrent soft X-ray flares from galactic nuclei. In this work, we analyze both the quiescent and eruption emission of eRO-QPE2, using 11 XMM-Newton observations spanning $4.33\,{\rm yr}$. The key findings include (1) the eruption peak count rate remains approximately constant, while the quiescent count rate shows an approximately linear decline superposed with a large-amplitude oscillation; (2) no secondary eruptions are detected between the normal eruptions and any such events would have to be fainter by more than two orders of magnitude; (3) the recurrence time decreases at an average rate of $\dot{T}_{\rm rec}\approx-5\times10^{-6}$. These findings are consistent with an extreme mass-ratio inspiral (EMRI) interacting with a precessing accretion disk and producing two normal eruptions per orbital period. Bayesian timing analyses further constrain the EMRI orbital eccentricity to $e<0.033$ (at $95\%$ confidence level).
[abstract 41 / 43] (score: 2) - Title: Convective Oscillations of Cosmic RaysAuthors: Yiran Zhang, Siming Liu,Comments: accepted for publication in ApJSubjects: astro-ph.HECreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
Turbulent motion of the background plasma can introduce fluctuations in the spatial distribution of COSMIC RAYs (CRs). For an ensemble-averaged Gaussian CR distribution with a width $ Λ\left( t,p \right) $ at time $ t $ and momentum $ p $, it is found that $ P_\text{s}\left( t,k,p \right) $ and $ P_\text{d}\left( t,k,p \right) $, the fluctuation power spectra induced by incompressible and acoustic turbulent convection, respectively, have power-law asymptotics in wavenumber $ k $: $ P_\text{s}\left( t,k,p \right) \propto k^4 $ and $ P_\text{d}\left( t,k,p \right) \propto k^2 $ for $ k\ll 1/Λ\left( t,p \right) $; $ P_\text{s}\left( t,k,p \right) \propto k^{γ_\text{s}-4} $ for $ k\gg 1/L_\text{s} $, and $ P_\text{d}\left( t,k,p \right) \propto k^{γ_\text{d}-2} $ for $ k\gg 1/L_\text{d} $, where $ γ_\text{s} $ and $ γ_\text{d} $ are the spectral indices of the velocity power spectra of the incompressible and acoustic turbulence below their outer scales $ L_\text{s} $ and $ L_\text{d} $, respectively. These results have implications for probing interstellar turbulence via future high-resolution images of pulsar gamma-ray halos.
[abstract 42 / 43] (score: 2) - Title: Breakdown of hydrodynamic universality in causal first-order viscous neutron star oscillationsAuthors: Lennox S. Keeble, Alejandro Cárdenas-Avendaño,Comments: 10 pages, 6 figuresSubjects: gr-qc astro-ph.HECreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
Hydrodynamic modeling of viscous neutron stars requires a choice of theory of RELATIVISTIC hydrodynamics. That distinct formulations contain the same physical content in the long-wavelength limit is referred to as ``hydrodynamic universality.'' It has been recently shown that hydrodynamic universality can break down in radial neutron star oscillations: causality and finite-size effects restrict access to the long-wavelength universal hydrodynamic regime in sufficiently viscous stars. We show that this breakdown occurs for a broad range of causal hydrodynamic frames in Bemfica--Disconzi--Noronha--Kovtun (BDNK) theory. Increasing viscosity collectively pushes this class of causal frames away from the BDNK regime of validity, eventually forcing all to lie outside it at bulk viscosities in the range $ζ\sim10^{30}$--$10^{31}\mathrm{g}/\mathrm{cm}/\mathrm{s}$. This breakdown of universality is accompanied by material changes in the oscillation mode structure: non-hydrodynamic modes become damped on timescales comparable to those of hydrodynamic modes, the first overtone can become longer lived than the fundamental mode, and unphysical instabilities with sub-millisecond timescales can emerge. Even in regimes where universality has broken down, we find that the inviscid threshold of gravitational collapse remains unchanged in BDNK theory. These results provide evidence that first-order theories of RELATIVISTIC hydrodynamics may be insufficient for modeling sufficiently viscous neutron stars.
[abstract 43 / 43] (score: 2) - Title: The Radius-Luminosity Relationship for Active Galactic Nuclei with Hierarchical Bayesian Reverberation MappingAuthors: Hugh McDougall, Tamara M. Davis, Benjamin J. S. Pope, Paul Martini, Zhefu Yu, Chris Lidman, Geraint F. Lewis, Christian Adamcewicz, Rahma Alfarsy,Comments: 18 Figures, 33 PagesSubjects: astro-ph.GA astro-ph.CO astro-ph.IMCreated: 2026-10-15; Updated: 2026-10-16; Datestamp: 2026-10-16
Reverberation mapping of ACTIVE GALACTIC NUCLEi uses the time taken for variability to travel through the system as a measure of system size, with this size being used to inform estimates of the mass of the central BLACK HOLE, a technique that has graduated to an industrial-scale effort in recent decades. Such large target-count, multi-year surveys have been consistently undercut by poor light curve quality and the aliasing problems of seasonal observations. These impacts compound with statistical approaches that are not consistent between works and sometimes combine inconsistent statistical frameworks. Here, we present a new end-to-end Bayesian framework for fitting lags at scale in large surveys, simultaneous with the fitting of population models such as the radius-luminosity relation, and formulated in a numerically tractable way. This procedure is a statistically and numerically robust generalisation of the stacking and quality cut procedures of past works, fully marginalising over data uncertainty and data quality. Our approach remains numerically stable when scaling to larger surveys, and can act as a basis for any Bayesian population modelling of large sets of AGN time series observations. Applied to the OzDES sample, we demonstrate that this new approach yields more than double the constraining power on population-level properties like the R-L relationship, and an order-of-magnitude increase in the number of recovered lags and masses. With this method, we go from 24 high quality lag recoveries with traditional methods to a new effective sample size of ~297, all while being robust against random chance false positive measurements.
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