Current date: 2026-05-28
Setting default datestamp limit: 0
Datestamp limit: 2026-05-28 (0 days ago)
Created/updated limit: 2026-05-21 (7 days ago)
Found keywords_cs.datFound keywords_cis.dat
Suggested sets: physics, physics:astro-ph, physics:gr-qc, physics:physics
Setting default set: physics
OAI-PMH request: http://export.arxiv.org/oai2?verb=ListRecords&from=2026-05-28&until=2026-05-28&set=physics&metadataPrefix=arXiv
Scoring abstracts
Number of records retrieved: 719
Keyword score statistics
score 6 -- 2 abstracts
score 5 -- 5 abstracts
score 4 -- 2 abstracts
score 3 -- 7 abstracts
score 2 -- 20 abstracts
in total -- 36 abstracts
Articles that appeared on 2026-05-28
-
[abstract 1 / 36] Yes (score: 6)
- Title: BlackHoleWeather -- Spin-coupled chaotic cold accretion across the meso-scale: Morphology and thermodynamicsAuthors: Olmo Piana, Massimo Gaspari, Filippo Barbani, Vieri Cammelli, Giovanni Stel, Davide M. Brustio, Valeria Olivares, Francesco Salvestrini, Ashkbiz Danehkar, Francesco Tombesi, Pasquale Temi, Filippo M. Maccagni, Martin Fournier,Comments: Submitted to A&A. Comments welcomeSubjects: astro-ph.GA astro-ph.HECreated: 2026-05-26; Updated: 2026-05-28; Datestamp: 2026-05-28
Supermassive BLACK HOLE (SMBH) spin is a key but poorly constrained ingredient of the feeding-feedback loop. Chaotic cold accretion (CCA) of cold gas clouds delivers rapidly varying three-dimensional torques that drive spin evolution and JET-axis reorientation, and in turn spin regulates JET power. We introduce a time-dependent SMBH spin model linking resolved multiphase feeding at meso scales to unresolved RELATIVISTIC angular-momentum transfer at the innermost stable circular orbit (ISCO). We perform GPU-accelerated hydrodynamical simulations of a group atmosphere with JET feedback and SMBH spin evolution, resolving multiphase inflow and angular-momentum direction below parsec scales. We compare fixed-axis, direct, and hybrid prescriptions, with the latter preserving the resolved torque direction while filtering its magnitude through a Kerr ISCO closure. We then apply the hybrid model to low- and high-turbulence group setups. The cold-gas reservoir is nearly independent of whether the JET is fixed, spin-coupled, or rapidly reorienting. The spin prescription instead controls the inner feeding-feedback coupling, modulating central accretion, JET efficiency, and feedback geometry. The hybrid model is bracketed by analytic limits, whereas the direct model overestimates spin variability and JET-axis wandering, showing that an ISCO closure is required. Low-spin SMBHs are easier to reorient because a misaligned torque acts on a smaller angular-momentum reservoir. The decisive quantity is the coherence of the delivered angular momentum: the low-turbulence run preserves longer feeding bridges and faster spin evolution, whereas stronger turbulence fragments the inflow and enhances torque cancellation. In CCA, turbulence regulates whether the cold reservoir remains connected, how the angular momentum reaches the SMBH, where the next JET points, and how feedback is imprinted onto the halo.
[abstract 2 / 36] Yes (score: 6) - Title: Magnetic Configuration Imprints on Quasi-Periodic Variability in GRMHD Simulations of Thin Accretion DisksAuthors: Jing-Ze Xia, Hong-Xuan Jiang, Indu K. Dihingia, Yosuke Mizuno,Comments: 18 pages, 18 figuresSubjects: astro-ph.HECreated: 2026-05-27; Updated: 2026-05-28; Datestamp: 2026-05-28
The origin of quasi-periodic oscillations (QPOs) in BLACK HOLE accretion flow remains uncertain, particularly regarding the role of MAGNETic field configurations in shaping disk structure and variability signatures. We investigate this using global two- and three-dimensional (2D and 3D) general RELATIVISTIC MAGNETohydrodynamic (GRMHD) simulations of geometrically thin disks initialized with different multi-loop MAGNETic field configurations. These configurations naturally produce a puffed-up inner region. We find that QPO-like variability arises in the effective viscosity and mass accretion rate, with frequencies following the local radial epicyclic frequency and its harmonics. Time-series diagrams show coherent, inclined stripe-like patterns associated with inertial-acoustic perturbations, while power spectra exhibit narrow bands of enhanced variability linked to truncation radii associated with MAGNETic fields. Cross-correlation analysis reveals a finite lag between pressure and Maxwell stress at these interfaces, consistent with viscous-epicyclic overstability. The MAGNETic topology regulates both the truncation radius and the location of resonant cavities that sustain oscillations. As the disk becomes thicker, increased turbulent diffusion suppresses the overstability and the associated QPO signals. We find that the QPO frequency ranges and their evolution are consistent with observations of BLACK HOLE X-ray binaries during outbursts. These results suggest that MAGNETic field configurations play a pivotal role in shaping disk structure and variability in accreting BLACK HOLEs.
[abstract 3 / 36] Yes (score: 5) - Title: On The Nonthermal Power Laws In Magnetized Turbulent PlasmasAuthors: Rostom Mbarek, Daniel Grošelj, Alexander Philippov,Comments: ApJLSubjects: physics.plasm-ph astro-ph.HECreated: 2026-05-27; Updated: 2026-05-28; Datestamp: 2026-05-28
Building on recent progress in the understanding of particle transport in MAGNETized plasmas, we derive a scaling law for the formation of nonthermal spectral tails in mildly and strongly MAGNETized turbulent environments. We validate this scaling using driven-turbulence particle-in-cell simulations that incorporate particle escape, allowing the system to reach a steady state. The simulation results show good agreement with our theoretical predictions. We then discuss the astrophysical implications of these findings, focusing on proton acceleration in the coronae of supermassive BLACK HOLEs and the resulting high-energy neutrino emission.
[abstract 4 / 36] Yes (score: 5) - Title: BlackHoleWeather -- Jet-regulated chaotic cold accretion across the meso scale: Morphology and thermodynamicsAuthors: Vieri Cammelli, Massimo Gaspari, Olmo Piana, Filippo Barbani, Giovanni Stel, Davide M. Brustio, Valeria Olivares, Francesco Salvestrini, Ashkbiz Danehkar, Michael Reefe, Pasquale Temi, Filippo M. Maccagni, Francesco Tombesi, Martin Fournier,Comments: Submitted to A&A: comments welcomeSubjects: astro-ph.GA astro-ph.HECreated: 2026-05-26; Updated: 2026-05-28; Datestamp: 2026-05-28
How mechanical AGN feedback couples to multiphase condensation across scales remains a problem in galaxy groups and clusters. It is unclear how JETs reshape the chaotic cold accretion (CCA) cycle and regulate black-hole fueling. BlackHoleWeather aims to build a unified description of the AGN baryon cycle across horizon, galactic, and group scales. Here we focus on how weather states shape the morphology and thermodynamics of JET-regulated CCA. We perform two hydrodynamical simulations of a turbulent, radiatively cooling galaxy-group atmosphere with self-regulated AGN feedback. The runs are initialized in two turbulence regimes and evolved with a kinetic mass-loaded JET. The JET prevents cooling via heating, but anisotropically reorganizes condensation through compression, entrainment, and turbulent mixing. In the stronger-turbulence case, condensation starts later but becomes extended, filamentary, and mixed, with a broader hot-warm-cold bridge, a porous cocoon, and burst-dominated fueling. This run evolves toward a cloud-dominated state with inefficient central accretion. In the weaker-turbulence case, condensation starts earlier and remains coherent and centrally confined, yielding a regular cocoon, a longer-lived inner cold reservoir with sustained fueling. In both runs, condensation is suppressed inside the JET channel and survives in the surrounding atmosphere and along the JET-ambient interface. Once condensation begins, SMBH fueling becomes super-Bondi. These results extend CCA from a pure cooling + turbulence problem to a JET-regulated weather process. Ambient turbulence acts as a control parameter, producing an extended stormy phase, a centrally retained rainy cycle, and, in the high-turbulence case, a later cloudy state with inefficient central fueling. The meso scale emerges as the layer linking halo thermodynamics to SMBH feeding within the broader BlackHoleWeather framework.
[abstract 5 / 36] Yes (score: 5) - Title: BlackHoleWeather -- Spin-coupled chaotic cold accretion across the meso scale: Variability and kinematicsAuthors: Olmo Piana, Massimo Gaspari, Vieri Cammelli, Filippo Barbani, Davide M. Brustio, Giovanni Stel, Valeria Olivares, Ashkbiz Danehkar, Pasquale Temi, Roberto Serafinelli, Francesco Salvestrini, Filippo M. Maccagni, Francesco Tombesi,Comments: Submitted to A&A. Comments welcomeSubjects: astro-ph.GA astro-ph.HECreated: 2026-05-26; Updated: 2026-05-28; Datestamp: 2026-05-28
Supermassive BLACK HOLE (SMBH) spin records the vector history of accretion. In chaotic cold accretion (CCA), this history is set by clouds and filaments whose torques can add coherently, cancel, or reverse before reaching the horizon-scale closure. We test whether halo stirring regulates SMBH spin by changing the radial continuity and torque coherence of the meso-scale accretion bridge. We focus on spin evolution, JET-axis reorientation, accretion variability, and CCA kinematics. We analyse four 3D hydrodynamical simulations in a 100-kpc box, reaching sub-pc resolution, including SMBH spin-coupled JET feedback. All runs use the Hybrid SMBH spin model validated in a companion paper. Two simulations maintain continuous driven solenoidal turbulence, while two matched controls let the same initial turbulent field decay. The main effect of persistent stirring is to disrupt mass and angular-momentum continuity across the meso-scale bridge. Although all runs develop comparable macro-scale inflow, in the driven-turbulence suite, gas struggles to reach pc scales, and the radial accretion rate drops by 2-3 orders of magnitude. Torque delivery in this case is fragmented and cancellation-dominated. The interrupted-turbulence suite, on the other hand, preserves a connected gas channel to the sink, while sustaining higher torque coherence. Driven runs therefore settle to slow effective JET-axis drift, whereas interrupted runs maintain reorientation rates higher by about two orders of magnitude and can briefly reach a few degrees during coherent retrograde episodes. The same split appears in power spectra and k-plots: connected rain enhances low-frequency accretion power and produces narrower, phase-ordered kinematics, while stirring steepens high-frequency damping and broadens the gas velocity loci for all phases.
[abstract 6 / 36] Yes (score: 5) - Title: BlackHoleWeather -- Jet-regulated chaotic cold accretion across the meso scale: Variability and kinematicsAuthors: Vieri Cammelli, Massimo Gaspari, Filippo Barbani, Olmo Piana, Giovanni Stel, Davide M. Brustio, Valeria Olivares, Roberto Serafinelli, Pasquale Temi, Francesco Salvestrini, Michael Reefe, Filippo M. Maccagni, Francesco Tombesi,Comments: submitted to A&A; comments welcomeSubjects: astro-ph.HE astro-ph.GACreated: 2026-05-26; Updated: 2026-05-28; Datestamp: 2026-05-28
Chaotic cold accretion (CCA) predicts that supermassive BLACK HOLEs are fed by multiphase clouds condensing from turbulent hot atmospheres. In JET-regulated systems cold gas must also remain dynamically connected to the central accretion region. We investigate how a self-regulated kinetic JET modifies the kinematics, radial transport, and variability of CCA across the meso-scale of a typical galaxy-group atmosphere. The runs differ only in turbulent driving strength. We measure accretion histories, Eddington ratios, power spectra, phase-separated mass fluxes, projected k-plots, and cooling-to-eddy-time (C-ratio) profiles. Both runs become CCA-fed once precipitation begins, with accretion rising from Bondi-like to strongly super-Bondi values while remaining mostly low-Eddington and mechanically dominated. The strongly stirred run develops an early stormy phase with extended condensation, bursty feeding, and strong inflow/outflow variability, but later enters a cloudy phase in which cold and warm gas persist at meso- and inner macro-scales while sink coupling weakens. The calmer run maintains a compact rainy state with a longer-lived central reservoir. Accretion-rate spectra show flicker-like low-frequency slopes and red-noise tails; in the cloudy phase, the normalization drops and the low-frequency slope flattens. Phase-separated fluxes show fountain-like recycling in the strongly stirred run, but inner-kpc recycling in the calmer run. The JET excavates a hot channel where sustained condensation is suppressed, while C~1 is reached mostly outside the cone and near the JET-ambient interface. Jet-regulated CCA is controlled by meso-scale transport, not only by cold-gas production. Within the BlackHoleWeather framework, combined k-plot and C-ratio diagnostics are crucial to distinguish cold gas that is merely present from cold gas dynamically linked to SMBH feeding.
[abstract 7 / 36] Yes (score: 5) - Title: FERMI-LAT View on Three Ultra-high-energy 1LHAASO Sources in the $52^{\circ}[abstract 8 / 36] Yes (score: 4)Authors: Linjie Liu, Xian Hou, Pierrick Martin, Chuyuan Yang,Comments: 17 pages, 3 figures, 4 tablesSubjects: astro-ph.HECreated: 2026-05-27; Updated: 2026-05-28; Datestamp: 2026-05-28
Using more than 17 yr of FERMI-LAT data, we performed a detailed investigation of the complex $52^{\circ}
arXiv:2605.27510 [pdf, ps, other]X-ray quasi-periodic oscillations (QPOs) are a characteristic feature of low-mass X-ray binaries (LMXBs). These oscillations have been studied for decades and revealed a rich and complex phenomenology that is still not fully understood. RXTE archival studies have shown that the amplitude of these oscillations differs significantly between BLACK HOLEs (BH) with high or low inclination. Yet, the actual dependence on inclination has never been adequately estimated. Thanks to the improvement of inclination measurements through radio observations and the recent observations by the HXMT satellite, we quantified for the first time the dependence of Type-C QPO amplitudes on the JET inclination of individual BH LMXBs. Our analysis reveals the presence of a significant linear correlation up to 8 Hz, strengthening the case for a ''geometrical'' origin of the QPOs. In addition, for a given QPO frequency, we observe systematically lower amplitudes during the decay of outbursts compared to the rise. This data collection represents a key benchmark for any QPO model. Our comparison with the predictions from a precessing hot flow shows that the amplitude of the QPOs can be reproduced by this scenario if the spin-orbit misalignment is at least $\approx$10-15$^\circ$.
arXiv:2605.27629 [pdf, ps, other]We present an updated K band (24 GHz) celestial reference frame (CRF) constructed from 3.5 million Very Long Baseline Interferometry (VLBI) observations collected during 211 observing epochs between May 2002 and December 2025 using the Very Long Baseline Array (VLBA), the HARTRAO-HOBART26 baseline, the HARTRAO-YEBES40M baseline, and the Korean VLBI Network (KVN) augmented with several other VLBI stations. We have successfully observed and determined precise angular coordinates for 1317 compact extragalactic radio sources, essentially QUASARs, covering the full sky. This updated K band catalog is designated as CRF-K-2025. The precision of CRF-K-2025 is characterized by median scaled uncertainties of 60 and 104 micro-arc-seconds in right ascension and declination, respectively. The increase in number of observations and sensitivity over earlier K band campaigns has resulted in a catalog with 493 additional sources and a precision approximately 25% better than the ICRF3-K catalog, and similar to the ICRF3-SX catalog. At K band, these QUASAR radio sources generally show less extended emission than at lower frequencies and thus can potentially provide a more stable long term celestial reference frame than at the standard S/X (2.3/8.4 GHz) observing bands of ICRF3-SX.
arXiv:2510.14715 [pdf, ps, other]Recent long-term radio monitoring of tidal disruption events (TDEs) suggests that radio afterglows are common. Most studies argue that these afterglows may arise from forward shocks (FS) produced by the interaction between the TDE outflow and the hot, diffuse circumnuclear medium (CNM). Current theoretical models do not model the evolution of RELATIVISTIC electrons in space, which introduces uncertainties. Here we conducted hydrodynamic simulations to study the spatial evolution of RELATIVISTIC electrons, and calculated the SYNCHROTRON spectra via radiative transfer. We focus on the FS scenario with non-RELATIVISTIC outflows, and various parameters of the outflow and CNM are explored. A moderate outflow with kinetic energy of several $10^{50}$ erg in a Galactic center - like CNM can produce mJy-level radio afterglows at a distance of 100 Mpc. The self-absorption frequency exhibits a slow decline at early times and a rapid decrease at late times. We derived the temporal evolution of the high-frequency radio flux, revealing its characteristic rise and decline pattern. We also find that: (1) the radio spectra for narrow outflows are clearly anisotropic along different sight lines; (2) the FS parameters inferred from radio spectra using conventional analytical formulas deviate significantly from those in simulations, in which the inferred shock radii are half of those from simulations, and the inferred energies are an order of magnitude lower.
arXiv:2510.22190 [pdf, ps, other]Bent radio ACTIVE GALACTIC NUCLEi (RAGNs) -- wide-angle tails (WATs) and narrow-angle tails (NATs) -- trace dense environments in galaxy groups and clusters, yet no multiclass classifier simultaneously separates them from straight Fanaroff--Riley types (sFRI, sFRII) using visually inspected labels and unlabelled data. We release FIRST-2060, a four-class labelled dataset of 2060 RAGNs (sFRI, sFRII, WAT, NAT) constructed from three publicly available catalogues through multi-tier visual inspection, together with the semi-supervised RGC 1.0 model that leverages 20,000 unlabelled sources. We benchmark RGC against five supervised baselines. FIRST-2060 is provided in two preprocessing variants: $\mathbf{R}_{L1}$, which retains spurious sources, and $\mathbf{R}_{L2}$, from which they are removed. The RGC model integrates the self-supervised framework BYOL (Bootstrap Your Own Latent) with an $E(2)$-equivariant steerable CNN (E2CNN) encoder, pre-trained on the unlabelled data and fine-tuned on the labelled sets. All six models are evaluated with 5-fold cross-validation, Grad-CAM attention analysis, and controlled class-imbalance experiments. ConvNeXT ($M_1$) and RGC ($M_2$) form a top tier at macro-$F_1$ $0.80\pm0.02$ and $0.79\pm0.02$ respectively, a difference within one standard deviation. $M_2$ is the only model whose Grad-CAM contours consistently trace the morphological structure of RAGNs -- lobes, JETs, and bends -- rather than defaulting to compact blobs or diffuse patterns. The four-class scheme introduced here enables WAT/NAT-resolved catalogues that can serve as environment probes and progenitor classifications for diffuse cluster radio emission. The complementary strengths of $M_1$ and $M_2$ -- in cross-type and within-type discrimination respectively -- suggest that an ensemble approach may offer a practical framework for survey-scale morphological catalogues.
arXiv:2604.15012 [pdf, ps, other]Variations in the Faraday rotation measure (RM) of repeating fast radio bursts (FRBs) provide critical diagnostics of the dynamically evolving MAGNETo-ionic environments surrounding their progenitors. Sudden, transient ``RM flares'' can trace the passage of discrete MAGNETo-ionic structures, such as stellar coronal mass ejections from the companion or other dense plasma clumps, across the line of sight. However, identifying these rare events is difficult because RM evolution manifests a wide range of complex behaviors, from smooth, long-term trends to chaotic stochasticity, further complicated by highly non-uniform temporal sampling. This complexity makes it a non-trivial challenge to distinguish localized ``flares'' from intrinsic environmental volatility. We present a generalized algorithmic framework that establishes a robust methodology for the automated detection and characterization of RM flares. By isolating discrete transient perturbations from quiescent backgrounds, this pipeline enables the uniform census of environmental variability across the FRB population. Applying this framework to 15 repeating FRBs, we find that distinct RM flares are rare, with FRB 20220529A being the only source to exhibit an algorithmic detection under standardized parameters. Most of other active repeaters instead display high-level intrinsic fluctuations or secular evolution. This work provides a rigorous foundation for distinguishing between different modes of local plasma dynamics, offering a crucial diagnostic tool for identifying the diverse progenitor systems and local environments of FRBs.
arXiv:2605.23484 [pdf, ps, other]Solar radio bursts exhibit complex fine structures that reveal intricate coronal plasma dynamics. Here, we report detection of spike-like repeating burst pairs, characterized by two short-lived (0.1-2 s), narrowband components separated by about 4 s at frequencies 30-50 MHz. Using high-resolution dynamic spectra and spectroscopic imaging, we analyzed 613 burst pairs, measuring their durations, bandwidths, drift rates, flux densities, and spatial characteristics. Imaging links sources to an active region, with earlier components spatially concentrated above the region while delayed components are displaced and exhibit reduced drift rates. Radio-wave propagation simulations support the delayed bursts as turbulent echoes of harmonic emission in anisotropic coronal plasma. The location of the burst sources high in the corona suggests ongoing MAGNETic RECONNECTion and electron acceleration well above typical flare heights. Our findings offer new insights into coronal turbulence effects while advancing diagnostics of coronal plasma and the elusive nature of solar radio echoes from ground-based transmitters.
arXiv:2605.27504 [pdf, ps, other]Accretion onto supermassive BLACK HOLEs (SMBHs) in realistic halos is time-variable, governed by turbulence, cooling, and multiphase condensation. In chaotic cold accretion (CCA), clouds and filaments condense out of the hot gas and feed the SMBH stochastically. We investigate how turbulence regulates the variability, radial transport, and kinematics of CCA, focusing on the meso-scale connecting halo rain to inner inflow. We analyse 3D hydrodynamic simulations with a GPU-accelerated code, including cooling and driven subsonic turbulence in a stratified galaxy group, resolving scales from kpc to sub-pc and probing two turbulent weather regimes. In both regimes, SMBH accretion proceeds through CCA, remains super-Bondi, and varies by up to $\sim 2$ dex. The runs diverge mainly at meso-scales: strong stirring sustains fragmented feeding and clear inflow enhancement at 0.1-1 kpc, whereas weaker turbulence yields a smoother central cascade. Yet innermost feeding rates remain similar, implying SMBH accretion is not directly supply-limited by macro-scale weather. Accretion rate distributions peak at low Eddington ratios, indicating maintenance-mode state. Accretion rate power spectra follow a broken power law, with pink noise on long/intermediate timescales and a steeper red-noise tail at high frequencies, consistent with parsec-scale collisional damping. CCA modes are captured by two complementary diagnostics: the $\mathcal{C}$-ratio ($\equiv t_{\rm cool}/t_{\rm eddy}$) $\approx 1$ identifies soft X-ray gas as the gateway of condensation, while the k-plot (line broadening vs. shift) shows that the weather distinction is strongest on meso-scales, where the stormy regime produces broader, overlapping multiphase kinematics than the rainy regime. The meso-scale bridges halo rain and micro-scale CCA feeding, regulating spatial transport, kinematic imprint, and temporal coherence of SMBH growth.
arXiv:2605.27507 [pdf, ps, other]Supermassive BLACK HOLEs (SMBHs) self-regulate galaxies, groups, and clusters, yet the pathway transporting gas from halo scales to sub-pc radii remains debated. In hot stratified atmospheres, subsonic turbulence can trigger nonlinear thermal instability and a multiphase condensation cascade, producing chaotic time-variable BH `weather'. A key missing link is how the meso-scale connects halo rain to nuclear inflow. We study turbulence-driven condensation and chaotic cold accretion (CCA) in a group-scale halo, quantifying how the stirring level shapes multiphase morphology, thermodynamics, and SMBH feeding. We ran 3D hydrodynamic hyper-zoom simulations with a GPU-accelerated code, including cooling and driven subsonic turbulence in a hot intragroup halo. Two endpoint runs bracket weak and strong stirring, capturing distinct BH weather states. In both regimes the atmosphere becomes thermally unstable and develops a multiphase medium spanning 8-10 dex in temperature and density. Strong stirring delays cold gas accretion and sustains an extended filament-rich rain pattern to kpc radii (`stormy' CCA), with broader thermodynamic distributions beyond the nucleus. Weak stirring triggers earlier condensation but yields a more compact rain, with most cold gas confined within 100 pc (`rainy' CCA). At micro-scales the inflow is partly mediated by a clumpy rotating torus. Despite large differences in condensed cold mass, the BH accretion rate is recurrently boosted by up to 100x above the hot-mode Bondi baseline and varies weakly between the weather regimes, indicating that feeding is regulated primarily by how efficiently multiphase structures couple to the central inflow. Modest turbulence changes are sufficient to shift the same hot halo between stormy (extended) and rainy (centralized) BH weather, providing a quantitative multiscale baseline for interpreting multiphase CCA and SMBH feeding.
arXiv:2605.28777 [pdf, ps, other]Supermassive Population III.1 stars, i.e., formed from pristine, metal-free gas leading to conditions where DARK MATTER annihilation heating is significant, have been proposed as the progenitors of supermassive BLACK HOLEs (SMBHs) in the early universe ($z \sim 20-40$). Since such Pop III.1 stars only form from non-irradiated gas in DARK MATTER minihalos, they are predicted to appear isolated from each other and other sources of feedback. The previous papers in this series used the isolation distance of Pop III.1 stars as a free parameter to seed SMBH in cosmological simulations of DARK MATTER halos. Here we develop a feedback-regulated model of Pop III.1 isolation, based on the growth of HII regions around each Pop III.1 star and lower-mass, irradiated Pop III.2 stars. Our model considers the time delay between the formation of a minihalo and its Pop III.1 star, R-type expansion of HII regions that expand into the intergalactic medium (IGM), and the redshift dependence of Strömgren spheres for longer-lived ionizing sources. For a fiducial Pop III.1 star H-ionizing photon luminosity of $10^{53}\:{\rm s}^{-1}$ and lifetime of $10\:$Myr we find an R-type HII region radius of $R_{\rm R}\simeq1.3\:$cMpc, approximately independent of redshift. The median formation redshift is $\sim20$, with the process essentially complete by $z\sim16$. The overall number density of SMBHs produced in this model is then $n_{\rm SMBH}\simeq 3 ϕ_V/(4πR_{\rm R}^3)\simeq 0.2\:{\rm cMpc}^{-3}$. We also discuss predictions for the abundance of binary SMBHs, which may appear as dual ACTIVE GALACTIC NUCLEi (AGN; $\lesssim 0.3\%$ for $z>6$), and SMBH binary merger rates, measurable by the forthcoming LISA mission.
arXiv:2409.15413 [pdf, ps, other]Wide, highly eccentric ($e>0.9$) compact binaries can naturally arise as progenitors of gravitational wave (GW) mergers. These systems are expected to have a significant population in the mHz band (e.g., $\sim 3-45$ detectable stellar-mass binary BLACK HOLEs with $e>0.9$ in the Milky Way), with their GW signals characterized by "repeated bursts" emitted upon each pericenter passage. In this study, we show that the detection of mHz GW signals from highly eccentric stellar mass binaries in the local universe can strongly constrain their orbital parameters. Specifically, it can achieve a relative measurement error of $\sim 10^{-6}$ for orbital frequency and $\sim 1\%$ for eccentricity (as $1-e$) in most of the detectable cases. On the other hand, the binary's mass ratio, distance, and intrinsic orbital orientation may be less precisely determined due to degeneracies in the GW waveform. We also perform mock LISA data analysis to evaluate the realistic detectability of highly eccentric compact binaries. Our results show that highly eccentric systems could be efficiently identified when multiple GW sources and stationary Gaussian instrumental noise are present in the detector output. This work highlights the potential of extracting the signal of "bursting'' LISA sources to provide valuable insights into their orbital evolution, surrounding environment, and formation channels.
arXiv:2511.06733 [pdf, ps, other]Complicated hardenings and softenings of the spectra of COSMIC RAY protons and helium have been revealed by the newest measurements, which indicate the existence of multiple source populations of Galactic COSMIC RAYs. We study the physical implications of these results in this work. A phenomenological fitting shows that three components can properly give the measured structures of the proton and helium spectra. The data are then accounted for in a physically motivated, spatially-dependent propagation model. It has been shown that one background source population plus two local sources, or two background source populations plus one local source can well reproduce the measurements. The spectral structures of individual species of COSMIC RAYs are thus natural imprints of different source components of COSMIC RAYs. Combined with ultra-high-energy $γ$-ray observations of various types of sources, the mystery about the origin of Galactic COSMIC RAYs may be uncovered in future.
arXiv:2512.24433 [pdf, ps, other]One of the hallmarks of ACTIVE GALACTIC NUCLEi are that they are highly variable with time. In watching the spectra vary it has been observed that the emission-lines often appear to "reverberate" -- that is they vary in response to continuum variations assumed to originate close to the BLACK HOLE. This critical observation underlies the reverberation mapping technique, an elegant physics experiment that has allowed us to characterize the environment around many supermassive BLACK HOLEs in nearby ACTIVE GALACTIC NUCLEi. Recent observations are of such quality that the response can be measured as a function of velocity across the emission-line, and in doing so we can construct velocity-delay maps that show the structure and physics of the gas in the broad-line region better than any other measurement to date. Unfortunately constructing such maps requires a deconvolution, and given that the data are often noisy and with gaps such deconvolutions are non-trivial. Here we present a novel deconvolution method for the recovery of velocity-delay maps using a custom convolutional neural network architecture, showcasing that such methods have great promise for the deconvolution of reverberation mapping data products. While we have designed this new method with the BLR in mind, in principle this technique could be applied to any reverberation deconvolution problem, including in the accretion disk and torus.
arXiv:2602.02778 [pdf, ps, other]High-redshift QUASARs have been an excellent tracer to study the astrophysics and cosmology at early Universe. Using 577 spectroscopically confirmed high-redshift QUASARs and 1,796 highly reliable photometric QUASAR candidates (all with $5.0 \leq z < 6.2$, median $M_{1450} \sim -25.9$) selected via machine learning, we perform wide-field clustering analyses to investigate the large-scale environment of these objects. We construct the projected auto correlation function of those high-redshift QUASARs that is weighted by its predicted probability of being a true high-redshift QUASAR, from which we derive the bias parameter and the typical DARK MATTER halo mass of those QUASARs. The DARK MATTER halo mass of QUASARs estimated from the projected auto correlation function is $\log(M_h/M_{\odot})=12.13 \pm 0.07$ ($12.45 \pm 0.14$), with the bias parameter $b$ of $14.80 \pm 0.84 $ ($24.18 \pm 3.11$) for the redshift interval of $5.0 \leq z <5.6$ ($5.6 \leq z <6.2$). Moreover, we estimate the duty cycle of those QUASARs, which is $0.0002 \pm 0.0001$ ($0.0021^{+0.0049}_{-0.0014}$) for the redshift interval of $5.0 \leq z <5.6$ ($5.6 \leq z <6.2$), well aligning with the $f_{\rm duty} - M_{\rm halo}$ scaling relation. These comparably small duty cycle estimates might indicate that a significant fraction of supermassive BLACK HOLE growth occurs in an obscured phase.
arXiv:2602.10462 [pdf, ps, other]Massive scalar charges are ubiquitous in extensions to General Relativity and the Standard Model in particle physics. We describe spectral methods which can accurately construct the spacetime of rotating BLACK HOLEs with dimensionless spin up to $a \leq 0.8$ surrounded by massive scalar fields nonminimally coupled to spacetime curvature. We consider axi dilaton, dynamical Chern Simons, and scalar Gauss Bonnet couplings, and obtain leading order solutions for both the scalar field and the associated metric modifications. Our method accurately resolves massive scalar fields with Compton wavelengths as short as 5 times the BLACK HOLE mass, achieving residual errors $\lesssim 10^{-5}$, and yields the corresponding leading order spacetime modifications with residual errors $\lesssim 10^{-3}$. Using the constructed spacetimes, we computes the leading-order shifts in the surface gravity and the angular velocity of the event horizon, important information for computing the quasinormal modes. These results pave the way to incorporate massive scalar charges into electroMAGNETic observations and gravitational-wave detections of BLACK HOLEs, potentially enabling new probes of fundamental scalar degrees of freedom.
arXiv:2605.03271 [pdf, ps, other]The idea of an energy cascade in the inertial range is often invoked in turbulent space plasmas to estimate the energy dissipation rate. Laws governing the behavior of third-order structure functions in the inertial range, so-called third-order laws, are among the few rigorous theoretical results quantifying cross-scale energy transfer. The widely used third-order-law derived rate assumes isotropy, which fundamentally conflicts with the anisotropic nature of space plasmas. Elementary questions persist regarding how such anisotropic energy cascades can be quantified using multi-spacecraft constellations. As the heliospheric community increasingly progresses towards multi-spacecraft, multi-scale constellations, such as Plasma Observatory and HelioSwarm, we revisit these crucial issues pertinent to accurately measuring the inertial-range energy transfer. Here we make a systematic comparison between two methods: direction-averaging (DA) and lag polyhedral derivative ensemble (LPDE) to determine the full three-dimensional (3D) dependence of cross-scale energy transfer. We find that DA exhibits both polar and azimuthal dependence, but is insensitive to spacecraft configuration. By contrast, LPDE is strongly affected by spacecraft separation and tetrahedral shape, while being comparatively insensitive to the sampling trajectory. Our findings have direct implications for current and future multi-spacecraft missions. Both DA and LPDE will provide crucial information on the nature of turbulence in space and astrophysics.
arXiv:2605.15265 [pdf, ps, other]Eccentric binary BLACK HOLEs (BBHs) formed through dynamical interactions can significantly contribute to gravitational wave (GW) detections. In this work, we present a simulated catalog of dynamically-formed, stellar-mass BBHs in the local universe, incorporating contributions from the Galactic field (flyby interactions), Galactic nucleus (eccentric Kozai-Lidov evolution), and globular clusters (N-body interactions). Our results predict a wide, highly eccentric BBH population in the Milky Way (MW), with source counts of $\sim 36, 13, 4.7, 2.3, 1.0$ (for $\mathrm{SNR} > 1, 3, 8, 20, 50$, respectively) during a 10-yr LISA observation. Extending this model to cosmological populations, we show that different dynamical channels can produce distinct eccentricity distributions in the LVK band and can contribute hundreds of additional low-SNR mHz sources. Specifically, our model yields a merger rate of $Γ\sim 9 \mathrm{Gpc}^{-3}\mathrm{yr}^{-1}$ and $\sim 490$ extragalactic mHz BBHs with $\mathrm{SNR} > 1$. However, due to the lower mass and weaker GW signals of stellar-mass BBHs, this number declines sharply at higher detection thresholds (e.g., $\sim 1$ for $\mathrm{SNR} > 8$). We further highlight the impact of eccentric BBH signals on the LISA global fit, showing that their individual harmonics can be independently detected in the Milky Way, and may mimic circular binaries with systematically biased chirp masses. Lastly, we show that post-Newtonian waveforms converge reliably for eccentric BBHs with masses of $\lesssim 10^3 M_\odot$ in the mHz band. Overall, eccentric BBHs represent a prevalent and promising target for future space-based GW observatories. The simulated catalog and the LISA Eccentricity Astrophysics Package (LEAP) developed in this work are publicly available at https://github.com/zeyuanxuan/lisa-leap/.
arXiv:2605.27549 [pdf, ps, other]This work presents the compact experimental negative triangularity reactor (CENTAUR), a low overnight cost, high-field tokamak, breakeven reactor design, achieving a predicted total fusion power of 40MW and scientific energy gain of 1.3. Ballooning stability calculations confirm that the device's pedestal is within the first stability regime, which is consistent with the expected ELM-free operation associated with negative triangularity (NT) plasmas. The geometry of the NT divertor allows for high fraction of radiated power (13.5$\%$) between the separatrix and plasma facing components. Heat transport modeling based on simulations of the edge region show heat loads into plasma facing components well below material limits. The MAGNET system employs rare-earth barium copper oxide (REBCO) high-temperature superconductors in 18 toroidal field coils, an hourglass-shaped central solenoid, and six poloidal field coils to support high-field ($B_0=10.9$ T) plasma confinement, shaping, and current drive. Neutronics analysis shows that a 12 cm $B_4C$ shield keeps superconducting MAGNET heating below the 33~K quench limit during 10 s, 40 MW DT pulses. With this shielding, the modeled fluence indicates HTS components can survive more than ten times the 3000-pulse design lifetime. Iteration of economic analysis in tandem with the technical design process allows CENTAUR to achieve its overnight cost goal of $\$$2B determined using a custom costing model that predicts a total overnight cost of $1.6$B$\pm0.2$B.
arXiv:2605.27728 [pdf, ps, other]We investigate the appearance of a low-frequency 1/f MAGNETic spectrum in three-dimensional incompressible MAGNETohydrodynamic turbulence using direct numerical simulations and virtual spacecraft sampling. Our goal is to determine how the measured temporal spectra depend on the mean MAGNETic guide field, the probe velocity relative to the Alfvén speed, and the sampling angle with respect to the guide field. We find that the clearest 1/f ranges are obtained for stronger guide fields and are favored by faster sampler trajectories oriented more nearly perpendicular to the mean MAGNETic field. To characterize this behavior, we introduce a quantitative score that measures the quality and spectral coverage of the detected 1/f interval. We further show that, as the probe speed increases, the measured temporal spectra become progressively more consistent with a direct mapping between spatial and temporal fluctuations, particularly for nearly perpendicular sampling in the strong guide field case. These results indicate that the presence and clarity of a temporal 1/f range depend not only on the underlying turbulent dynamics, but also on the geometry and speed of the sampling process, with implications for the interpretation of low-frequency in situ measurements in the solar wind.
arXiv:2605.27871 [pdf, ps, other]The role of a transverse liquid n-heptane JET in initiating and stabilizing liquid n-heptane oblique detonation waves (ODWs) in a confined model combustor was computationally investigated in the present work. The JET-to-inflow momentum ratio, J, was identified as the primary control parameter. Under steady inflow pressures, a weak JET with a small J fails to initiate an ODW; a slightly stronger JET ignites only a local near-normal detonation between the OSW and the separation shock wave without forming a developed ODW branch; a moderate JET establishes a standing detonation wave system consisting of an ODW, a near-normal detonation branch, and a separation shock wave; a large but still admissible J produces a wall-coupled ODW-Mach-stem configuration; and an excessive JET momentum destabilizes the ODW by pushing it out of the combustor into the external compression region. Under oscillatory inlet pressure, the standing ODW remains dynamically stabilized within the combustor through bounded, phase-dependent transitions between distinct combustion modes. At sufficiently large J, the transverse JET ceases to act as an effective stabilization actuator. The resulting dynamic-stabilization map reveals a finite operating window governed jointly by JET momentum and inlet-pressure fluctuation.
arXiv:2605.27903 [pdf, ps, other]We utilize JWST imaging of the massive lensing cluster field A2744 to find close pairs of compact sources with separations less than 0.25". A large fraction of these "Double Dots" correspond to Little Red Dots (LRDs) or high-redshift broad-line ACTIVE GALACTIC NUCLEi (BLAGNs). Our analysis of 31 identified pairs reveals a median separation of 0.15". Statistical comparison against a uniform background shows that these are mostly physical pairs. We find that at least 16 of the 24 previously published LRDs in this field (~67%) are such pairs, as are both of the high-redshift BLAGNs. We demonstrate that the presence of a companion can significantly contaminate the measured spectral energy distribution, potentially masking the characteristic ``v-shape" used for LRD classification. Furthermore, our 2D spectroscopic analysis of several pairs reveals that BLAGN activity is not confined to the redder member of the pair but can originate in either one. Since most LRDs contain broad emission lines, our findings suggest that close pairs are extremely effective markers of galaxies with broad lines at high redshift. We speculate on possible mechanisms, concluding that we are likely seeing merger-driven accretion.
arXiv:2605.27953 [pdf, ps, other]Effective field theory (EFT) provides a systematic framework for parametrizing possible higher-energy corrections to general relativity through higher-curvature interactions. In this work, we investigate gravitational lensing in both weak- and strong-field regimes for EFT-corrected Reissner-Nordström BLACK HOLE spacetimes, focusing on both weakly charged and near-extremal configurations. Using the strong deflection limit formalism, we derive the corresponding corrections to the deflection angle, photon sphere radius, critical impact parameter, and strong lensing coefficients induced by higher-derivative curvature-electroMAGNETic interactions. Our analysis is restricted to purely geometrical corrections associated with modifications of the background spacetime geometry, without including POLARIZATION-dependent corrections to the photon propagation law. We show that strong gravitational lensing observables in charged BLACK HOLE backgrounds can provide complementary probes of effective interactions between gravity and electroMAGNETic fields. These results suggest that future high-precision observations of strong lensing phenomena may place constraints on higher-curvature EFT couplings beyond general relativity.
arXiv:2605.28024 [pdf, ps, other]A mechanism of resonant excitation of surface MAGNEToplasmons (SMPs) is proposed in the terahertz (THz) frequency range by {\emph{beating of two p-polarized LASERs}}, obliquely incident at an angle $θ$ on a graphene sheet deposited over a rippled surface of a MAGNETized n-type semiconductor. The resulting LASER-beat-envelope induces a nonlinear velocity to free electrons, which couples with the modulated charge carrier density and generates a nonlinear current. This time-varying oscillating nonlinear current acts as the source of THz SMPs wave generation, as opposed to THz generation by a different process with {\emph{a single LASER}} in the earlier work [Phys. Rev. E 113, 015208 (2026)] where light dispersion characteristics as well as the required phase-matching conditions are markedly different. The resulting THz SMPs field amplitude is shown to be controlled in the frequency range of $2-5$~THz by varying the graphene's FERMI energy ($\textrm{E}_\textrm{F}=20-130$ meV), LASER incident angle ($θ= 0-90^{o}$), the semiconductor's temperature ($T = 320 - 380$~K) and external MAGNETic field ($\textrm{B}_{0} \approx 0 - 0.09 $~T). The amplitude of THz SMPs field now reaches on the order of $10^{-1}$ w.r.t. the incident field amplitude, and it is almost $10^1 - 10^2$ fold higher compared to previous works. Thus, the proposed mechanism may open new avenues for the development of actively tunable plasmonic device, with potential applications in future THz technologies and 6G wireless communication systems.
arXiv:2605.28370 [pdf, ps, other]We develop an analytical theory of coherent (scaled quadratically with the number of particles) radiation and coherent radiation friction in a head-on collision of a dense charged particle bunch with an intense LASER pulse. We demonstrate that the low-frequency coherent radiation in the forward and backward directions dominates the energy-momentum losses of a mildly RELATIVISTIC bunch and can result in a substantial enhancement of the overall radiation friction as compared to the incoherent case. We derive the scaling laws for the average momentum losses of the bunch over the collision with respect to LASER intensity, pulse duration, and particle bunch parameters, and show their robustness with respect to LASER POLARIZATION and the shape of the particle distribution in the bunch.
arXiv:2605.28407 [pdf, ps, other]Measurements of interplanetary MAGNETic fields have long relied on spacecraft measurements, which provide only in-situ sampling and therefore cannot capture the global MAGNETic structure. Faraday rotation of radio signals extends in-situ measurements to line-of-sight measurements, but it still depends on the number and spatial distribution of available radio sources. The Zeeman effect offers another route to remote sensing of MAGNETic fields, but it is generally too weak to diagnose the weak interplanetary MAGNETic fields. Here, we present a remote-sensing method to constrain weak MAGNETic field strength and orientation using spectral-line POLARIZATION induced by ground-state alignment (GSA) and Hanle effect, with collisional effects taken into account. This method is sensitive to weak MAGNETic fields in environments ranging from the high solar atmosphere and solar wind to the outer heliosphere, and we identify suitable spectral lines for different targets. We further perform forward modeling of Mercury's MAGNETosphere to demonstrate the feasibility of this imaging method. Spectral-POLARIZATION imaging therefore provides a new way toward remote imaging of dynamic heliospheric MAGNETic structures.
arXiv:2605.28580 [pdf, ps, other]We investigate perturbative dynamics, tidal effects, and RELATIVISTIC frequency shifts in a dyonic Kalb-Ramond BLACK HOLE generated by a Lorentz-violating antisymmetric tensor background. The geometry is controlled by the mass $M$, the electric charge $Q$, the MAGNETic charge $p$, and the Lorentz-violating parameter $\ell$, with the dyonic sector entering through the effective combination $P_{\ell}^{2}=Q^{2}/(1-\ell)^{2}+p^{2}/(1-2\ell)$. First, we analyze the gravitational Doppler effect for radial signal exchange between freely falling and static observers, showing how the dyonic charges weaken the redshift by shifting the frequency ratio toward unity. We then compute the radial and angular tidal forces in a freely falling frame and determine the characteristic radii at which the usual stretching and compression patterns are reversed. The gravitational time delay is also evaluated for null trajectories, showing that the electric and MAGNETic sectors reduce the delay relative to the reference configuration. In the perturbative sector, we derive the scalar, vector, tensor, and spinor effective potentials and compute the corresponding quasinormal frequencies through the sixth-order WKB method. The numerical spectra indicate that the Lorentz-violating parameter gives the dominant correction, increasing the oscillation frequencies and modifying the damping rates, while the dyonic charges produce milder shifts. Finally, the time-domain profiles confirm the presence of damped quasinormal ringing followed by late-time power-law tails.
arXiv:2605.28658 [pdf, ps, other]The measurement of the Hubble constant $H_0$ plays a central role in modern cosmology. In this work, we investigate the potential of strongly lensed gravitational-wave (SLGW) signals from massive binary BLACK HOLE mergers to constrain $H_0$ using future space-based detector networks. We consider two observational scenarios: one in which the source redshift is unknown, and another in which it is independently determined through electroMAGNETic observations. We show that meaningful constraints on $H_0$ can still be achieved without source-redshift information, provided that the lens redshift is known. For individual SLGW events, the joint Taiji+LISA analysis improves the measurement precision of $H_0$ by approximately a factor of two compared with the Taiji-only configuration. Extending the analysis to the population level, we combine five simulated SLGW events and find that the uncertainty in $H_0$, quantified by the 95\% credible interval, reaches the $1.1\times10^{-1}$ level when the source redshift is treated as unknown, and further improves to $4.2\times10^{-2}$ when the source redshift is independently measured. Our results demonstrate that joint space-based gravitational-wave observations can substantially enhance the cosmological capability of SLGW events and provide a promising avenue for precision measurements of the Hubble constant.
arXiv:2605.28662 [pdf, ps, other]We employ the sample of 244 GAMMA-RAY BURSTs (GRBs; i.e., C244) with the Combo correlation to test cosmic anisotropy. Meanwhile, the Pantheon sample is introduced to verify whether the GRB sample can suppress the fake anisotropic signals induced by inhomogeneous spatial distributions. In the dipole fitting (DF) method, under the dipole-modulated $Λ$CDM model, the C244 sample shifts the best-fitting longitude $l$ derived from the Pantheon sample by $54.09^\circ$ and reduces the uncertainty in $l$ by approximately $40\%$. Compared to the 118 GRBs (i.e., A118) with the $E_\mathrm{p}$-$E_\mathrm{iso}$ correlation, the shift in longitude $l$ increases by additional $21.35^\circ$. In the hemisphere comparison (HC) method, the preferred direction derived from the C244+Pantheon sample deviates from that of the Pantheon-only sample by more than $1σ$. In contrast, the preferred direction from the A118+Pantheon sample is consistent with the Pantheon-only result within the $1σ$ uncertainty. The preferred direction changes significantly as the number of GRBs increases from 118 to 244. Our results show that a larger GRB sample can reduce the fake anisotropic signals caused by inhomogeneous spatial distributions. Accordingly, we suggest that GRBs have the potential to provide a reliable probe of cosmic anisotropy.
arXiv:2605.28663 [pdf, ps, other]We present a systematic theoretical framework for investigating first-order electroMAGNETic (EM) perturbations induced by gravitational waves (GWs). Beginning with the covariant Maxwell equations, we derive the complete first-order perturbation equations in terms of both the EM field tensor and the four-potential, demonstrating their equivalence alongside the residual gauge invariance under the Lorenz gauge condition. Furthermore, explicit first-order expressions for the induced electric and MAGNETic fields, as well as the associated EM energy-momentum tensor, are obtained. As an explicit illustration, we analytically evaluate the interaction between a plane EM wave and a GW within the transverse-traceless gauge. By demonstrating that the maximum modulus of the coupling coefficient is on the order of $10^2$, we quantitatively establish that a typical astrophysical GW with a dimensionless strain of $h_0 \sim 10^{-21}$ generates a first-order EM response on the order of $10^{-19}$ relative to the incident field amplitude.
arXiv:2605.28715 [pdf, ps, other]Title: Accurate waveforms for generic planar-orbit binary BLACK HOLEs: The multipolar effective-one-body model SEOBNRv6EHMAuthors: Aldo Gamboa, Alessandra Buonanno, Lorenzo Pompili, Raffi Enficiaud, Michael Boyle, Lawrence E. Kidder, Oliver Long, Peter James Nee, Harald P. Pfeiffer, Antoni Ramos-Buades, Mark A. Scheel,Comments: 64 pages, 23 figuresSubjects: gr-qc astro-ph.HECreated: 2026-05-27; Updated: 2026-05-28; Datestamp: 2026-05-28Accurate and computationally efficient waveform models are required to infer the parameters of compact binaries from their gravitational wave (GW) emission. Among these parameters, orbital eccentricity serves as a smoking gun for dynamical formation channels and must be accounted for to avoid systematic errors in GW analyses. Here, we present SEOBNRv6EHM, a time-domain, multipolar waveform model for binaries on generic planar orbits, calibrated to quasi-circular (QC) numerical-relativity (NR) simulations from the SXS collaboration. In addition to the dominant $(2,2)$ mode, the model provides the $(2,1)$, $(3,3)$, $(3,2)$, $(4,4)$, and $(4,3)$ multipoles for the full inspiral-merger-ringdown process of coalescing binaries, as well as for dynamical captures and scattering encounters. The model is built within the effective-one-body (EOB) framework, and it employs novel resummations of the radiation-reaction force and waveform modes. We validate its accuracy through comparisons against 592 QC, 319 eccentric, one dynamical-capture, and two scattering SXS NR waveforms, and through scattering-angle comparisons against 61 SXS NR simulations. For QC and small-eccentricity binaries, its accuracy is comparable to previous-generation SEOBNRv5 models. For highly eccentric systems, however, SEOBNRv6EHM attains unprecedented accuracy, with waveform mismatches remaining below or close to $ 2\% $ across the total mass range $ 20-200\, \mathrm{M}_\odot $ for eccentricities up to $\sim 0.9$ at 14 periastron passages before merger. Additionally, SEOBNRv6EHM achieves waveform-generation walltimes that are $ 2 - 6 $ times faster than other state-of-the-art EOB eccentric models, enabling efficient and accurate applications in GW astronomy.
arXiv:2605.27502 [pdf, ps, other]
arXiv:2605.28676 [pdf, ps, other]
arXiv:2605.03033 [pdf, ps, other]
arXiv:2605.27503 [pdf, ps, other]
arXiv:2605.27508 [pdf, ps, other]
arXiv:2605.27511 [pdf, ps, other]
arXiv:2605.28081 [pdf, ps, other]