Current date: 2026-06-03
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Created/updated limit: 2026-05-27 (7 days ago)
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Suggested sets: physics, physics:astro-ph, physics:gr-qc, physics:physics
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OAI-PMH request: http://export.arxiv.org/oai2?verb=ListRecords&from=2026-06-03&until=2026-06-03&set=physics&metadataPrefix=arXiv
Scoring abstracts
Number of records retrieved: 158
Keyword score statistics
score 6 -- 1 abstracts
score 5 -- 1 abstracts
score 4 -- 2 abstracts
score 3 -- 1 abstracts
score 2 -- 6 abstracts
in total -- 11 abstracts
Articles that appeared on 2026-06-03
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[abstract 1 / 11] Yes (score: 6)
- Title: The Life and Death of Stars That Capture Primordial Black HolesAuthors: Ore Gottlieb, Matteo Cantiello, Cameron Norton, Ken Van Tilburg, Matthew Kleban,Comments:Subjects: astro-ph.HE astro-ph.CO astro-ph.SR gr-qcCreated: 2026-06-01; Updated: 2026-06-03; Datestamp: 2026-06-03
Primordial BLACK HOLEs (PBHs) in the asteroid mass window ($10^{17}-10^{23}\,{\rm g}$) remain viable DARK MATTER candidates and can be captured by stars. We develop the first global framework for the evolution of stars that capture PBHs, combining analytic calculations, stellar evolution models, 3D general-RELATIVISTIC MAGNETohydrodynamic simulations, and Monte Carlo population synthesis. We find that the fate of these systems bifurcates: PBHs that form an accretion disk before consuming the host drive explosive disruption, whereas PBHs captured too late or growing too slowly consume the star quietly. Capture is dominated by three-body interactions with planetary or stellar companions. For a solar-type host with a Jupiter analog, inspiral within a main-sequence lifetime requires $M_{\rm BH}^{\rm crit}\gtrsim 10^{22}\,{\rm g}$, while lighter PBHs generally require tighter companions. Once deposited at the center, the PBH grows through inefficient quasi-spherical Bondi accretion; if it reaches the angular-momentum threshold before consuming the host, the inflow circularizes into a disk. Our Monte Carlo calculations yield sizable quiet-consumption and explosive-disruption populations, with final PBH masses $M_{\rm BH}\sim0.01-1\,M_\odot$ and disk-forming PBH spins $a_\ast\approx0.8$. Disk formation is the point of no return: disk winds and RELATIVISTIC JETs of $\sim10^{45}-10^{50}\,{\rm erg\,s^{-1}}$ disrupt the star within minutes. The resulting transients may include a $\sim$day-long UV/blue signal, radio afterglow, and, if the JET escapes, an X-ray-flash/low-luminosity gamma-ray-burst (XRF/llGRB) signal. For an $O(1)$ PBH DARK MATTER fraction and optimistic capture assumptions, the event rate can reach that of llGRBs. The low-mass, high-spin remnants offer a complementary PBH probe and possible source for subsolar BH mergers.
[abstract 2 / 11] Yes (score: 5) - Title: Systematic Error in Approximate Models of the GRB Early AfterglowAuthors: Benjamin Amend, Eric R. Coughlin, Jonathan Zrake,Comments:Subjects: astro-ph.HECreated: 2026-06-01; Updated: 2026-06-03; Datestamp: 2026-06-03
Gamma-ray burst (GRB) afterglows are thought to arise when RELATIVISTIC ejecta launched by a compact central engine drive a blast wave into the surrounding circumburst medium, producing broadband SYNCHROTRON emission. We present a rigorous assessment, based on high-resolution special RELATIVISTIC hydrodynamics simulations, of a widely adopted `two-zone model' for approximating the dynamics of the early afterglow phase. Before the onset of the Blandford-McKee (BMK) self-similar solution, the outflow generally produces two emission components, associated with the forward-shocked circumburst medium and the reverse-shocked ejecta. The subsequent evolution depends on whether the reverse shock significantly decelerates the ejecta as it crosses the shell, separating the so-called RELATIVISTIC and Newtonian reverse shock regimes. We show that when the reverse shock is Newtonian, it crosses the ejecta shell long before BMK self-similarity is established, leaving a prolonged interval that can span $\sim$ hours in observer time in which the true hydrodynamic evolution is not captured by standard semi-analytic prescriptions. We demonstrate that this mismatch can substantially overpredict the reverse-shock emission from radio through ultraviolet frequencies, or overpredict the forward-shock emission at X-ray frequencies, depending on how the transition away from the two-zone model is prescribed.
[abstract 3 / 11] Yes (score: 4) - Title: A recoiling supermassive BLACK HOLE in a powerful QUASARAuthors: Marco Chiaberge, Takahiro Morishita, Matteo Boschini, Stefano Bianchi, Alessandro Capetti, Gianluca Castignani, Davide Gerosa, Masahiro Konishi, Shuhei Koyama, Kosuke Kushibiki, Erini Lambrides, Eileen T. Meyer, Kentaro Motohara, Massimo Stiavelli, Hidenori Takahashi, Grant R. Tremblay, Colin Norman,Comments: 36 pages, 10 figures, revised version after referees' commentsSubjects: astro-ph.GA gr-qcCreated: 2026-06-01; Updated: 2026-06-03; Datestamp: 2026-06-03
Supermassive BLACK HOLEs (SMBH) are thought to grow through accretion of matter and mergers. Models of SMBH mergers have long suffered the final parsec problem, where SMBH binaries may stall before energy loss from gravitational waves (GW) becomes significant, leaving the pair unmerged. Direct evidence of coalesced SMBH remains elusive. Theory predicts that GW recoiling BLACK HOLEs can occur following a BLACK HOLE merger. Here we present new and conclusive spectroscopic evidence that both the accretion disk and the broad line region in the spatially offset QUASAR 3C 186 are blue-shifted by the same velocity relative to the host galaxy, with a line of sight velocity of (-1310 +- 21) km/s. This is best explained by the GW recoil super-kick scenario. This confirmation of the ejection process implies that the final parsec problem is resolved in nature, providing evidence that even the most massive BLACK HOLEs can merge.
[abstract 4 / 11] Yes (score: 4) - Title: Elemental COSMIC RAY spectra reveal two populations of Galactic sources and an immediate transition to an extragalactic component after the kneeAuthors: Timur A. Dzhatdoev, Anatoly A. Semenov,Comments: 8 pages, 6 figuresSubjects: astro-ph.HECreated: 2026-06-01; Updated: 2026-06-03; Datestamp: 2026-06-03
The energy spectra for individual elements and/or for groups of elements in COSMIC RAYs (CR) in the energy range between 100 $\times$ Z GeV and 10$^{3}$ $\times$ Z PeV (where Z is the charge number of the nucleus) have a number of features, including two steepenings ("knees") with the rigidity-dependent energies $E_{k1} \approx$ 15 $\times$ Z TeV and $E_{k2} \approx$ 3 $\times$ Z PeV and three hardenings ("ankles") at $E_{a1} \approx$ 500 $\times$ Z GeV; for protons $E_{a2-p} \approx$ 150 TeV and $E_{ a3-p} \approx$ 100 PeV. While the values of $E_{a1}$ for different nuclei are rigidity-dependent, the values of $E_{a2}$ (and probably of $E_{a3}$) are not: $E_{a2-He} \approx$ 1 PeV for Helium. The recent advances in precision measurements of the elemental CR spectra in the DAMPE and LHAASO experiments, and, to some extent, in IceTop and other experiments, make it possible, for the first time, to clarify the origin of the aforementioned spectral features. We show that the elemental CR spectra are reasonably well described with a sum of three components: 1) a low-energy Galactic component with a convex spectral shape reflecting the accelerated particle spectrum in the source; this component peters out after the TeV knee, 2) a high-energy Galactic component including the PeV knee, and 3) an extragalactic component. There is no need for any third, additional component of Galactic COSMIC RAYs in the energy range between 10 PeV and 1 EeV.
[abstract 5 / 11] (score: 3) - Title: Eigenmodes in an ultra-RELATIVISTIC ultra-MAGNETized pair QED-plasmaAuthors: Ryan T. Low, Mikhail V. Medvedev,Comments:Subjects: physics.plasm-ph astro-ph.HECreated: 2026-06-01; Updated: 2026-06-03; Datestamp: 2026-06-03
Ultra-RELATIVISTIC quantum-electrodynamic (QED) plasmas, characterized by MAGNETic field strengths approaching and even exceeding the Schwinger field of approximately $B_{Q} \approx 4 \times 10^{13}$ gauss, hold significant interest for LASER-plasma experiments and astrophysical observations of neutron stars and MAGNETars. In this study, we investigate the joint modification of normal plasma modes in ultra-RELATIVISTIC electron-positron plasmas, both charge neutral and non-neutral, by the super-strong MAGNETic field and plasma RELATIVISTIC temperature. Our analysis shows that the most substantial modification concerns the reduction of the plasma frequency cutoff, resulting in RELATIVISTIC and field-induced transparency. Additionally, we observe a temperature-independent modification of the index of refraction of electroMAGNETic waves, which coincides with the behavior observed in a cold QED plasma.
[abstract 6 / 11] (score: 2) - Title: The Impact of Population III.1 Flash Reionization for CMB Polarization and Thomson Scattering Optical DepthAuthors: Jonathan C. Tan, Eiichiro Komatsu,Comments: Accepted to Astrophysical Journal LettersSubjects: astro-ph.COCreated: 2026-06-01; Updated: 2026-06-03; Datestamp: 2026-06-03
The Population III.1 theory for supermassive BLACK HOLE (SMBH) formation predicts a very early ($z\sim20-25$) transient phase, the ``Pop III.1 Flash'', of cosmic reionization powered by supermassive stars that are SMBH progenitors. The universe then quickly recombined to become mostly neutral, with this state persisting until galaxies begin to reionize intergalactic gas again at $z\sim 10$. The overall Thomson scattering optical depth, $τ$, from the Pop III.1 Flash has been shown to be $τ_{\rm PopIII.1}\sim0.03$, leading to a total $τ\sim0.08-0.09$. Such a value, while significantly larger than that previously inferred from {\it Planck} observations of the low-$l$ $EE$ POLARIZATION power spectrum of the CMB, can help relieve several ``tensions'' faced by the standard $Λ$CDM cosmological model, especially the preference for negative neutrino masses and dynamic DARK ENERGY. Here we compute $EE$ power spectra of example models of the Pop III.1 Flash. We find that, because of its very high redshift, the contribution to $l\lesssim\:$6 modes is dramatically reduced compared to usual low-$z$ reionization models for the same value of $τ$, while the power at $l\gtrsim\:$6 is boosted. Thus the Pop III.1 reionization scenario provides a natural way to increase $τ$, while remaining closer to the latest CMB low-$l$ POLARIZATION observations.
[abstract 7 / 11] (score: 2) - Title: MCMC Constraints on Dyonic Kalb-Ramond Black Holes with a Cloud of Strings from Twin-Peak QPOs and EHT ShadowsAuthors: Faizuddin Ahmed, Ahmad Al-Badawi, İzzet Sakallı,Comments: 27 pages, 11 Figures, 11 Tables (comments are welcome)Subjects: gr-qc hep-thCreated: 2026-06-01; Updated: 2026-06-03; Datestamp: 2026-06-03
We study a dyonic BLACK HOLE in a Lorentz-violating gravity that carries a background Kalb--Ramond field and is pierced by a cloud of strings. The resulting metric reduces to the recent Lin--Liu--Liu solution when the string density~$ξ$ is switched off, and to the Duan and Yang solutions in further degenerate limits. We work out the timelike circular geodesics and read off the quasi-periodic oscillation (QPO) frequencies $ν_ϕ$, $ν_r$ and $ν_θ$ within both the RELATIVISTIC-precession and epicyclic-resonance models. We then map these frequencies onto the observed twin-peak signals of XTE~J1550$-$564, GRO~J1655$-$40 and GRS~1915$+$105, and place constraints on $(\ell, ξ)$ from a Markov chain Monte Carlo (MCMC) fit. We extract the full thermodynamic dictionary, first law and Smarr relation included, and follow the heat capacity, free energy and sparsity of Hawking radiation through their dependence on the four parameters $(M, Q, p, \ell, ξ)$. Finally, we compute the spectral energy emission rate and look at the photon-sphere and shadow radii in the presence of the cosmic string. The Lorentz-violating coupling $\ell$, the MAGNETic charge $p$, and the string density $ξ$ all leave distinct fingerprints on the dynamical, thermodynamic and radiative observables, with $ξ$ exerting the strongest pull on the ISCO, the shadow size and the sparsity of Hawking emission
[abstract 8 / 11] (score: 2) - Title: The Role of Stellar Spin in Repeating Partial Tidal Disruption EventsAuthors: Ananya Bandopadhyay, Benjamin Amend, Eric R. Coughlin, C. J. Nixon, Dheeraj R. Pasham, T. Wevers,Comments: 9 pages, 5 figures, 1 appendix; submittedSubjects: astro-ph.HECreated: 2026-06-01; Updated: 2026-06-03; Datestamp: 2026-06-03
The repeated tidal stripping of a star by a supermassive BLACK HOLE, known as a repeating partial tidal disruption event (rpTDE), can give rise to a transient that rebrightens months to years after the first outburst. Among the rpTDE candidates so far observed, some exhibit dimmer peak luminosities during each successive outburst, which is a trend that has not been reproduced from theoretical models when the star survives more than one encounter with the BLACK HOLE. Here we suggest that this trend can be recovered if the partially disrupted star is initially (i.e., prior to its first mass-stripping event) rapidly rotating, which is expected if the star was placed on its orbit through the Hills breakup of a tidally locked and tight binary. We test this hypothesis with hydrodynamical simulations of high-mass ($\geqslant 1 M_{\odot}$) main sequence stars repeatedly partially disrupted by a $10^6 M_{\odot}$ BLACK HOLE, and demonstrate that successively dimmer outbursts are indeed recovered for high (tens of percent breakup) and prograde (i.e., aligned with the orbital angular momentum) stellar spins. Our results provide strong indirect evidence for the operation of the Hills mechanism in seeding the stars in rpTDEs.
[abstract 9 / 11] (score: 2) - Title: A New Record Census of Dwarf AGN and a Bimodal $M_{\rm BH}$-$M_{\star}$ Scaling Relation with DESI DR1Authors: Ragadeepika Pucha, S. Juneau, M. Mezcua, Arjun Dey, Y. -Y. Mao, D. M. Alexander, C. Circosta, V. A. Fawcett, Wei-Jian Guo, J. Moustakas, S. Panda, M. Siudek, Z. Yu, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, K. S. Dawson, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, Satya Gontcho A Gontcho, G. Gutierrez, C. Hahn, K. Honscheid, R. Joyce, R. Kehoe, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, S. Nadathur, W. J. Percival, F. Prada, I. Pérez-Ràfols, G. Rossi, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou,Comments: 32 pages, 15 figures, Submitted to AAS JournalsSubjects: astro-ph.GACreated: 2026-06-01; Updated: 2026-06-03; Datestamp: 2026-06-03
Using the first spectroscopic data release from the Dark Energy Spectroscopic Instrument (DESI DR1), we search for AGN signatures in 1,678,787 low-redshift ($0.001 \le z \le 0.45$) line-emitting galaxies. Based on the [NII]-BPT emission-line ratio diagnostic, we identify AGN in 314,245/1,211,573 (25.9%) high-mass ($\log (M_{\star}/M_{\odot}) > 9.5$) and 9648/467,214 (2.1%) dwarf ($\log (M_{\star}/M_{\odot}) \le 9.5$) galaxies. Among these AGN, 17,949 are broad-line candidates (BL-AGN) with broad H$α$ emission, enabling BLACK HOLE (BH) mass estimates using single-epoch virial methods. We find that the AGN fraction in line-emitting galaxies increases monotonically with stellar mass, rising from $\sim$1.4% at the low-mass end to $\sim$93.3% at the high-mass end. Using the large BL-AGN sample, we extend the $M_{\rm BH} - M_{\star}$ scaling relation down to $\log (M_{\star}/M_{\odot}) \approx 7.8$ and $\log (M_{\rm BH}/M_{\odot}) \approx 4.4$. In the context of high-redshift overmassive BHs, our results suggest that galaxies and their central BHs may follow two distinct evolutionary pathways across cosmic time. With this paper, we release the EmFit value-added catalog, containing emission-line flux and width measurements for $\sim$7.4 million galaxies, the largest catalog with emission-line decomposition into narrow, broad, and outflow components to date. This work significantly expands upon the early DESI results and provides a statistical sample for probing the galaxy$-$BH connection in the low-mass galaxy regime.
[abstract 10 / 11] (score: 2) - Title: Accretion of Primordial Black Holes in Stellar InteriorsAuthors: Matteo Cantiello, Ore Gottlieb, Cameron Norton, Matthew Kleban, Ken Van Tilburg,Comments: 21 pages, 11 figures. Submitted to ApJSubjects: astro-ph.HE astro-ph.SRCreated: 2026-06-01; Updated: 2026-06-03; Datestamp: 2026-06-03
We study spherical accretion onto primordial BLACK HOLEs (PBHs) embedded in the core of a solar-type star. We compute the radiative efficiency self-consistently for the first time across the optically thin range ($10^{-16.5}$-$10^{-10}M_\odot$) with time-dependent simulations, and follow the growth up to $10^{-2}M_\odot$ using an analytical photon-trapping prescription above $5\times 10^{-13}M_\odot$. Near the Schwarzschild radius ($r_{\rm S}\sim 10^{-11}$cm for a $10^{-16}M_\odot$ PBH), gas compressed to $T\sim 10^{11}$K radiates through microphysical processes that fundamentally alter the classical adiabatic Bondi solution. We solve the time-dependent spherical Euler equations with an implicit cooling source term, determining $\dot M$, $η= L/\dot M c^2$, and the flow structure self-consistently. We identify three regimes for spherical accretion: a Hot Bondi regime ($M_{\rm BH}\lesssim 10^{-14}M_\odot$) in which bremsstrahlung cooling is dynamically negligible; a bremsstrahlung-cooling regime ($10^{-14}$-$5\times 10^{-13}M_\odot$) driving the flow toward isothermal with $η\approx 10^{-2}$; and a photon-trapping regime above $5\times 10^{-13}M_\odot$, in which the Bondi sphere is optically thick and the accretion rate remains close to the Bondi value. Cooling enhances $\dot M$ by a factor of $\sim$2-7, keeping growth super-exponential throughout the spherical regime. The radiative efficiency is an order of magnitude lower than previously assumed, and the critical initial PBH mass required to consume a solar-mass star within a Hubble time is $M_{\rm 0,crit}\sim 10^{-16}M_\odot$.
[abstract 11 / 11] (score: 2) - Title: Experimental Tests of Radio-Frequency Heating Saturation in Ultracold Neutral PlasmasAuthors: Bridget O'Mara, Ryan C. Baker, Jacob L. Roberts,Comments:Subjects: physics.plasm-phCreated: 2026-06-01; Updated: 2026-06-03; Datestamp: 2026-06-03
For non-resonant radio-frequency (RF) fields, electron heating in sufficiently collisional plasmas can be driven primarily by inverse bremsstrahlung absorption. When the quiver velocity v_osc approaches the electron thermal velocity v_th, theory often predicts sublinear scaling of the heating rate with RF power, indicating saturation. We experimentally test this prediction in ultracold neutral plasmas by finding RF pulses of different amplitude and duration that produce the same electron heating. Despite v_osc being comparable to v_th, we measured no observable saturation. We compare our results to linear response theory (LRT) and a binary collision theory (BCT). The predicted saturation in both theories is sensitive to how common assumptions about cutoff parameters are applied, and agreement with experimental results is much better if quiver-velocity-dependent cutoffs in LRT and BCT are used. Additionally, under our conditions of moderate coupling and MAGNETization, we find no evidence that RF heating distorts the electron velocity distribution from Maxwell-Boltzmann, indicating saturation from the Langdon effect is suppressed.
arXiv:2606.02700 [pdf, ps, other]
arXiv:2606.02691 [pdf, ps, other]
arXiv:2501.18730 [pdf, ps, other]
arXiv:2606.02748 [pdf, ps, other]
arXiv:2602.04065 [pdf, ps, other]
arXiv:2510.19647 [pdf, ps, other]
arXiv:2606.02654 [pdf, ps, other]
arXiv:2606.02692 [pdf, ps, other]
arXiv:2606.02699 [pdf, ps, other]
arXiv:2606.02726 [pdf, ps, other]
arXiv:2606.02821 [pdf, ps, other]