High Energy Astrophysical Phenomena

New submissions

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New submissions for Fri, 31 May 24

[1]  arXiv:2405.19406 [pdf, other]

Title: Quasars can Signpost Supermassive Black Hole Binaries

Authors: J. Andrew Casey-Clyde, Chiara M. F. Mingarelli, Jenny E. Greene, Andy D. Goulding, Siyuan Chen, Jonathan R. Trump

Comments: 9 pages, 5 figures, 1 appendix

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); Astrophysics of Galaxies (astro-ph.GA)

Supermassive black holes (SMBHs) are found in the centers of massive galaxies, and galaxy mergers should eventually lead to SMBH mergers. Quasar activity has long been associated with galaxy mergers, so here we investigate if supermassive black hole binaries (SMBHBs) are preferentially found in quasars. Our multimessenger investigation folds together a gravitational wave background signal from NANOGrav, a sample of periodic AGN candidates from the Catalina Real-Time Transient Survey, and a quasar mass function, to estimate an upper limit on the fraction of quasars which could host a SMBHB. We find at 95\% confidence that quasars are at most seven times as likely to host a SMBHB as a random galaxy. Quasars should therefore be prioritized as targets for SMBHB searches in pulsar timing arrays.

[2]  arXiv:2405.19434 [pdf, other]

Title: The Pulsar Science Collaboratory: Multi-Epoch Scintillation Studies of Pulsars

Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavso, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin

Comments: Submitted to ApJ

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

We report on findings from scintillation analyses using high-cadence observations of nine canonical pulsars with observing baselines ranging from one to three years. We obtain scintillation bandwidth and timescale measurements for all pulsars in our survey and obtain scintillation arc curvature measurements for four pulsars, detecting multiple arcs for two of them. Using updated pulsar distance estimates, we find evidence of previously undocumented scattering screens along the line of sight (LOS) of PSRs J1645$-$0317 and J2022$+$5154, as well as evidence that one of the arcs along the LOS to PSR J2313$+$4253 may reside somewhere within the Orion-Cygnus arm of the Milky Way. By augmenting the results of previous studies, we find general agreement with estimations of scattering delays from pulsar observations and those predicted by the NE2001 electron density model. In a similar manner, we find additional evidence of a correlation between a pulsar's dispersion measure and the overall variability of its scattering delays over time. The plethora of interesting science obtained through these observations demonstrates the capabilities of the Green Bank Observatory's 20m telescope to contribute to pulsar-based studies of the interstellar medium.

[3]  arXiv:2405.19611 [pdf, other]

Title: Nonthermal Acceleration of Electrons, Positrons and Protons at a Nonrelativistic Quasiparallel Collisionless Shock

Authors: Huan Yu, Qi Xia, Jun Fang

Comments: 7 pages, 7 figures, Accepted for publication in ApJ

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

Energetic positrons have been observed in the interstellar medium, and high-energy positrons with relativistic energies up to approximately 1 TeV have been detected in Galactic cosmic rays. We conducted a study on the acceleration of particles, specifically positrons, in a nonrelativistic quasiparallel collisionless shock induced by a plasma consisting of protons, electrons, and positrons. The positron-to-proton number density ratio in the plasma is 0.1. We focused on a representative shock with a sonic Mach number of 17.1 and an Alfv\'{e}nic Mach number of 16.8 in the rest frame of the shock. To investigate the acceleration mechanisms of particles including positrons in the shock, we utilized one-dimensional particle-in-cell (PIC) simulations. It was found that all three species of particles in the shock can be accelerated and exhibit power law spectra. At the shock front, a significant portion of incoming upstream particles are reflected and undergo significant energy increase, and these reflected particles can be efficiently injected into the process of diffusive shock acceleration (DSA). Moveover, the reflected positrons can be further accelerated by an electric field parallel to the magnetic field when they move along the magnetic field upstream of the shock. As a result, positrons can be preferentially accelerated to be injected in the DSA process compared to electrons.

[4]  arXiv:2405.19827 [pdf, other]

Title: The variable radio jet of the accreting neutron star the Rapid Burster

Authors: J. van den Eijnden, D. Robins, R. Sharma, C. Sánchez-Fernández, T. D. Russell, N. Degenaar, J. C. A. Miller-Jones, T. Maccarone

Comments: Submitted to MNRAS. 15 pages, 8 figures, 2 tables. Reproduction package to be made public upon acceptance

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

The Rapid Burster is a unique neutron star low-mass X-ray binary system, showing both thermonuclear Type-I and accretion-driven Type-II X-ray bursts. Recent studies have demonstrated how coordinated observations of X-ray and radio variability can constrain jet properties of accreting neutron stars - particularly when the X-ray variability is dominated by discrete changes. We present a simultaneous VLA, Swift, and INTEGRAL observing campaign of the Rapid Burster to investigate whether its jet responds to Type-II bursts. We observe the radio counterpart of the X-ray binary at its faintest-detected radio luminosity, while the X-ray observations reveal prolific, fast X-ray bursting. A time-resolved analysis reveals that the radio counterpart varies significantly between observing scans, displaying a fractional variability of $38 \pm 5$%. The radio faintness of the system prevents the robust identification of a causal relation between individual Type-II bursts and the evolution of the radio jet. However, based on a comparison of its low radio luminosity with archival Rapid Burster observations and other accreting neutron stars, and on a qualitative assessment of the X-ray and radio light curves, we explore the presence of a tentative connection between bursts and jet: i.e., the Type-II bursts may weaken or strengthen the jet. The former of those two scenarios would fit with magneto-rotational jet models; we discuss three lines of future research to establish this potential relation between Type-II bursts and jets more confidently.

[5]  arXiv:2405.20009 [pdf, ps, other]

Title: Primary and secondary source of energy in the superluminous supernova 2018ibb

Authors: Alexandra Kozyreva, Luke Shingles, Petr Baklanov, Alexey Mironov, Fabian R. N. Schneider

Comments: 7 pages, 4 figures, accepted for publication in A & A

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); Solar and Stellar Astrophysics (astro-ph.SR)

We examine the pair-instability origin of superluminous supernova 2018ibb. As the base model, we use a non-rotating stellar model with an initial mass of 250 Msun at about 1/15 solar metallicity. We consider three versions of the model as input for radiative transfer simulations done with the STELLA and ARTIS codes: with 25 Msun of 56Ni, 34 Msun of 56Ni, and a chemically mixed case with 34 Msun of 56Ni. We present light curves and spectra in comparison to the observed data of SN 2018ibb, and conclude that the pair-instability supernova model with 34 Msun of 56Ni explains broad-band light curves reasonably well between -100 and 250 days around the peak. Our synthetic spectra have many similarities with the observed spectra. The luminosity excess in the light curves and the blue-flux excess in the spectra can be explained by an additional energy source, which may be interaction of the SN ejecta with circumstellar matter. We discuss possible mechanisms of the origin of the circumstellar matter being ejected in the decades before the pair-instability explosion.

[6]  arXiv:2405.20146 [pdf, other]

Title: Supermassive black holes and very high-energy neutrinos: the case of NGC 1068

Authors: P. Padovani, E. Resconi, M. Ajello, C. Bellenghi, S. Bianchi, P. Blasi, K.-Y. Huang, S. Gabici, V. Gámez Rosas, H. Niederhausen, E. Peretti, B. Eichmann, D. Guetta, A. Lamastra, T. Shimizu

Comments: 18 pages, 4 figures, review paper accepted for publication in Nature Astronomy; authors' version before editorial review

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); Astrophysics of Galaxies (astro-ph.GA)

We present a comprehensive multi-messenger study of NGC 1068, the prototype Seyfert II galaxy recently associated with high-energy IceCube neutrinos. Various aspects of the source, including its nuclear activity, jet, outflow, and starburst region, are analyzed in detail using a multi-wavelength approach and relevant luminosities are derived. We then explore its gamma-ray and neutrino emissions and investigate potential mechanisms underlying these phenomena and their relations with the different astrophysical components to try to understand which one is responsible for the IceCube neutrinos. By first using simple order-of-magnitude arguments and then applying specific theoretical models, we infer that only the region close to the accretion disc around the supermassive black hole has both the right density of X-ray photons needed to provide the targets for protons to sustain neutrino production and of optical/infrared photons required to absorb the associated but unobserved gamma rays. We conclude by highlighting ongoing efforts to constrain a possible broad connection between neutrinos and active galactic nuclei, as well as future synergies between astronomical and neutrino facilities.

[7]  arXiv:2405.20329 [pdf, other]

Title: Did Binary Neutron Star Merger GW170817 Leave Behind A Long-lived Neutron Star?

Authors: Marcus DuPont, Andrew MacFadyen

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

We consider the observational implications of the binary neutron star (BNS) merger GW170817 leaving behind a rapidly rotating massive neutron star that launches a relativistic, equatorial outflow as well as a jet. We show that if the equatorial outflow (ring) is highly beamed in the equatorial plane, its luminosity can be "hidden" from view until late times, even if carrying a significant fraction of the spin-down energy of the merger remnant. This hidden ring reveals itself as a re-brightening in the light curve once it slows down enough for Earth to be within the ring's relativistic beaming solid angle. We compute semi-analytic light curves using this model and find they are in agreement with the observations thus far, and we provide predictions for the ensuing afterglow.

Cross-lists for Fri, 31 May 24

[8]  arXiv:2405.17721 (cross-list from gr-qc) [pdf, other]

Title: Rapid detection of gravitational waves from binary black hole mergers using sparse dictionary learning

Authors: Charles Badger, Rahul Srinivasan, Alejandro Torres-Forné, Marie Anne Bizouard, José A. Font, Mairi Sakellariadou, Astrid Lamberts

Subjects: General Relativity and Quantum Cosmology (gr-qc); High Energy Astrophysical Phenomena (astro-ph.HE)

Current gravitational wave (GW) detection pipelines for compact binary coalescence based on matched-filtering have reported over 90 confident detections during the first three observing runs of the LIGO-Virgo-KAGRA (LVK) detector network. Decreasing the latency of detection, in particular for future detectors anticipated to have high detection rates, remains an ongoing effort. In this paper, we develop and test a sparse dictionary learning (SDL) algorithm for the rapid detection of GWs. We evaluate the algorithms biases and estimate its GW detection rate for an astrophysical population of binary black holes. The SDL algorithm is assessed using both, simulated data injected into the proposed A+ detector sensitivity and real data containing confident detections from the third LVK observing run. We find that our SDL algorithm can reconstruct a single binary black hole signal in less than 1 s. This suggests that SDL could be regarded as a promising approach for rapid, efficient GW detection in future observing runs of ground-based detectors.

[9]  arXiv:2405.19381 (cross-list from astro-ph.IM) [pdf, other]

Title: Motivating Emissions from Positive Energy Warp Bubbles

Authors: Erik W. Lentz, Ryan C. Felton

Comments: 12 pages, 8 figures

Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM); High Energy Astrophysical Phenomena (astro-ph.HE); General Relativity and Quantum Cosmology (gr-qc)

Recent research has proposed that advanced propulsion mechanisms such as warp drives are more physically feasible than previously thought, using positive energy sources potentially sourced by known classical physics. Motivated by this, we hypothesize that an advanced inter-planetary or interstellar civilization using warp drives at sub-luminal or super-luminal speeds will broadcast detectable emissions of their travels. These technosignatures would be of significant astronomical, physical, and technological interest. This paper seeks to motivate signatures from warp drive emissions due to intrinsic and extrinsic processes across several messenger types (electromagnetic, particle, and gravitational) and propose a research program to simulate such emissions in sufficient detail to search for their signatures through coordinated analyses across multiple observatories.

[10]  arXiv:2405.19393 (cross-list from hep-ph) [pdf, other]

Title: Supernova axions convert to gamma-rays in magnetic fields of progenitor stars

Authors: Claudio Andrea Manzari, Yujin Park, Benjamin R. Safdi, Inbar Savoray

Comments: 10+18 pages, 3+20 figures, video abstract at this https URL

Subjects: High Energy Physics - Phenomenology (hep-ph); High Energy Astrophysical Phenomena (astro-ph.HE); Solar and Stellar Astrophysics (astro-ph.SR)

It has long been established that axions could have been produced through the Primakoff process within the nascent proto-neutron-star formed following the type II supernova SN1987A, escaped the star due to their weak interactions, and then converted to gamma-rays in the Galactic magnetic fields; the non-observation of a gamma-ray flash coincident with the neutrino burst leads to strong constraints on the axion-photon coupling for axion masses $m_a \lesssim 10^{-10}$ eV. In this work we use SN1987A to constrain, for the first time, higher mass axions, all the way to $m_a \sim 10^{-3}$ eV, by accounting for axion-photon conversion on the still-intact magnetic fields of the progenitor star. Moreover, we show that gamma-ray observations of the next Galactic supernova, leveraging the magnetic fields of the progenitor star, could detect quantum chromodynamics axions for masses above roughly $50$ $\mu$eV, depending on the supernova. We propose a new full-sky gamma-ray satellite constellation that we call the GALactic AXion Instrument for Supernova (GALAXIS) to search for such future signals along with related signals from extragalactic neutron star mergers.

[11]  arXiv:2405.19417 (cross-list from astro-ph.SR) [pdf, other]

Title: Almost All Carbon/Oxygen White Dwarfs Can Support Double Detonations

Authors: Ken J. Shen, Samuel J. Boos, Dean M. Townsley

Comments: Submitted

Subjects: Solar and Stellar Astrophysics (astro-ph.SR); High Energy Astrophysical Phenomena (astro-ph.HE)

Double detonations of sub-Chandrasekhar-mass white dwarfs (WDs) in unstably mass-transferring double WD binaries have become a leading contender to explain most, if not all, Type Ia supernovae. However, past theoretical studies of the explosion process have assumed relatively ad hoc initial conditions for the helium shells in which the double detonations begin. In this work, we construct realistic C/O WDs to use as the starting points for multidimensional double detonation simulations. We supplement these with simplified one-dimensional detonation calculations to gain a physical understanding of the conditions under which shell detonations can propagate successfully. We find that C/O WDs <= 1.0 Msol, which make up the majority of C/O WDs, are born with structures that can support double detonations. More massive C/O WDs require ~1e-3 Msol of accretion before detonations can successfully propagate in their shells, but such accretion may be common in the double WD binaries that host massive WDs. Our findings strongly suggest that if the direct impact accretion stream reaches high enough temperatures and densities during mass transfer from one WD to another, the accreting WD will undergo a double detonation. Furthermore, if the companion is also a C/O WD <= 1.0 Msol, it will undergo its own double detonation when impacted by the ejecta from the first explosion. Exceptions to this outcome may explain the newly discovered class of hypervelocity supernova survivors.

[12]  arXiv:2405.19530 (cross-list from hep-ph) [pdf, other]

Title: Causal fermion states in magnetic field in relativistic rotating frame and electromagnetic radiation by rapidly rotating charge

Authors: Matteo Buzzegoli, Kirill Tuchin

Comments: 38 pages, 16 figures

Subjects: High Energy Physics - Phenomenology (hep-ph); High Energy Astrophysical Phenomena (astro-ph.HE); Nuclear Theory (nucl-th)

We consider the Dirac field uniformly rotating with angular velocity $\Omega$ and also subject to the constant magnetic field $B$ directed along the rotation axis. The causal states are constrained to the interior of the light cylinder of radius $c/\Omega$. When this radius is smaller than the system size, as in the quark-gluon plasma, the effect of the boundary on the fermion spectrum is critical. We derive the fermion spectrum and study its properties. We compute the intensity of the electromagnetic radiation emitted due to transitions between the fermion states. We study its dependence on energy and angular momentum for different values of the angular velocity and the magnetic field. Rotation has enormous impact on the electromagnetic radiation by the quark-gluon plasma with or without the magnetic field.

[13]  arXiv:2405.19733 (cross-list from nucl-th) [pdf, other]

Title: Unraveling the global behavior of equation of state by explicit finite nuclei constraints

Authors: Anagh Venneti, Sakshi Gautam, Sarmistha Banik, B. K. Agrawal

Comments: The manuscript has been accepted by Physics Letters B on May 24th 2024

Subjects: Nuclear Theory (nucl-th); High Energy Astrophysical Phenomena (astro-ph.HE)

We obtain posterior distribution of equations of state (EOSs) across a broad range of density by imposing explicitly the constraints from precisely measured fundamental properties of finite nuclei, in combination with the experimental data from heavy-ion collisions and the astrophysical observations of radius, tidal deformability and minimum-maximum mass of neutron stars. The acquired EOSs exhibit a distinct global behavior compared to those usually obtained by imposing the finite nuclei constraints implicitly through empirical values of selected key parameters describing symmetric nuclear matter and symmetry energy in the vicinity of the saturation density. The explicit treatment of finite nuclei constraints yields softer EOSs at low densities which eventually become stiffer to meet the maximum mass criteria. The Kullback-Leibler divergence has been used to perform a quantitative comparison of the distributions of neutron star properties resulting from the EOSs obtained from implicit and explicit finite nuclei constraints.

[14]  arXiv:2405.19750 (cross-list from astro-ph.GA) [pdf, other]

Title: Sloshing and spiral structures breeding a putative radio mini-halo in the environment of a cool-core cluster Abell 795

Authors: S. K. Kadam, Sameer Salunkhe, N. D. Vagshette, Surajit Paul, Satish S. Sonkamble, P. K. Pawar, M. K. Patil

Comments: 11 pages, 9 figures, Accepted for publication in MNRAS

Subjects: Astrophysics of Galaxies (astro-ph.GA); High Energy Astrophysical Phenomena (astro-ph.HE)

Spiral structures and cold fronts in X-rays are frequently observed in cool core galaxy clusters. However, studies on radio mini-haloes associated with such spirals and their physical connections are rare. Here, we present the detection of an extended diffuse radio emission entrained in the X-ray spiral structure in a known cool core cluster Abell 795 (A795). Though the cool core is a sign of the relaxed nature of the clusters, our re-analysed 30 ks Chandra X-ray data of cluster A795 confirms the presence of an interesting log spiral structure of X-ray deficit region complemented by an X-ray excess counter spiral in the residual map, exposing its dynamical activity. Our new analysis of 150 $\&$ 325 MHz GMRT archival data of the cluster confirms the detection of a $\sim180$ kpc ultra-steep ($\alpha\sim-2.7$) diffuse radio structure which was previously reported as a candidate radio mini halo from low sensitive survey maps. This radio emission spans the entire spiral structure ($\sim186$ kpc), enclosed by two previously reported cold fronts. Furthermore, SDSS DR13 optical spectra, as well as GALEX's FUV data, show a considerably low total star formation rate of 2.52 M$_{\odot}$ yr$^{-1}$ and having no significant variation in metallicity distribution. We argued that the two-phase (hot and cold) plasma at the cluster core with differential velocity has probably caused the spiral formation and has redistributed the secondary electrons from the central BCG or the pre-accelerated electrons which have been (re-)accelerated by the sloshing turbulence to form the observed candidate radio mini-halo structure. This has been supported by a few previous studies that indicate spiral formation and sloshing turbulence may quench star formation and facilitate smooth metallicity distribution by mixing the gas in the core.

[15]  arXiv:2405.20228 (cross-list from gr-qc) [pdf, other]

Title: Love-C relations for elastic hybrid stars

Authors: Zoey Zhiyuan Dong, Joshua Cole Faggert, Shu Yan Lau, Kent Yagi

Comments: 23 pages, 9 fighures, submitted to GRG

Subjects: General Relativity and Quantum Cosmology (gr-qc); High Energy Astrophysical Phenomena (astro-ph.HE); Nuclear Theory (nucl-th)

Neutron stars (NSs) provide a unique laboratory to study matter under extreme densities. Recent observations from gravitational and electromagnetic waves have enabled constraints on NS properties, such as tidal deformability (related to the tidal Love number) and stellar compactness. Although each of these two NS observables depends strongly on the stellar internal structure, the relation between them (called the Love-C relation) is known to be equation-of-state insensitive. In this study, we investigate the effects of a possible crystalline phase in the core of hybrid stars (HSs) on the mass-radius and Love-C relations, where HSs are a subclass of NS models with a quark matter core and a nuclear matter envelope with a sharp phase transition in between. We find that both the maximum mass and the corresponding radius increase as one increases the stiffness of the quark matter core controlled by the speed of sound, while the density discontinuity at the nuclear-quark matter transition effectively softens the equations of state. Deviations of the Love-C relation for elastic HSs from that of fluid NSs become more pronounced with a larger shear modulus, lower transition pressure, and larger density gap and can be as large as 60%. These findings suggest a potential method for testing the existence of distinct phases within HSs, though deviations are not large enough to be detected with current measurements of the tidal deformability and compactness.

Replacements for Fri, 31 May 24

[16]  arXiv:2309.03949 (replaced) [pdf, other]

Title: GRMHD simulations of accretion flows onto massive binary black hole mergers embedded in a thin slab of gas

Authors: Giacomo Fedrigo, Federico Cattorini, Bruno Giacomazzo, Monica Colpi

Comments: 16 pages, 8 figures, published in Phys. Rev. D

Journal-ref: Phys. Rev. D 109, 103024 - Published 15 May 2024

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); General Relativity and Quantum Cosmology (gr-qc)

[17]  arXiv:2401.05534 (replaced) [pdf, other]

Title: A closer look at the electromagnetic signatures of Bethe-Heitler pair production process in blazars

Authors: Despina Karavola, Maria Petropoulou

Comments: Accepted for publication on JCAP. Empirical function for the Bethe-Heitler injection spectrum can be found in this https URL

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

[18]  arXiv:2401.17289 (replaced) [pdf, other]

Title: A new understanding of the Gemini-Monoceros X-ray enhancement from discoveries with eROSITA

Authors: Jonathan R. Knies, Manami Sasaki, Werner Becker, Teng Liu, Gabriele Ponti, Paul P. Plucinsky

Comments: Accepted by A&A - 02/04/2024

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

[19]  arXiv:2402.15149 (replaced) [pdf, other]

Title: Possible spectral irregularities in the AMS-02 positron spectrum

Authors: Xing-Jian Lv, Xiao-Jun Bi, Kun Fang, Peng-Fei Yin, Meng-Jie Zhao

Comments: 6 pages, 6 figures

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); High Energy Physics - Phenomenology (hep-ph)

[20]  arXiv:2306.01682 (replaced) [pdf, other]

Title: Impacts of the $^{12}\rm{C}\left(α,γ\right)^{16}\!\rm{O}$ reaction rate on $^{56}{\rm Ni}$ nucleosynthesis in pair-instability supernovae

Authors: Hiroki Kawashimo, Ryo Sawada, Yudai Suwa, Takashi J. Moriya, Ataru Tanikawa, Nozomu Tominaga

Comments: 17 pages, 12 figures

Subjects: Solar and Stellar Astrophysics (astro-ph.SR); High Energy Astrophysical Phenomena (astro-ph.HE); Nuclear Theory (nucl-th)

[21]  arXiv:2307.09509 (replaced) [pdf, other]

Title: Shedding light on the $Δm^2_{21}$ tension with supernova neutrinos

Authors: Rasmi Hajjar, Sergio Palomares-Ruiz, Olga Mena

Comments: 10 pages, 4 figures. It matches the version accepted for publication

Journal-ref: Phys.Lett.B 854 (2024) 138719

Subjects: High Energy Physics - Phenomenology (hep-ph); High Energy Astrophysical Phenomena (astro-ph.HE)

[22]  arXiv:2311.01528 (replaced) [pdf, other]

Title: Halo Densities and Pericenter Distances of the Bright Milky Way Satellites as a Test of Dark Matter Physics

Authors: Kevin E. Andrade, Manoj Kaplinghat, Mauro Valli

Comments: Submitted to MNRAS. 32 pages, 27 figures

Subjects: Astrophysics of Galaxies (astro-ph.GA); Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Astrophysical Phenomena (astro-ph.HE); High Energy Physics - Phenomenology (hep-ph)

[23]  arXiv:2311.01819 (replaced) [pdf, other]

Title: Effects of stimulated emission and superradiant growth of non-spherical axion cluster

Authors: Liang Chen, Da Huang, Chao-Qiang Geng

Comments: 27 pages, 10 figures, 1 table; to appear in JCAP

Subjects: High Energy Physics - Phenomenology (hep-ph); High Energy Astrophysical Phenomena (astro-ph.HE)

[24]  arXiv:2403.00051 (replaced) [pdf, other]

Title: Sudden breakdown of effective field theory near cool Kerr-Newman black holes

Authors: Gary T. Horowitz, Maciej Kolanowski, Grant N. Remmen, Jorge E. Santos

Comments: 54 pages, 8 figures

Journal-ref: JHEP 2405:122,2024

Subjects: High Energy Physics - Theory (hep-th); High Energy Astrophysical Phenomena (astro-ph.HE); General Relativity and Quantum Cosmology (gr-qc); High Energy Physics - Phenomenology (hep-ph)

[25]  arXiv:2403.02721 (replaced) [pdf, other]

Title: Light Thermal Dark Matter Beyond $p$-Wave Annihilation in Minimal Higgs Portal Model

Authors: Yu-Tong Chen, Shigeki Matsumoto, Tian-Peng Tang, Yue-Lin Sming Tsai, Lei Wu

Comments: 35 pages, 4 figures

Subjects: High Energy Physics - Phenomenology (hep-ph); High Energy Astrophysical Phenomena (astro-ph.HE)

[26]  arXiv:2403.19604 (replaced) [pdf, other]

Title: More on Black Holes Perceiving the Dark Dimension

Authors: Luis A. Anchordoqui, Ignatios Antoniadis, Dieter Lust

Comments: Matching version to be published in PRD

Subjects: High Energy Physics - Theory (hep-th); High Energy Astrophysical Phenomena (astro-ph.HE); High Energy Physics - Phenomenology (hep-ph)

[27]  arXiv:2404.08780 (replaced) [pdf, other]

Title: The Population of Massive Stars in AGN Disks

Authors: Yi-Xian Chen, Douglas N. C. Lin

Comments: Published in ApJ

Subjects: Astrophysics of Galaxies (astro-ph.GA); High Energy Astrophysical Phenomena (astro-ph.HE); Solar and Stellar Astrophysics (astro-ph.SR)

[28]  arXiv:2405.17772 (replaced) [pdf, other]

Title: A Contact Binary Mis-Classified as an Ellipsoidal Variable: Complications for Detached Black Hole Searches

Authors: Tyrone N. O'Doherty, Arash Bahramian, Adelle J. Goodwin, James C. A. Miller-Jones, Jerome A. Orosz, Jay Strader

Comments: Accepted for publication in AJ. 16 pages, 8 figures, 2 tables. Updated description of ASAS-SN ellipsoidal search in Section 2.2

Subjects: Solar and Stellar Astrophysics (astro-ph.SR); Astrophysics of Galaxies (astro-ph.GA); High Energy Astrophysical Phenomena (astro-ph.HE)

• New submissions
• Cross-lists
• Replacements