Current date: 2025-11-11
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Datestamp limit: 2025-11-11 (0 days ago)
Created/updated limit: 2025-11-04 (7 days ago)
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Scoring abstracts
Number of records retrieved: 1005
Keyword score statistics
score 11 -- 1 abstracts
score 9 -- 3 abstracts
score 8 -- 2 abstracts
score 7 -- 1 abstracts
score 6 -- 2 abstracts
score 5 -- 1 abstracts
score 4 -- 9 abstracts
score 3 -- 13 abstracts
score 2 -- 21 abstracts
in total -- 53 abstracts
Articles that appeared on 2025-11-11
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[abstract 1 / 53] Wow! (score: 11)
- Title: Hadronic Processes in Advection-Dominated Accretion Flow as the Origin of TeV Excesses in BL Lac ObjectsAuthors: Ji-Shun Lian, Ze-Rui Wang, Jin Zhang,Comments: 13 pages, 2 Figures, 1 Table. Accepted for publication in ApJSubjects: astro-ph.HE astro-ph.GACreated: 2025-11-08; Updated: 2025-11-11; Datestamp: 2025-11-11
The spectral energy distributions (SEDs) of certain BL Lac objects (BL Lacs) exhibit an additional hard $γ$-ray component in the TeV energy range that surpasses the predictions of the one-zone leptonic JET model. The origin of this excess emission remains unclear. In this study, we selected five BL Lacs whose SEDs display a very hard intrinsic spectrum in the TeV band and successfully reproduced their broadband SEDs using a two-zone lepto-hadronic model. Within this framework, the emission observed in the optical, X-ray, GeV $γ$-ray, and sub-TeV $γ$-ray bands is modeled using the SYNCHROTRON and SYNCHROTRON self-Compton radiation processes of the RELATIVISTIC electrons in the JETs. Meanwhile, the TeV excess is attributed to $γ$-ray emission resulting from the photomeson ($pγ$) process via $π^0$ decay occurring within advection-dominated accretion flows (ADAFs). This scenario requires a hard proton spectrum with a spectral index of $p \sim 1.6-1.7$ and a cutoff energy ranging from 30 to 90 TeV, as well as a relatively large ADAF radius. Such hard proton spectra suggest that the dominant acceleration mechanisms are likely MAGNETic RECONNECTion and/or stochastic acceleration processes within ADAFs. Additionally, the emission from the cascaded electrons results in a bump in the keV--MeV band; however, it is overwhelmed by the JET emission. Although the hadronuclear ($pp$) process cannot be entirely ruled out, it would necessitate an even harder proton spectrum and a higher cutoff energy compared to the $pγ$ process, making it a less favorable explanation for the observed TeV excess.
[abstract 2 / 53] Wow! (score: 9) - Title: Probing Jet Compositions with Extreme Mass Ratio Binary Black HolesAuthors: Hung-Yi Pu,Comments: 23 pages, 7 figures. Accepted by published by UniverseSubjects: astro-ph.HECreated: 2025-11-07; Updated: 2025-11-11; Datestamp: 2025-11-11
Determining whether BLACK HOLE JETs are dominated by leptonic or baryonic matter remains an open question in high-energy astrophysics. We propose that extreme mass ratio binary (EMRB) BLACK HOLEs, where an intermediate mass secondary BLACK HOLE (a "miniQUASAR") periodically interacts with the accretion flow of a supermassive BLACK HOLE (SMBH), offer a natural laboratory to probe JET composition. In an EMRB, the miniQUASAR JET is launched episodically after each disk-crossing event, triggered by the onset of super-Eddington accretion. The resulting emissions exhibit temporal evolution as the JET interacts with the SMBH accretion disk. Depending on whether the JET is leptonic or hadronic in composition, the radiative signatures differ substantially. Notably, a baryonic JET produces a more pronounced gamma-ray output than a purely leptonic JET. By modeling the evolution of the multifrequency characteristic features, it is suggested that the gamma-ray-to-UV emissions may serve as a diagnostic tool capable of distinguishing between leptonic and baryonic scenarios. The resulting electroMAGNETic signals, when combined with multi-messenger observations, offer a powerful means to constrain the physical nature of RELATIVISTIC JETs from BLACK HOLEs.
[abstract 3 / 53] Wow! (score: 9) - Title: A New Phase of Optical Activity of BL Lacertae in the Fall of 2024: Intra-Night Flux and Polarization VariationsAuthors: Rumen Bachev, Milen Minev, Anton Strigachev, Alexander Kurtenkov,Comments: To be published in UniverseSubjects: astro-ph.HE astro-ph.GACreated: 2025-11-08; Updated: 2025-11-11; Datestamp: 2025-11-11
BL Lacertae is not only archetypical of an entire class of JET-dominated ACTIVE GALACTIC NUCLEi, BLAZARs, but also one of the most active and rapidly changing objects in this class. In the fall of 2024 (September--November), BL Lacertae underwent another episode of strong optical activity, reaching an R-band magnitude of about 12 and showing extremely rapid and large-amplitude inter- and intra-night flux and POLARIZATION variations. During this period, the object was monitored over 40 nights using telescopes with an aperture of up to 2 m at three observatories: Rozhen and Belogradchik in Bulgaria and Skinakas in Greece. The results from this study include some of the most spectacular intra-night variability episodes detected in a BLAZAR. These rapid variations, combined with high photometric accuracy and high time resolution, allowed for confirmation of consistency between different optical bands with zero time delays, down to a minute scale. Unlike previous activity reports, POLARIZATION was relatively stable on these short time-scales. Possible connections between POLARIZATION, flux, and intra-night variability were explored in order to better model or constrain the physical processes and emission mechanisms in the RELATIVISTIC JETs.
[abstract 4 / 53] Wow! (score: 9) - Title: Probing a cosmogenic origin of astrophysical neutrinos and COSMIC RAYs using gamma-ray observations of TXS 0506+056Authors: A. Acharyya, A. Archer, P. Bangale, J. T. Bartkoske, W. Benbow, J. H. Buckley, Y. Chen, J. L. Christiansen, A. Duerr, M. Errando, M. Escobar Godoy, A. Falcone, S. Feldman, Q. Feng, S. Filbert, L. Fortson, A. Furniss, W. Hanlon, O. Hervet, C. E. Hinrichs, J. Holder, Z. Hughes, M. Iskakova, W. Jin, P. Kaaret, M. Kertzman, M. Kherlakian, D. Kieda, T. K. Kleiner, N. Korzoun, M. J. Lang, M. Lundy, G. Maier, C. L. Mooney, R. Mukherjee, W. Ning, R. A. Ong, A. Pandey, M. Pohl, E. Pueschel, J. Quinn, P. L. Rabinowitz, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, I. Sadeh, A. C. Sadun, L. Saha, G. H. Sembroski, R. Shang, M. Splettstoesser, D. Tak, A. K. Talluri, J. V. Tucci, J. Valverde, D. A. Williams, S. L. Wong, T. Yoshikoshi, M. Meyer, J. Müller,Comments: 14 pages, 5 figures, Accepted for publication in the Astrophysical Journal (ApJ)Subjects: astro-ph.HECreated: 2025-11-08; Updated: 2025-11-11; Datestamp: 2025-11-11
In September 2017, a high-energy neutrino event detected by the IceCube Neutrino Observatory (IceCube-170922A) was associated, at the $3σ$ level, with a gamma-ray flare from the BLAZAR TXS 0506+056. Cosmic rays that are accelerated in astrophysical sources can escape from their JETs and interact with background radiation fields. Interactions with the extragalactic background light can produce pions and hence neutrinos, while interactions with the cosmic microwave background predominantly drive inverse Compton scattering, contributing to electroMAGNETic cascades in intergalactic space. The resulting secondary gamma-ray emission can be detected with high-energy gamma-ray telescopes. Here, we report on a new search for such cosmogenic cascade emission from the BLAZAR TXS 0506+056, using a combined data set from the FERMI-Large Area Telescope and VERITAS. We compare the gamma-ray spectrum and neutrino observations with the predictions of cosmic-ray induced cascades in intergalactic space. The observed gamma-ray spectrum is modeled as a combination of the primary spectrum and the cascade spectrum. We apply a Monte Carlo simulation with a $Δχ^2$-based likelihood analysis to jointly determine the best-fit parameters of a proton emission spectrum describing the data and derive constraints on the proton escape luminosity. Assuming a log-parabola primary photon spectrum, we find consistency with a proton injection spectral index of $α_{p} \simeq 2.0$ and a cutoff energy of $E_{p,\text{max}} \simeq 1.3 \times 10^{16}$ eV, and constrain the isotropic proton escape luminosity to $1 \times 10^{44}$ erg s$^{-1}$ $\lesssim L_{p, esc} \lesssim 3 \times 10^{45}$ erg s$^{-1}$ at the 90 % confidence level.
[abstract 5 / 53] Wow! (score: 8) - Title: Hadronic origin of the very high-energy gamma-ray emission from the low-luminosity AGN in NGC 4278Authors: Asahi Shoji, Yutaka Fujita, Norita Kawanaka, Susumu Inoue, Kosuke Nishiwaki,Comments: 8 pages, 7 figures. This article has been accepted for publication in "Publications of the Astronomical Society of Japan'' published by Oxford University PressSubjects: astro-ph.HE astro-ph.GACreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
The Large High Altitude Air Shower Observatory has detected very high-energy (VHE) gamma rays from NGC 4278, which is known to host a low-luminosity ACTIVE GALACTIC NUCLEus (AGN). Having only very weak radio JETs, the origin of its VHE gamma rays is unclear. In this paper we first show that NGC 4278 has a massive molecular cloud surrounding the nucleus by analyzing data taken with the Atacama Large Millimeter/submillimeter Array. We then assume that COSMIC RAY protons are accelerated in a radiatively inefficient accretion flow around the supermassive BLACK HOLE, which diffuse into the molecular cloud and produce gamma rays and neutrinos via $pp$ interactions. We model the gamma-ray spectra and find that the observations can be explained by such hadronic processes if the AGN activity was higher in the past than at present, and the diffusion coefficient in the molecular cloud is appreciably smaller than in the Milky Way interstellar medium. We also show that although the high-energy neutrinos co-produced with the gamma rays are unlikely to be detectable even with IceCube-Gen2, the accompanying SYNCHROTRON X-ray emission due to pion-decay secondary electrons and positrons may be detectable in the future, providing a valuable test of our hadronic model.
[abstract 6 / 53] Wow! (score: 8) - Title: Hard X-ray view of two $γ$-ray detected low-luminosity ACTIVE GALACTIC NUCLEi: NGC 315 and NGC 4261Authors: Yuwei Yu, Jin Zhang,Comments: 11 pages, 6 figures, 6 tables. Accepted for publication in A&ASubjects: astro-ph.HECreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
Aims. The accretion disk of low-luminosity ACTIVE GALACTIC NUCLEi (LLAGNs) is a radiatively inefficient accretion flow (RIAF). Our goal is to find evidence of RIAF radiation from LLAGNs with JETs and analyze their radiation properties, which also adds samples to future research on LLAGNs. Methods. Weconducted an analysis of the X-ray data obtained from NUSTAR and XMM-Newton observations of NGC 315 and NGC 4261, encompassing both timing and spectral investigations. The joint X-ray spectra of the two LLAGNs were fitted using various functional forms and radiative models in XSPEC. Results. No significant variability on timescales of days is observed for both NGC 315 and NGC 4261. The X-ray continuum emission of NGC 315 is suitable for cutoff power-law (PL) fitting, yielding a cutoff energy of Ecut = 18.45 keV, which is the lowest value found in LLAGNssofar. In contrast, the X-ray continuum of NGC 4261 is composed of two PL components, with no signs of a cutoff energy. A prominent neutral Fe Kα line is observed in NGC 315, while an ionized Fe XXV line is seen in NGC 4261. The derived reflection fractions are R = 0.61 for NGC 315 and R = 0.18 for NGC 4579. Neither NGC 315 nor NGC 4261 shows evidence of a Compton reflection bump. Conclusions. The X-ray spectral characteristics support the RIAF emission as the dominant origin of the X-rays in both sources, although an additional soft PL component originating from the inner JET is observed in NGC 4261. The higher reflection fraction compared to other LLAGNs, along with the detection of a neutral Fe Kα line, suggests the existence of a truncated accretion disk with a relatively small radius in NGC 315. Bremsstrahlung radiation appears to be the dominant cooling mechanism for the plasma in NGC315, while Comptonization within the RIAF is more likely responsible for the X-ray emission in NGC 4261.
[abstract 7 / 53] Wow! (score: 7) - Title: A Comprehensive Hadronic Code Comparison for Active Galactic NucleiAuthors: Matteo Cerruti, Annika Rudolph, Maria Petropoulou, Markus Böttcher, Stamatios I. Stathopoulos, Foteini Oikonomou, Stavros Dimitrakoudis, Anton Dmytriiev, Shan Gao, Susumu Inoue, Apostolos Mastichiadis, Kohta Murase, Anita Reimer, Joshua Robinson, Xavier Rodrigues, Walter Winter, Andreas Zech,Comments: 34 pages; in press in ApJS. Online material available at https://doi.org/10.5281/zenodo.17177642Subjects: astro-ph.HECreated: 2025-11-09; Updated: 2025-11-11; Datestamp: 2025-11-11
We perform the first dedicated comparison of five hadronic codes (AM$^3$, ATHE$ν$A, B13, LeHa-Paris, and LeHaMoC) that have been extensively used in modeling of the spectral energy distribution (SED) of JETted ACTIVE GALACTIC NUCLEi. The purpose of this comparison is to identify the sources of systematic errors (e.g., implementation method of proton-photon interactions) and to quantify the expected dispersion in numerical SED models computed with the five codes. The outputs from the codes are first tested in SYNCHROTRON self-Compton scenarios that are the simplest BLAZAR emission models used in the literature. We then compare the injection rates and spectra of secondary particles produced in pure hadronic cases with monoenergetic and power-law protons interacting on black-body and power-law photon fields. We finally compare the photon SEDs and the neutrino spectra for realistic proton-SYNCHROTRON and leptohadronic BLAZAR models. We find that the codes are in excellent agreement with respect to the spectral shape of the photons and neutrinos. There is a remaining spread in the overall normalization that we quantify, at its maximum, at the level of $\pm 40\%$. This value should be used as an additional, conservative, systematic uncertainty term when comparing numerical simulations and observations.
[abstract 8 / 53] Yes (score: 6) - Title: GW231123: a Binary Black Hole Merger with Total Mass 190-265 $M_{\odot}$Authors: The LIGO Scientific Collaboration, the Virgo Collaboration, the KAGRA Collaboration, A. G. Abac, I. Abouelfettouh, F. Acernese, K. Ackley, C. Adamcewicz, S. Adhicary, D. Adhikari, N. Adhikari, R. X. Adhikari, V. K. Adkins, S. Afroz, A. Agapito, D. Agarwal, M. Agathos, N. Aggarwal, S. Aggarwal, O. D. Aguiar, I. -L. Ahrend, L. Aiello, A. Ain, P. Ajith, T. Akutsu, S. Albanesi, W. Ali, S. Al-Kershi, C. Alléné, A. Allocca, S. Al-Shammari, P. A. Altin, S. Alvarez-Lopez, W. Amar, O. Amarasinghe, A. Amato, F. Amicucci, C. Amra, A. Ananyeva, S. B. Anderson, W. G. Anderson, M. Andia, M. Ando, M. Andrés-Carcasona, T. Andrić, J. Anglin, S. Ansoldi, J. M. Antelis, S. Antier, M. Aoumi, E. Z. Appavuravther, S. Appert, S. K. Apple, K. Arai, C. Araujo Alvarez, A. Araya, M. C. Araya, M. Arca Sedda, J. S. Areeda, N. Aritomi, F. Armato, S. Armstrong, N. Arnaud, M. Arogeti, S. M. Aronson, K. G. Arun, G. Ashton, Y. Aso, L. Asprea, M. Assiduo, S. Assis de Souza Melo, S. M. Aston, P. Astone, F. Attadio, F. Aubin, K. AultONeal, G. Avallone, E. A. Avila, S. Babak, C. Badger, S. Bae, S. Bagnasco, L. Baiotti, R. Bajpai, T. Baka, A. M. Baker, K. A. Baker, T. Baker, G. Baldi, N. Baldicchi, M. Ball, G. Ballardin, S. W. Ballmer, S. Banagiri, B. Banerjee, D. Bankar, T. M. Baptiste, P. Baral, M. Baratti, J. C. Barayoga, B. C. Barish, D. Barker, N. Barman, P. Barneo, F. Barone, B. Barr, L. Barsotti, M. Barsuglia, D. Barta, A. M. Bartoletti, M. A. Barton, I. Bartos, A. Basalaev, R. Bassiri, A. Basti, M. Bawaj, P. Baxi, J. C. Bayley, A. C. Baylor, P. A. Baynard, M. Bazzan, V. M. Bedakihale, F. Beirnaert, M. Bejger, D. Belardinelli, A. S. Bell, D. S. Bellie, L. Bellizzi, W. Benoit, I. Bentara, J. D. Bentley, M. Ben Yaala, S. Bera, F. Bergamin, B. K. Berger, S. Bernuzzi, M. Beroiz, C. P. L. Berry, D. Bersanetti, T. Bertheas, A. Bertolini, J. Betzwieser, D. Beveridge, G. Bevilacqua, N. Bevins, R. Bhandare, R. Bhatt, D. Bhattacharjee, S. Bhattacharyya, S. Bhaumik, S. Bhagwat, V. Biancalana, A. Bianchi, I. A. Bilenko, G. Billingsley, A. Binetti, S. Bini, C. Binu, S. Biot, O. Birnholtz, S. Biscoveanu, A. Bisht, M. Bitossi, M. -A. Bizouard, S. Blaber, J. K. Blackburn, L. A. Blagg, C. D. Blair, D. G. Blair, N. Bode, N. Boettner, G. Boileau, M. Boldrini, G. N. Bolingbroke, A. Bolliand, L. D. Bonavena, R. Bondarescu, F. Bondu, E. Bonilla, M. S. Bonilla, A. Bonino, R. Bonnand, A. Borchers, S. Borhanian, V. Boschi, S. Bose, V. Bossilkov, Y. Bothra, A. Boudon, L. Bourg, M. Boyle, A. Bozzi, C. Bradaschia, P. R. Brady, A. Branch, M. Branchesi, I. Braun, T. Briant, A. Brillet, M. Brinkmann, P. Brockill, E. Brockmueller, A. F. Brooks, B. C. Brown, D. D. Brown, M. L. Brozzetti, S. Brunett, G. Bruno, R. Bruntz, J. Bryant, Y. Bu, F. Bucci, J. Buchanan, O. Bulashenko, T. Bulik, H. J. Bulten, A. Buonanno, K. Burtnyk, R. Buscicchio, D. Buskulic, C. Buy, R. L. Byer, G. S. Cabourn Davies, R. Cabrita, V. Cáceres-Barbosa, L. Cadonati, G. Cagnoli, C. Cahillane, A. Calafat, J. Calderón Bustillo, T. A. Callister, E. Calloni, S. R. Callos, M. Canepa, G. Caneva Santoro, K. C. Cannon, H. Cao, L. A. Capistran, E. Capocasa, E. Capote, G. Capurri, G. Carapella, F. Carbognani, M. Carlassara, J. B. Carlin, T. K. Carlson, M. F. Carney, M. Carpinelli, G. Carrillo, J. J. Carter, G. Carullo, A. Casallas-Lagos, J. Casanueva Diaz, C. Casentini, S. Y. Castro-Lucas, S. Caudill, M. Cavaglià, R. Cavalieri, A. Ceja, G. Cella, P. Cerdá-Durán, E. Cesarini, N. Chabbra, W. Chaibi, A. Chakraborty, P. Chakraborty, S. Chakraborty, S. Chalathadka Subrahmanya, J. C. L. Chan, M. Chan, K. Chandra, K. Chang, S. Chao, P. Charlton, E. Chassande-Mottin, C. Chatterjee, Debarati Chatterjee, Deep Chatterjee, M. Chaturvedi, S. Chaty, K. Chatziioannou, A. Chen, A. H. -Y. Chen, D. Chen, H. Chen, H. Y. Chen, S. Chen, Yanbei Chen, Yitian Chen, H. P. Cheng, P. Chessa, H. T. Cheung, S. Y. Cheung, F. Chiadini, G. Chiarini, A. Chiba, A. Chincarini, M. L. Chiofalo, A. Chiummo, C. Chou, S. Choudhary, N. Christensen, S. S. Y. Chua, G. Ciani, P. Ciecielag, M. Cieślar, M. Cifaldi, B. Cirok, F. Clara, J. A. Clark, T. A. Clarke, P. Clearwater, S. Clesse, F. Cleva, E. Coccia, E. Codazzo, P. -F. Cohadon, S. Colace, E. Colangeli, M. Colleoni, C. G. Collette, J. Collins, S. Colloms, A. Colombo, C. M. Compton, G. Connolly, L. Conti, T. R. Corbitt, I. Cordero-Carrión, S. Corezzi, N. J. Cornish, I. Coronado, A. Corsi, R. Cottingham, M. W. Coughlin, A. Couineaux, P. Couvares, D. M. Coward, R. Coyne, A. Cozzumbo, J. D. E. Creighton, T. D. Creighton, P. Cremonese, S. Crook, R. Crouch, J. Csizmazia, J. R. Cudell, T. J. Cullen, A. Cumming, E. Cuoco, M. Cusinato, L. V. Da Conceição, T. Dal Canton, S. Dal Pra, G. Dálya, B. D'Angelo, S. Danilishin, S. D'Antonio, K. Danzmann, K. E. Darroch, L. P. Dartez, R. Das, A. Dasgupta, V. Dattilo, A. Daumas, N. Davari, I. Dave, A. Davenport, M. Davier, T. F. Davies, D. Davis, L. Davis, M. C. Davis, P. Davis, E. J. Daw, M. Dax, J. De Bolle, M. Deenadayalan, J. Degallaix, M. De Laurentis, F. De Lillo, S. Della Torre, W. Del Pozzo, A. Demagny, F. De Marco, G. Demasi, F. De Matteis, N. Demos, T. Dent, A. Depasse, N. DePergola, R. De Pietri, R. De Rosa, C. De Rossi, M. Desai, R. DeSalvo, A. DeSimone, R. De Simone, A. Dhani, R. Diab, M. C. Dí, M. Di Cesare, G. Dideron, T. Dietrich, L. Di Fiore, C. Di Fronzo, M. Di Giovanni, T. Di Girolamo, D. Diksha, J. Ding, S. Di Pace, I. Di Palma, D. Di Piero, F. Di Renzo, Divyajyoti, A. Dmitriev, J. P. Docherty, Z. Doctor, N. Doerksen, E. Dohmen, A. Doke, A. Domiciano De Souza, L. D'Onofrio, F. Donovan, K. L. Dooley, T. Dooney, S. Doravari, O. Dorosh, W. J. D. Doyle, M. Drago, J. C. Driggers, L. Dunn, U. Dupletsa, P. -A. Duverne, D. D'Urso, P. Dutta Roy, H. Duval, S. E. Dwyer, C. Eassa, M. Ebersold, T. Eckhardt, G. Eddolls, A. Effler, J. Eichholz, H. Einsle, M. Eisenmann, M. Emma, K. Endo, R. Enficiaud, L. Errico, R. Espinosa, M. Esposito, R. C. Essick, H. Estellés, T. Etzel, M. Evans, T. Evstafyeva, B. E. Ewing, J. M. Ezquiaga, F. Fabrizi, V. Fafone, S. Fairhurst, A. M. Farah, B. Farr, W. M. Farr, G. Favaro, M. Favata, M. Fays, M. Fazio, J. Feicht, M. M. Fejer, R. Felicetti, E. Fenyvesi, J. Fernandes, T. Fernandes, D. Fernando, S. Ferraiuolo, T. A. Ferreira, F. Fidecaro, P. Figura, A. Fiori, I. Fiori, R. P. Fisher, R. Fittipaldi, V. Fiumara, R. Flaminio, S. M. Fleischer, L. S. Fleming, E. Floden, H. Fong, J. A. Font, F. Fontinele-Nunes, C. Foo, B. Fornal, K. Franceschetti, N. Franchini, F. Frappez, S. Frasca, F. Frasconi, J. P. Freed, Z. Frei, A. Freise, O. Freitas, R. Frey, W. Frischhertz, P. Fritschel, V. V. Frolov, G. G. Fronzé, M. Fuentes-Garcia, S. Fujii, T. Fujimori, P. Fulda, M. Fyffe, B. Gadre, J. R. Gair, S. Galaudage, V. Galdi, R. Gamba, A. Gamboa, S. Gamoji, D. Ganapathy, A. Ganguly, B. Garaventa, J. García-Bellido, C. García-Quirós, J. W. Gardner, K. A. Gardner, S. Garg, J. Gargiulo, X. Garrido, A. Garron, F. Garufi, P. A. Garver, C. Gasbarra, B. Gateley, F. Gautier, V. Gayathri, T. Gayer, G. Gemme, A. Gennai, V. Gennari, J. George, R. George, O. Gerberding, L. Gergely, Sayantan Ghosh, Shaon Ghosh, Shrobana Ghosh, Suprovo Ghosh, Tathagata Ghosh, J. A. Giaime, K. D. Giardina, D. R. Gibson, C. Gier, S. Gkaitatzis, J. Glanzer, F. Glotin, J. Godfrey, R. V. Godley, P. Godwin, A. S. Goettel, E. Goetz, J. Golomb, S. Gomez Lopez, B. Goncharov, G. González, P. Goodarzi, S. Goode, M. Gosselin, R. Gouaty, D. W. Gould, K. Govorkova, A. Grado, V. Graham, A. E. Granados, M. Granata, V. Granata, S. Gras, P. Grassia, J. Graves, C. Gray, R. Gray, G. Greco, A. C. Green, L. Green, S. M. Green, S. R. Green, C. Greenberg, A. M. Gretarsson, H. K. Griffin, D. Griffith, H. L. Griggs, G. Grignani, C. Grimaud, H. Grote, S. Grunewald, D. Guerra, D. Guetta, G. M. Guidi, A. R. Guimaraes, H. K. Gulati, F. Gulminelli, H. Guo, W. Guo, Y. Guo, Anuradha Gupta, I. Gupta, N. C. Gupta, S. K. Gupta, V. Gupta, N. Gupte, J. Gurs, N. Gutierrez, N. Guttman, F. Guzman, D. Haba, M. Haberland, S. Haino, E. D. Hall, E. Z. Hamilton, G. Hammond, M. Haney, J. Hanks, C. Hanna, M. D. Hannam, A. G. Hanselman, H. Hansen, J. Hanson, S. Hanumasagar, R. Harada, A. R. Hardison, S. Harikumar, K. Haris, I. Harley-Trochimczyk, T. Harmark, J. Harms, G. M. Harry, I. W. Harry, J. Hart, B. Haskell, C. J. Haster, K. Haughian, H. Hayakawa, K. Hayama, M. C. Heintze, J. Heinze, J. Heinzel, H. Heitmann, F. Hellman, A. F. Helmling-Cornell, G. Hemming, O. Henderson-Sapir, M. Hendry, I. S. Heng, M. H. Hennig, C. Henshaw, M. Heurs, A. L. Hewitt, J. Heynen, J. Heyns, S. Higginbotham, S. Hild, S. Hill, Y. Himemoto, N. Hirata, C. Hirose, D. Hofman, B. E. Hogan, N. A. Holland, I. J. Hollows, D. E. Holz, L. Honet, D. J. Horton-Bailey, J. Hough, S. Hourihane, N. T. Howard, E. J. Howell, C. G. Hoy, C. A. Hrishikesh, P. Hsi, H. -F. Hsieh, H. -Y. Hsieh, C. Hsiung, S. -H. Hsu, W. -F. Hsu, Q. Hu, H. Y. Huang, Y. 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Zweizig,Comments: 27 pages, 10 figuresSubjects: astro-ph.HE gr-qcCreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
On 2023 November 23 the two LIGO observatories both detected GW231123, a gravitational-wave signal consistent with the merger of two BLACK HOLEs with masses $137^{+23}_{-18}\, M_\odot$ and $101^{+22}_{-50}\, M_\odot$ (90\% credible intervals), at luminosity distance 0.7-4.1 Gpc and redshift of $0.40^{+0.27}_{-0.25}$, and a network signal-to-noise ratio of $\sim$20.7. Both BLACK HOLEs exhibit high spins, $0.9^{+0.10}_{-0.19}$ and $0.80^{+0.20}_{-0.52}$ respectively. A massive BLACK HOLE remnant is supported by an independent ringdown analysis. Some properties of GW231123 are subject to large systematic uncertainties, as indicated by differences in inferred parameters between signal models. The primary BLACK HOLE lies within or above the theorized mass gap where BLACK HOLEs between 60-130 $M_\odot$ should be rare due to pair instability mechanisms, while the secondary spans the gap. The observation of GW231123 therefore suggests the formation of BLACK HOLEs from channels beyond standard stellar collapse, and that intermediate-mass BLACK HOLEs of mass $\sim$200 $M_\odot$ form through gravitational-wave driven mergers.
[abstract 9 / 53] Yes (score: 6) - Title: Accretion Geometry of the New Galactic Black Hole Candidate AT2019wey in the Hard StateAuthors: Pragati Sahu, Swadesh Chand, Gulab C. Dewangan, Andrzej A. Zdziarski, Vivek K. Agrawal, Parijat Thakur,Comments: 17 pages, 9 figures, 4 tables, Revised version, Submitted on July 11, 2025Subjects: astro-ph.HECreated: 2025-11-09; Updated: 2025-11-11; Datestamp: 2025-11-11
We perform broadband spectral and timing studies of the Galactic low-mass BLACK HOLE candidate AT2019wey during its 2022 outburst, using quasi-simultaneous observations from NICER, SWIFT, and NUSTAR. The long-term MAXI light curve, along with the hardness-intensity diagram (HID) derived from NICER data, indicates that the source remained in the hard state and did not switch to the soft state. Spectral modeling using two different model combinations reveals that the broadband spectrum is best described by two distinct Comptonizing regions, associated reflection components, and thermal emission from the disk. The harder Comptonizing region dominates ($\gtrsim88\%$) the total flux and is primarily responsible for the observed reflection features from the distant part of the disk. We find that the accretion disk is truncated at a radius of $\sim16-56~r_{\rm{g}}$, while the luminosity is $\sim1.9\%$ of the Eddington limit. Our spectral results also show consistency in the estimated inner disk radius obtained through two independent methods: modeling the disk continuum and the reflection spectrum. The variability studies imply the presence of intrinsic disk variability, likely originating from an instability in the disk. We also detect hard time lags at low frequencies, possibly arising from the inward propagation of mass accretion rate fluctuations from the outer to the inner regions of the accretion disk. Moreover, an observed deviation of the lag-energy spectrum from the log-linear trend at $\lesssim 0.7$ keV is most likely attributed to thermal reverberation, arising from the reprocessing of hard coronal photons in the accretion disk.
[abstract 10 / 53] Yes (score: 5) - Title: Hunting for Extragalactic Axion-like Dark Matter in a Decade-long Blazar Optical PolarimetryAuthors: Qiu-Ju Huang, Bao Wang, Jun-Jie Wei, Xue-Feng Wu,Comments: 6 pages, 3 figuresSubjects: astro-ph.HE astro-ph.CO hep-phCreated: 2025-11-08; Updated: 2025-11-11; Datestamp: 2025-11-11
Axions or axion-like particles (ALPs) are well-motivated DARK MATTER (DM) candidates whose coupling to photons induces periodic oscillations in the POLARIZATION angle of astrophysical light. This work reports the first search for such a signature using ten years of optical polarimetric monitoring of the BLAZAR 1ES 1959+650. No statistically significant periodicity is detected using a Lomb-Scargle periodogram and Monte Carlo analysis. Assuming a central DM density in the host galaxy, this null result places tight upper limits on the ALP-photon coupling constant at $g_{aγ}<(5.8 \times 10^{-14}-1.8\times 10^{-10})\,\mathrm{GeV}^{-1}$ across a broad ALP mass range of $m_a \sim (1.4\times10^{-23}-5.2\times10^{-20})\,\mathrm{eV}$. Our constraints surpass those from Very Long Baseline Array polarimetry of active galactic JETs and are competitive with those from long-term Galactic pulsar timing of PSR J0437-4715 over the same ALP mass window. These results establish long-term BLAZAR polarimetry as a competitive and complementary approach for probing axion-like DM on extragalactic scales.
[abstract 11 / 53] Yes (score: 4) - Title: Impact of mass transfer on the orbital evolution of a white dwarf close to an intermediate-mass BLACK HOLEAuthors: Yang Yang, Jie Yang, Xian Chen, Zihan Zhang,Comments: 24 pages, 12 figures, Accepted for publication in MNRASSubjects: astro-ph.HECreated: 2025-11-08; Updated: 2025-11-11; Datestamp: 2025-11-11
Extreme mass ratio inspirals (EMRIs) of low-mass white dwarfs (WDs, 0.1 - 0.3 Msun) around spinning intermediate-mass BLACK HOLEs (IMBHs, 10^3 - 10^5 Msun) offer unique opportunities for multi-messenger astronomy, emitting both gravitational waves (GWs) and electroMAGNETic (EM) signals. Yet, despite their astrophysical relevance, theoretical models often omit key interactions between RELATIVISTIC dynamics and phase-dependent mass transfer (MT). In this study, we integrate a perturbed Keplerian formalism with post-Newtonian (PN) corrections to simulate the RELATIVISTIC orbit of a WD around a rotating IMBH, explicitly resolving the narrow phase near pericentre where Roche-lobe overflow initiates MT. We find that GW emission and MT exert competing influences on the orbit: MT episodes can increase both orbital period and eccentricity, potentially enabling the WD to avoid complete tidal disruption and even escape. We further quantify the GW phase evolution induced by MT, identifying parameter regimes in which GW detectors could observe a one-radian phase shift over observational timescales. Finally, we propose that the orbital expansion driven by MT may lead to the disappearance of quasi-periodic eruptions (QPEs). Our results underscore the necessity of jointly modeling RELATIVISTIC effects and dynamic mass transfer in WD-IMBH systems.
[abstract 12 / 53] Yes (score: 4) - Title: Gravitational Waves from Massive Black Hole Mergers in ASTRID: Predictions for LISAAuthors: Bonny Y. Wang, Yihao Zhou, William Chen, Nianyi Chen, Tiziana Di Matteo, Rupert Croft, Simeon Bird, Yueying Ni,Comments: 19 Pages, 12 Figures; Published in ApJSubjects: astro-ph.GACreated: 2025-11-09; Updated: 2025-11-11; Datestamp: 2025-11-11
We use the ASTRID cosmological simulation to forecast massive BLACK HOLE (MBH) mergers detectable by Laser Interferometer Space Antenna (LISA) down to $z=0$. ASTRID directly models MBH dynamical friction, allowing a realistic tracking of their trajectory. It also incorporates relatively low-mass MBH seeds down to $5\times10^{4} M_{\odot}$, providing a more complete picture of LISA MBH mergers. We find that LISA MBH mergers initially have high eccentricities, peaking around $e_0 = 0.8$ across all redshifts. Accounting for this boosts the event rate from 5.6 yr$^{-1}$ (if circular orbits are assumed) to 10.5 yr$^{-1}$. This enhancement is largely due to additional inspiral sources that will coalesce after LISA's observation, which constitute $46\%$ of detected events.This underscores the importance of LISA's sensitivity to the early inspiral phase, especially for eccentric binaries that emit gravitational waves across a wider frequency band. Most LISA events in ASTRID arise from $M_{\mathrm{BH}}\sim10^{5-6}\ M_\odot$, low-redshift ($z<2$) and low mass-ratio ($q\sim0.01$-$0.1$) mergers. Accounting for eccentricity broadens the detectable MBH mass range up to $10^{9} M_\odot$ and shifts the peak of detectable mergers to a lower redshift $z_{\rm peak}=0.8$. This implies that the most massive LISA events may also be PTA sources. We predict LISA events to be in various galaxy environments, including many low-mass satellite galaxies. The electroMAGNETic (EM) counterparts of most LISA sources have ACTIVE GALACTIC NUCLEi (AGN) luminosities $L_{\rm bol}>10^{42}$ erg s$^{-1}$, albeit only $1\%$ with $>10^{44}$ erg s$^{-1}$. The brightest AGN are those associated with the rare LISA/PTA events with $M_{\rm BH}>10^{8} M_\odot$.
[abstract 13 / 53] Yes (score: 4) - Title: When Magnetic Field Lines Stretch, Snap, and Expand: A New Look at Solar Flares with L-mapsAuthors: Maria D. Kazachenko, Yuhong Fan, Andrey N. Afanasyev,Comments: 11 pages, 5 figures, submitted to Astrophysical Journal on October 23, 2025Subjects: astro-ph.SRCreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
Understanding the three-dimensional evolution of coronal MAGNETic fields during solar flares remains challenging due to the lack of direct coronal field measurements. Here we combine data-driven MHD simulations of NOAA AR 11158 (Fan et al., 2024) with flare-ribbon and coronal-dimming observations to investigate realistic coronal MAGNETic-field evolution during an X-class flare. We introduce L-maps, maps of the logarithm of MAGNETic field line lengths, as a diagnostic tool to track the dynamics of simulated coronal MAGNETic structures. Variations in L-maps identify flare ribbons through field-line shortening and coronal dimmings through field-line lengthening. Comparison with SDO/AIA observations demonstrates strong morphological and temporal agreement, validating the simulated field evolution. Applying K-means clustering to the L-map temporal profiles, we distinguish three stages of coronal evolution: (1) slow pre-flare rise phase, (2) flare RECONNECTion accompanied by CME rise, and (3) post-RECONNECTion CME expansion. We detect a slow pre-flare rise phase of MAGNETic field lines rooted in ribbon footpoints and identify a new phenomenon, RECONNECTion dimming, a rapid expansion of RECONNECTed inner flux-rope field lines during the impulsive phase. Our results show that L-maps provide a powerful and physically intuitive framework for bridging simulations and observations and for tracking the full three-dimensional evolution of coronal MAGNETic fields during flares.
[abstract 14 / 53] Yes (score: 4) - Title: The future ability to test theories of gravity with black-hole shadowsAuthors: Akhil Uniyal, Indu K. Dihingia, Yosuke Mizuno, Luciano Rezzolla,Comments: Published in Nature AstronomySubjects: gr-qcCreated: 2025-11-05; Updated: 2025-11-11; Datestamp: 2025-11-11
The horizon-scale images of supermassive BLACK HOLEs (BHs) by the Event Horizon Telescope Collaboration (EHT) have provided new opportunities to test general relativity and other theories of gravity. In view of future projects, such as the next-generation Event Horizon Telescope (ngEHT) and the Black-Hole Explorer (BHEX), having the potential of enhancing our ability to probe extreme gravity, it is natural to ask: \textit{how much can two black-hole images differ?} To address this question and assess the ability of these projects to test theories of gravity with black-hole shadows, we use general-RELATIVISTIC MAGNETohydrodynamic and radiative-transfer simulations to investigate the images of a wide class of accreting BHs deviating from the Kerr solution. By measuring the mismatch between images of different BHs we show that future missions will be able to distinguish a large class of BHs solutions from the Kerr solution when the mismatch in the images exceeds values between $2\%$ and $5\%$ depending on the image-comparison metric considered. These results indicate future horizon-scale imaging with percent-level image fidelity can place meaningful observational constraints on deviations from the Kerr metric and thereby test strong-field predictions of general relativity.
[abstract 15 / 53] Yes (score: 4) - Title: Towards the Composition of sub-PeV Cosmic Rays at IceCubeAuthors: Julian Saffer,Comments: Presented at the XVIII International Conference on Topics in Astroparticle and Underground Physics (TAUP 2023)Subjects: astro-ph.HECreated: 2025-11-07; Updated: 2025-11-11; Datestamp: 2025-11-11
With the implementation of a low-energy trigger, the surface array of the IceCube Neutrino Observatory is able to record cosmic-ray induced air showers with a primary energy of a few hundred TeV. This extension of the energy range closes the gap between direct and indirect observations of primary COSMIC RAYs and provides the potential to test the validity of hadronic interaction models in the sub-PeV regime. Composition analyses at IceCube highly benefit from its multi-detector design. Combining the measurement of the electroMAGNETic shower component and low-energy muons at the surface with the response of the in-ice array to the associated high-energy muons improves the directional reconstruction accuracy and opens unique possibilities to extract the primary particle's mass. In this contribution, a new methodical approach for the analysis of these low-energy air showers is presented, including techniques for the identification of coincident background in the in-ice detector and a machine learning model based on convolutional neural networks to determine the elemental composition. The achieved performance in primary mass discrimination and energy reconstruction of air-shower events is discussed.
[abstract 16 / 53] Yes (score: 4) - Title: A JWST/NIRSpec Integral Field Unit Survey of Luminous Quasars at z ~ 5-6 (Q-IFU): Rest-frame Optical Nuclear Properties and Extended NebulaeAuthors: Weizhe Liu, Xiaohui Fan, Huan Li, Richard Green, Jaclyn B. Champagne, Xiangyu Jin, Jianwei Lyu, Maria Pudoka, Wei Leong Tee, Feige Wang, Jinyi Yang, Yongda Zhu, Nayera Abdessalam,Comments: 22 pages, 12 figures, submitted to ApJ, comments are more than welcome!Subjects: astro-ph.GA astro-ph.COCreated: 2025-11-08; Updated: 2025-11-11; Datestamp: 2025-11-11
It remains debatable how billion-solar-mass supermassive BLACK HOLEs (SMBHs) form and evolve within the first billion years. We report results from a James Webb Space Telescope (JWST)/NIRSpec integral field unit (IFU) survey of 27 luminous QUASARs at $z \sim 5$-$6$, enabling a systematic investigation of their key physical properties and the associated, extended line emission. Our sample hosts SMBHs with $\log(M_{\mathrm{BH}}/M_\odot) \sim 8.6$-$9.7$ and Eddington ratios of $\sim 0.1$-$2.6$ based on H$β$, and the H$β$-based and H$α$-based BH mass are broadly consistent with each other. Our sample may have a slightly smaller median BH mass and larger median Eddington ratio than lower-redshift QUASARs within the same luminosity range, although the difference could still be explained by statistical uncertainties. They generally follow the empirical correlations between [O III] $λ$5007 equivalent width and bolometric luminosities or Eddington ratios formed by lower-redshift QUASARs. The majority of them fall within the Eigenvector~1 planes formed by lower-redshift QUASARs. Nevertheless, a subset of the sample shows enhanced, blueshifted [O III] emission associated with fast outflows. Spatially extended [O III] line emission is detected in 6 objects and shows morphologies and kinematics consistent with merging activities and/or turbulent and clumpy interstellar media (ISM). Tentative evidence of QUASAR radiative feedback shaping the ISM of a merging companion galaxy is seen in the object with the most extended [O III] emission. Our results provide crucial insight into the rapid growth of SMBHs and the gaseous environments they reside in at z$\sim$5-6.
[abstract 17 / 53] Yes (score: 4) - Title: Kerr Black Hole Shadows in Dispersive Plasma: Frequency-Dependent Geodesics and Shadow DistortionsAuthors: Sai Karan Mukthapuram, Sandeep Kumar Kataria,Comments: 12 pages, 4 figuresSubjects: astro-ph.HE gr-qc physics.plasm-phCreated: 2025-11-09; Updated: 2025-11-11; Datestamp: 2025-11-11
The BLACK HOLE shadow, a direct probe of the event horizon's gravitational influence, has been observationally confirmed by the Event Horizon Telescope (EHT). While theoretical models of shadows in vacuum are mature, real astrophysical BLACK HOLEs like M87* and Sgr A* are enveloped in plasma, which can alter photon trajectories through dispersion. Current understanding, based on foundational work, indicates that only specific plasma distributions allow for an analytical treatment via the separation of the Hamilton-Jacobi equation. In this work, we build upon this framework to systematically investigate the propagation of light rays in Kerr spacetime surrounded by a pressureless, non-MAGNETized cold plasma. We explicitly derive the separability condition, identifying the exact class of plasma densities that permit a generalized Carter constant. For these models, we compute the photon regions and shadow boundaries, characterizing how the shadow's size and shape deviate from the vacuum case in a frequency-dependent manner. Our results provide analytical benchmarks for the distortion of shadows in dispersive media and determine the critical plasma frequency beyond which the shadow is erased, offering a direct link between observable shadow features and the properties of the ambient plasma environment and providing a foundation for studying more dynamic, non-separable plasma distributions.
[abstract 18 / 53] Yes (score: 4) - Title: Seyfert Galaxies as Neutrino Sources: An Outflow$-$Cloud Interaction PerspectiveAuthors: Zhi-Peng Ma, Kai Wang, Yuan-Yuan Zuo, Yuan-Chuan Zou, Yong-Han Huang,Comments:Subjects: astro-ph.HECreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
Following the identification of the first confirmed individual neutrino source, Seyfert galaxies have emerged as the most prominent class of high-energy neutrino emitters. In this work, we perform a detailed investigation of the outflow--cloud interaction scenario for neutrino production in Seyfert nuclei. In this framework, fast AGN-driven winds collide with clumpy gas clouds in the nuclear region, forming bow shocks that efficiently accelerate cosmic-ray protons. The accelerated protons subsequently interact with cold protons from the outflows via inelastic proton--proton ($pp$) collisions, producing high-energy neutrinos, while the photomeson ($pγ$) process with disk photons may provide a subdominant contribution at the highest energies. Applying this model to five neutrino-associated Seyfert galaxies, we successfully reproduce the observed TeV neutrino fluxes without violating existing gamma-ray constraints. By integrating over the Seyfert population using X-ray luminosity functions, we further demonstrate that Seyfert galaxies can account for a substantial fraction of the diffuse astrophysical neutrino background in the $10^4-10^5~{\rm GeV}$ energy range.
[abstract 19 / 53] Yes (score: 4) - Title: Analysis and implications of the spatio-spectral morphology of the FERMI BubblesAuthors: Ami Tank, Roland Crocker, Mark R. Krumholz,Comments: 12 pages, 11 figures, Submitted to The Open Journal of Astrophysics, Data available at https://doi.org/10.5281/zenodo.17568107Subjects: astro-ph.HE astro-ph.GACreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
The FERMI Bubbles are gamma-ray structures extending from the center of the Milky Way to +/-50 degree Galactic latitude that were discovered in data obtained by the FERMI/LAT instrument. Their origin and power source remain uncertain. To help address this uncertainty, here we use a template-free reconstruction of ten years of all-sky FERMI/LAT data provided by Platz et al. (2023) to carry out a pixel-by-pixel spectral analysis of the Bubbles. We recover the position-dependent spectral shape and normalization that would be required for parent proton or electron COSMIC RAY populations to produce the Bubbles' observed gamma-ray spectra. We find that models in which the gamma-ray emission is driven by either hadronic or leptonic processes can explain the data equally well. The COSMIC RAY population driving the emission must have either broken power-law or exponentially cut-off spectra, with break or cutoff energies that are almost constant with latitude but spectral indices below the break that harden towards the Bubbles' southern tip. For the leptonic channel, reproducing the observed position-dependent gamma-ray spectrum also requires a COSMIC RAY electron energy density that grows with distance from the Galactic plane and increases towards the edges of the Bubbles. This finding disfavors scenarios for the origin of the Bubbles where a population of COSMIC RAY electrons is accelerated near the Milky Way center and subsequently advected out to the extremities of the Bubbles.
[abstract 20 / 53] (score: 3) - Title: Near-infrared Variability Detected in the Young Star-Forming Dwarf Galaxy SBS 0335-052EAuthors: Shun Hatano, Mitsuru Kokubo, Masami Ouchi, Kimihiko Nakajima, Toshihiro Kawaguchi, Satoshi Kikuta, Nozomu Tominaga, Yi Xu, Kuria Watanabe, Yuichi Harikane, Yuki Isobe, Akinori Matsumoto, Moka Nishigaki, Yoshiaki Ono, Masato Onodera, Yuma Sugahara, Hiroya Umeda, Yechi Zhang, Ryotaro Chiba, Takashi J. Moriya,Comments: 19 pages, 5 figures, submitted to ApJSubjects: astro-ph.GACreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
SBS~0335-052E is a young star-forming dwarf galaxy with a total stellar mass of $M_{*} \lesssim 10^{8}~M_{\odot}$ and an extremely low metallicity ($Z \sim 1/40~Z_{\odot}$), which has long been considered to be devoid of an ACTIVE GALACTIC NUCLEus (AGN). Here we report the detection of temporal flux variability of SBS~0335-052E in near-infrared (NIR) 3-4\ ${\rm μ}$m bands on timescales of several years, showing dimming and brightening of up to 50\% over 14~years, based on archival data from the Wide-field Infrared Survey Explorer. Our spectral energy distribution (SED) fitting of archival ultraviolet (UV)-NIR photometry, including AGN SED models, indicates that the variable NIR emission arises from an edge-on AGN dust torus. The UV-optical emission from the accretion disk is obscured and does not reach us, leading to the dominance of the host galaxy's young stellar population in the UV-optical wavelengths. This analysis favors the presence of a Compton-thick, heavily obscured AGN in SBS~0335-052E, consistent with its observed X-ray weakness. From the SED fitting, we estimate an AGN bolometric luminosity of $L_{\rm bol} = 1.2\times10^{43}\ {\rm erg\ s^{-1}}$, which implies a BLACK HOLE mass of $M_{\rm BH} \simeq 10^{5}\ M_\odot$ if the AGN is accreting at the Eddington limit. If confirmed, SBS~0335-052E would be the least massive galaxy known to host an AGN, likely harboring an intermediate-mass BLACK HOLE.
[abstract 21 / 53] (score: 3) - Title: A probe of the maximum energetics of fast radio bursts through a prolific repeating sourceAuthors: O. S. Ould-Boukattine, P. Chawla, J. W. T. Hessels, A. J. Cooper, M. P. Gawroński, W. Herrmann, D. M. Hewitt, J. Huang, D. Huppenkothen, F. Kirsten, D. C. Konijn, K. Nimmo, Z. Pleunis, W. Puchalska, M. P. Snelders,Comments: accepted for publication in MNRAS, see https://doi.org/10.1093/mnras/staf1937Subjects: astro-ph.HECreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
Fast radio bursts (FRBs) are sufficiently energetic to be detectable from luminosity distances up to at least seven billion parsecs (redshift $z > 1$). Probing the maximum energies and luminosities of FRBs constrains their emission mechanism and cosmological population. Here we investigate the maximum energetics of a highly active repeater, FRB 20220912A, using 1,500 h of observations. We detect $130$ high-energy bursts and find a break in the burst energy distribution, with a flattening of the power-law slope at higher energy -- consistent with the behaviour of another highly active repeater, FRB 20201124A. There is a roughly equal split of integrated burst energy between the low- and high-energy regimes. Furthermore, we model the rate of the highest-energy bursts and find a turnover at a characteristic spectral energy density of $E^{\textrm{char}}_ν = 2.09^{+3.78}_{-1.04}\times10^{32}$ erg/Hz. This characteristic maximum energy agrees well with observations of apparently one-off FRBs, suggesting a common physical mechanism for their emission. The extreme burst energies push radiation and source models to their limit: at this burst rate a typical MAGNETar ($B = 10^{15}$ G) would deplete the energy stored in its MAGNETosphere in $\sim$ 2150 h, assuming a radio efficiency $ε_\mathrm{radio} = 10^{-5}$. We find that the high-energy bursts ($E_ν> 3 \times 10^{30}$ erg Hz$^{-1}$) play an important role in exhausting the energy budget of the source.
[abstract 22 / 53] (score: 3) - Title: Properties of Pair Plasmas Emerging from ElectroMAGNETic Showers in MatterAuthors: M. Pouyez, G. Nicotera, M. Galbiati, T. Grismayer, L. Lancia, C. Riconda, M. Grech,Comments:Subjects: physics.plasm-ph astro-ph.HE hep-ex hep-thCreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
ElectroMAGNETic showers from high-energy electron beams interacting with a target are a promising path to creating pair plasmas in the laboratory. Here, we solve analytically the kinetic equations describing this process. Two regimes are defined by the ratio of the target thickness $L$ to the shower length $L_{\rm{sh}}$, which depends on the electron energy and target composition. For thin targets ($L < L_{\rm{sh}}$), we derive explicit expressions for the spectra of produced photons and pairs, as well as the number of pairs. For thick targets ($L > L_{\rm{sh}}$), we obtain the total pair number and photon spectrum. Analytical results agree well with Geant4 simulations, and it is found that significant pair escape requires $L < L_{\rm{sh}}$. The divergence, density and characteristic dimensions of the escaping pair JETs are derived, and a criterion for pair plasma formation is obtained. While current LASER wakefield beams are not well adapted, multi-petawatt LASERs may provide new electron or photon sources suitable for laboratory pair plasma production.
[abstract 23 / 53] (score: 3) - Title: Confronting general relativity with principal component analysis: Simulations and results from GWTC-3 eventsAuthors: Parthapratim Mahapatra, Sayantani Datta, Ish Gupta, Poulami Dutta Roy, Muhammed Saleem, Purnima Narayan, Soumen Roy, Jan Steinhoff, Deirdre Shoemaker, Alan J. Weinstein, Anuradha Gupta, B. S. Sathyaprakash, K. G. Arun,Comments: 26 pages, 10 figures, 9 tablesSubjects: gr-qc astro-ph.HECreated: 2025-11-08; Updated: 2025-11-11; Datestamp: 2025-11-11
We present a comprehensive assessment of multiparameter tests of general relativity (GR) in the inspiral regime of compact binary coalescences using principal component analysis (PCA). Our analysis is based on an extensive set of simulated gravitational-wave (GW) signals, including both general RELATIVISTIC and non-GR sources, injected into zero-noise data colored by the noise power spectral densities of the LIGO and Virgo GW detectors at their designed sensitivities. We evaluate the performance of PCA-based methods in the context of two established frameworks: TIGER and FTI. For GR-consistent signals, we find that PCA enables stringent constraints on potential deviations from GR, even in the presence of multiple free parameters. Applying the method to simulated signals that explicitly violate GR, we demonstrate that PCA is effective at identifying such deviations. We further test the method using numerical relativity waveforms of eccentric binary BLACK HOLE systems and show that missing physical effects--such as orbital eccentricity--can lead to apparent violations of GR if not properly included in the waveform models used for analysis. Finally, we apply our PCA-based test to selected real gravitational-wave events from GWTC-3, including GW190814 and GW190412. We present joint constraints from selected binary BLACK HOLE events in GWTC-3, finding that the 90% credible bound on the most informative PCA parameter is $0.03^{+0.08}_{-0.08}$ in the TIGER framework and $-0.01^{+0.05}_{-0.04}$ in the FTI framework, both of which are consistent with GR. These results highlight the sensitivity and robustness of the PCA-based approach and demonstrate its readiness for application to future observational data from the fourth observing runs of LIGO, Virgo, and KAGRA.
[abstract 24 / 53] (score: 3) - Title: Laboratory formation of scaled astrophysical outflowsAuthors: Shun-yi Yang, Guang-yue Hu, Chao Xiong, Tian-yi Li, Xue-cheng Li, Hui-bo Tang, Shuo-ting Shao, Xiang Lv, Chen Zhang, Ming-yang Yu,Comments:Subjects: physics.plasm-phCreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
Astrophysical systems exhibit a rich diversity of outflow morphologies, yet their mechanisms and existence conditions remain among the most persistent puzzles in the field. Here we present scaled laboratory experiments based on LASER-driven plasma outflow into MAGNETized ambient gas, which mimic five basic astrophysical outflows regulated by interstellar medium, namely collimated JETs, blocked JETs, elliptical bubbles, as well as spherical winds and bubbles. Their morphologies and existence conditions are found to be uniquely determined by the external Alfvenic and sonic Mach numbers Me-a and Me-s, i.e. the relative strengths of the outflow ram pressure against the MAGNETic/thermal pressures in the interstellar medium, with transitions occurring at Me-a ~ 2 and 0.5, as well as Me-s ~ 1. These results are confirmed by MAGNETohydrodynamics simulations and should also be verifiable from existing and future astronomical observations. Our findings provide a quantitative framework for understanding astrophysical outflows.
[abstract 25 / 53] (score: 3) - Title: Continuum Reverberation Mapping of 18 AGN Over Four YearsAuthors: Jake A. Miller, Edward M. Cackett, Misty C. Bentz, Michael R. Goad, Kirk T. Korista, Ian M. McHardy,Comments: 26 Pages, 7 Figures (5 In Main and 2 in Appendix), Accepted for publication in ApJSubjects: astro-ph.GA astro-ph.HECreated: 2025-11-07; Updated: 2025-11-11; Datestamp: 2025-11-11
Continuum reverberation mapping probes the size scale of the optical continuum-emitting region in ACTIVE GALACTIC NUCLEi (AGN). The source of this emission has long been thought to originate from the accretion disk, but recent studies suggest the broad line region (BLR) may significantly contribute to both the observed flux and continuum interband delays. We monitored 18 AGN over four years of observations to acquire high quality optical continuum light curves, measuring time lags between different photometric bands and determining continuum emission sizes for each AGN. We add this sample to existing lag measurements to test the correlation between continuum lags at $5100Å$ ($τ_{5100}$) and $5100Å$ luminosity ($L_{5100}$). We observe that $τ_{5100} \propto L_{5100}^{0.4}$, broadly consistent with the theoretical expectations of $τ\propto L^{1/2}$ expected for continuum reverberation from either the accretion disk or the BLR.
[abstract 26 / 53] (score: 3) - Title: The UV/optical Continuum Reverberation Mapping of Eight Active Galactic Nuclei with SWIFT: Further Evidence for the Outer ComponentAuthors: Chi-Zhuo Wang, Xue-Bing Wu, Yuanzhe Jiang, Qinchun Ma, Huapeng Gu, Yuhan Wen,Comments: Accepted for publication in ApJ, 26 pages, 16 figures, 4 tables. The processed light curves are available on Zenodo at DOI: 10.5281/zenodo.14930797Subjects: astro-ph.GACreated: 2025-11-08; Updated: 2025-11-11; Datestamp: 2025-11-11
In our previous work, we applied the ICCF-Cut method to the continuum reverberation mapping (CRM) of six ACTIVE GALACTIC NUCLEi (AGNs) based on the published SWIFT data. Extending this work, we perform a systematic AGN CRM study utilizing the SWIFT archive. We enlarge our sample with eight additional AGNs at $z<0.05$ with high-cadence ($<3$ days) and multiband photometric observations. Time series analysis of these light curves shows two main results: (1) The interband lags are broadly consistent with $τ\propto λ^{4/3}$, while the average interband lags are larger than those predicted by the standard thin accretion disk model. (2) For most targets, there exists a $U$ band lag excess, which is probably due to the diffuse continuum emission from the broad-line region (BLR). We employ the ICCF-Cut method to extract the possible diffuse continuum component from the $U$ band light curves and calculate the diffuse continuum lags ($τ_{\rm cut}$), which are generally consistent with the lags ($τ_{\rm jav}$) derived by the JAVELIN Photometric Reverberation Mapping Model. Further analysis with our sample indicates a positive correlation between the diffuse continuum region size and the BLR size ($R_{\rm DCR}-R_{\rm BLR}$ relation), as well as another correlation with the luminosity ($R_{\rm DCR}-L$ relation). These findings provide further evidence for a significant contribution of diffuse continuum emission from the BLR to the AGN continuum lags.
[abstract 27 / 53] (score: 3) - Title: Supermassive Black Hole and Broad-line Region in NGC 5548: 2023 Reverberation Mapping ResultsAuthors: Wen-Zhe Xi, Kai-Xing Lu, Jin-Ming Bai, Zhang Yue, Weimin Yi, Liang Xu, Sha-Sha Li, Hai-Cheng Feng, Jian-Guo Wang,Comments: 15 pages, 6 figures, 4 Tables, accepted by ApJSubjects: astro-ph.GACreated: 2025-11-08; Updated: 2025-11-11; Datestamp: 2025-11-11
We present the results of the 2023 spectroscopic reverberation mapping (RM) campaign for ACTIVE GALACTIC NUCLEi (AGN) of NGC 5548, continuing our long-term monitoring program. Using the Lijiang 2.4-meter telescope, we obtained 74 spectra with a median cadence of 1.9 days. Through detailed spectral decomposition, we measured the light curves of the optical continuum at 5100~Å and the broad He~{\sc ii}, He~{\sc i}, H$γ$, and H$β$ emission lines. The time lags of these lines relative to the continuum are measured as $1.3^{+1.6}_{-0.6}$, $2.3^{+1.5}_{-2.1}$, $10.0^{+2.0}_{-1.8}$, and $15.6^{+2.6}_{-2.9}$ days (rest-frame), respectively. Velocity-resolved lag profiles for H$γ$ and H$β$ were constructed. Combined with data from previous seasons (2015$-$2021), we find that the radial ionization stratification of the broad-line region (BLR) is stable; the average virial mass of the supermassive BLACK HOLE in NGC~5548 is $(2.6\pm1.1)\times 10^{8}M_{\odot}$, consistent with the $M_{\rm BH}-σ_*$ relation; the broad He~{\sc ii} line exhibits the largest responsivity, followed by broad He~{\sc i} (or H$γ$) and H$β$ lines; the BLR kinematics show significant temporal evolution, transitioning from virialized motions to signatures of inflow and outflow. Furthermore, an analysis of 35 years of historical data confirms a 3.5-year time lag between variations in the optical luminosity and the BLR radius, potentially implicating the role of radiation pressure or dynamical structure changes in the inner accretion disk. Long-term campaign demonstrates that the BLR in NGC 5548 is a robust yet dynamically evolving entity, providing crucial insights into AGN structure and accretion physics.
[abstract 28 / 53] (score: 3) - Title: On the numerical convergence of MRI simulationsAuthors: Thomas Jannaud, Henrik N. Latter,Comments: Accepted for publication in MNRAS. 14 pages and 14 figures, including 2 pages and 6 figures in the appendixSubjects: astro-ph.HE astro-ph.SRCreated: 2025-11-08; Updated: 2025-11-11; Datestamp: 2025-11-11
The MAGNETorotational instability (MRI) plays a crucial role in the evolution of many types of accretion disks. It is often studied using ideal-MHD numerical simulations. In principle, such simulations should be numerically converged, i.e. their properties should not change with resolution. Convergence is often assessed via the MRI quality factor, $Q$, the ratio of the Alfvén length to the grid-cell size. If it is above a certain threshold, the simulation is deemed numerically converged. In this paper we argue that the quality factor is not a good indicator of numerical convergence. First, we test the performance of the quality factor on simulations known to be unconverged, i.e. local ideal-MHD simulations with zero net-flux, and show that their $Q$s are well over the typical convergence threshold. The quality-factor test thus fails in these cases. Second, we take issue with the linear theory underpinning the use of $Q$, which posits a constant vertical field. This is a poor approximation in real nonlinear simulations, where the vertical field can vary rapidly in space and generically exhibits zeros. We calculate the linear MRI modes in such cases and show that the MRI can reach near-maximal growth rates at arbitrarily small scales. Yet, the quality factor assumes a single and well-defined scale, near the Alfvén length, below which the MRI cannot grow. We discuss other criticisms and suggest a modified quality factor that addresses some, though not all, of these issues.
[abstract 29 / 53] (score: 3) - Title: Force-free Electrodynamics in Arbitrary GeometriesAuthors: Rakshak Adhikari,Comments:Subjects: gr-qcCreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
The dynamics of highly MAGNETized plasmas in extreme astrophysical environments are effectively modeled by Force-Free Electrodynamics (FFE), a framework essential for studying objects like neutron stars and accreting BLACK HOLEs. The inherently nonlinear nature of the FFE equations makes finding exact solutions a challenging task. This paper explores an innovative approach to solving these equations by foliating spacetime into two-dimensional surfaces, specifically tailored to the geometry of electroMAGNETic fields. The foliation approach exploits the fact that the kernel of the force-free field defines an involutive distribution, naturally lending itself to a geometric decomposition. This method has previously been applied with great success in Kerr and FLRW spacetimes. By extending this formalism, we develop new exact solutions to the FFE equations in several distinct spacetimes, including cases where the metric remains partially undetermined. Additionally, we present a novel class of solutions that smoothly transition between MAGNETically dominated and electrically dominated regimes over time. Finally, we construct a pair of vacuum degenerate fields in arbitrary axisymmetric spacetimes, further demonstrating the utility of the foliation approach. These results offer a new perspective on the dynamical evolution of electroMAGNETic fields and their geometric underpinnings in various spacetime geometries, broadening the applicability of the framework for understanding the dynamics of highly MAGNETized plasmas in general RELATIVISTIC astrophysical contexts.
[abstract 30 / 53] (score: 3) - Title: Vacuum Polarization Effects in Baryon-Loaded Magnetar Bursts and Implications for X-ray PolarizationAuthors: Tomoki Wada,Comments: 15 pages, 5 figures, accepted for publication in Physical Review DSubjects: astro-ph.HECreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
Magnetars provide natural laboratories for strong-field quantum electrodynamics processes, such as vacuum POLARIZATION, which gives rise to vacuum resonance together with the plasma response. We develop a general framework to describe vacuum resonance in a three-component plasma consisting of ions, electrons, and positrons, as expected in baryon-loaded MAGNETar bursts. By introducing a parametrization of the plasma composition, we establish the general criterion for the occurrence of vacuum resonance in such plasmas. Our analysis encompasses both Mikheyev-Smirnov-Wolfenstein-like adiabatic mode conversion and nonadiabatic eigenmode transition, highlighting their dependence on the plasma composition. Applying this framework to baryon-loaded fireballs in MAGNETar bursts, we estimate the characteristic X-ray POLARIZATION signatures. Detection of these POLARIZATIONs will provide observational signatures of vacuum POLARIZATION as well as baryon loading in MAGNETar fireballs.
[abstract 31 / 53] (score: 3) - Title: Pulse profile modelling of the accretion-powered millisecond pulsar SAX J1808.4-3658 using NICER data from its 2019 and 2022 outburstsAuthors: Bas Dorsman, Tuomo Salmi, Anna L. Watts, Mason Ng, Anna Bobrikova, Vladislav Loktev, Juri Poutanen, Joern Wilms,Comments: 21 pages, 11 figures, 3 tables. Accepted in MNRASSubjects: astro-ph.HECreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
Pulse profile modelling is a RELATIVISTIC ray-tracing technique that has provided constraints on parameters, with a focus on mass and radius, of five rotation-powered millisecond pulsars. While the technique can also be applied to accretion-powered millisecond pulsars (AMPs), this requires accounting for the X-rays from the accretion disc and has only been applied to archival data from the Rossi X-ray Timing Explorer. Here, we apply a previously developed neutron star and accretion disc model to the NICER (Neutron star Interior Composition Explorer) data of the 2019 and 2022 outbursts of SAX J1808.4-3658. We find that a single circular hotspot model is insufficient to explain the data. Modelling with two hotspots and an accretion disc model provides better phase-residuals, but a spectral residual at around 1 keV remains. In contrast, we find a good fit with a flexible background approach, replacing the accretion disk. However, the inferred parameters are not robust due to a degeneracy in the origin of the non-pulsed radiation, which can be caused either by the background or a hotspot that is at least partially in view throughout a full rotation. This work represents an important next step in pulse profile modelling of AMPs by analysing NICER data and underlines the need for more accurate accretion disc and hotspot modelling to achieve robust parameter constraints. We expect the inclusion of higher energy and polarimetric data will provide complementary constraints on inclination, hotspot colatitude, and hotspot size, improving the accuracy of pulse profile modelling of AMPs.
[abstract 32 / 53] (score: 3) - Title: Search for steady and flaring neutrino emission from cosmic sources using the complete ANTARES datasetAuthors: ANTARES Collaboration, A. Albert, S. Alves, M. André, M. Ardid, S. Ardid, J. J. Aubert, J. Aublin, B. Baret, S. Basa, Y. Becherini, B. Belhorma, F. Benfenati, V. Bertin, S. Biagi, J. Boumaaza, M. Bouta, M. C. Bouwhuis, H. Brânzaş, R. Bruijn, J. Brunner, J. Busto, B. Caiffi, D. Calvo, S. Campion, A. Capone, F. Carenini, J. Carr, V. Carretero, T. Cartraud, S. Celli, L. Cerisy, M. Chabab, R. Cherkaoui El Moursli, T. Chiarusi, M. Circella, J. A. B. Coelho, A. Coleiro, R. Coniglione, P. Coyle, A. Creusot, A. F. Díaz, B. De Martino, C. Distefano, I. Di Palma, C. Donzaud, D. Dornic, D. Drouhin, T. Eberl, A. Eddymaoui, T. van Eeden, D. van Eijk, S. El Hedri, N. El Khayati, A. Enzenhöfer, P. Fermani, G. Ferrara, F. Filippini, L. Fusco, S. Gagliardini, J. García, C. Gatius Oliver, P. Gay, N. Geißelbrecht, H. Glotin, R. Gozzini, R. Gracia Ruiz, K. Graf, C. Guidi, L. Haegel, S. Hallmann, H. van Haren, A. J. Heijboer, Y. Hello, L. Hennig, J. J. Hernández-Rey, J. Hößl, F. Huang, G. Illuminati, B. Jisse-Jung, M. de Jong, P. de Jong, M. Kadler, O. Kalekin, U. Katz, A. Kouchner, I. Kreykenbohm, V. Kulikovskiy, R. Lahmann, M. Lamoureux, A. Lazo, D. Lefèvre, E. Leonora, G. Levi, S. Le Stum, S. Loucatos, J. Manczak, M. Marcelin, A. Margiotta, A. Marinelli, J. A. Martínez-Mora, P. Migliozzi, A. Moussa, R. Muller, S. Navas, E. Nezri, B. Ó Fearraigh, E. Oukacha, A. M. Păun, G. E. Păvălaş, S. Peña-Martínez, M. Perrin-Terrin, P. Piattelli, C. Poirè, V. Popa, T. Pradier, N. Randazzo, D. Real, G. Riccobene, A. Romanov, A. Sánchez Losa, A. Saina, F. Salesa Greus, D. F. E. Samtleben, M. Sanguineti, P. Sapienza, F. Schüssler, J. Seneca, M. Spurio, Th. Stolarczyk, M. Taiuti, Y. Tayalati, B. Vallage, G. Vannoye, V. Van Elewyck, S. Viola, D. Vivolo, J. Wilms, S. Zavatarelli, A. Zegarelli, J. D. Zornoza, J. Zúñiga,Comments:Subjects: astro-ph.HECreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
ANTARES, a neutrino detector located in the depths of the Mediterranean Sea, operated successfully for over 15 years before being decommissioned in 2022. The telescope offered an ideal vantage view of the Southern Sky and benefited from optimal water properties for enhanced angular resolution. This study makes use of data collected over the entire operational period of ANTARES to search for sources of high-energy cosmic neutrinos, considering both steady and flaring emission scenarios. First, a time-integrated search for high-energy neutrino clustering across the celestial sphere is conducted. The most significant accumulation is found at coordinates $(α, δ) =(200.5^\circ\, 17.7^\circ)$ with a post-trial p-value equal to 0.38. A dedicated search in the Galactic Plane is also performed for extended sources, yielding no significant excess. Additionally, a list of potential neutrino sources are investigated. The BLAZAR MG3 J225517+2409 is identified as the most significant object, yet the excess remains compatible with background fluctuations. A mild local excess of 2.4$σ$ is found for the BLAZAR TXS 0506+056. The full sky is also examined for the presence of flaring neutrino emissions. The most significant excess in this case corresponds to a $\sim$4-day flare from the direction $(α, δ) = (141.3^\circ\, 9.8^\circ)$, with a post-trial p-value of 0.30. Finally, the directions of sources highlighted in IceCube's time-dependent searches are investigated. Temporal overlaps between ANTARES and IceCube flares are identified for PKS 1502+106 and TXS 0506+056, with an estimated chance probability of about 0.02%, making this observation particularly noteworthy.
[abstract 33 / 53] (score: 2) - Title: Modeling of the High Column Density systems in The Lyman-Alpha ForestAuthors: T. Tan, J. Rich, E. Chaussidon, J. M. Le Goff, C. Balland, E. Armengaud, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, P. Martini, R. Miquel, S. Nadathur, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, G. Rossi, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, D. Sprayberry, G. Tarlé, M. Walther, B. A. Weaver, H. Zou,Comments:Subjects: astro-ph.COCreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
The Lyman-$α$ forests observed in the spectra of high-redshift QUASARs can be used as a tracer of the cosmological matter density to study baryon acoustic oscillations (BAO) and the Alcock-Paczynski effect. Extraction of cosmological information from these studies requires modeling of the forest correlations. While the models depend most importantly on the bias parameters of the intergalactic medium (IGM), they also depend on the numbers and characteristics of high-column-density systems (HCDs) ranging from Lyman-limit systems with column densities $\log_{10}\!\bigl(N_{\mathrm{HI}}/\mathrm{cm}^{-2}\bigr)>17$ to damped Lyman-$α$ systems (DLAs) with $\log_{10}\!\bigl(N_{\mathrm{HI}}/\mathrm{cm}^{-2}\bigr)>20.2$. These HCDs introduce broad damped absorption characteristic of a Voigt profile. Consequently they imprint a component on the power spectrum whose modes in the radial direction are suppressed, leading to a scale-dependent bias. Using mock data sets of known HCD content, we test a model that describes this effect in terms of the distribution of column densities of HCDs, the Fourier transforms of their Voigt profiles and the bias of the halos containing the HCDs. Our results show that this physically well-motivated model describes the effects of HCDs with an accuracy comparable to that of the ad-hoc models used in published forest analyses. We also discuss the problems of applying the model to real data, where the HCD content and their bias is uncertain.
[abstract 34 / 53] (score: 2) - Title: Kinematics of Circumgalactic O VI Gas and Disk Rotation of $z\approx0.2$ Star-forming GalaxiesAuthors: Stephanie H. Ho, Crystal L. Martin, Hasti Nateghi, Glenn G. Kacprzak, Jonathan Stern,Comments: 37 pages with 11 figures; accepted for publication in ApJSubjects: astro-ph.GACreated: 2025-11-09; Updated: 2025-11-11; Datestamp: 2025-11-11
Quasar sightline observations reveal that low-ionization-state gas corotates with the galaxy disk and often at sub-centrifugal velocities, suggesting that the gas is spiraling towards the galaxy disk. However, while observations ubiquitously detect O VI absorption around low-redshift, $\sim L^*$ star-forming galaxies, the relationship between O VI and the galaxy disk, especially the kinematics, is not well-established. This work focuses on the O VI kinematics and its comparison with that of the low ions and galactic disk rotation. We present observations of 18 pairs of QUASARs and $z\approx0.2$ star-forming galaxies. All QUASAR sightlines intersect the circumgalactic medium (CGM) within 45$^\circ$ from the galaxy major axes. We show that while individual O VI velocity components do not correlate with disk rotation, the bulk of O VI gas in individual sightlines rarely counter-rotates. We then match O VI velocity components with those of low ions by minimizing the difference of their velocity centroids. The O VI velocity components with successful low-ion matches are typically found at small sightline impact parameters and are more likely to corotate with the disk. We suggest that the low-ion-matched O VI velocity components trace the gas co-spatial with the low ions near the extended disk plane in the inner CGM, whereas those without low-ion matches represent the gas at large 3D radii. While the gas at large radii is theoretically expected to kinematically correlate with the disk angular momentum, this correlation is expected to be weaker due to the higher turbulent to mean rotation velocity ration at large radii, consistent with our results.
[abstract 35 / 53] (score: 2) - Title: Constraining STAR FORMATION in M87 using deep HST UV dataAuthors: Prathamesh Tamhane, William Waldron, Ming Sun, Silvia Martocchia, Claudia Maraston, Alessandro Boselli, William Forman, Massimo Gaspari, Juhi Tiwari, Megan Donahue, G. Mark Voit, Tim Edge, Grant Tremblay, Daniel Thomas,Comments: 15 pages, 7 figures and 3 tables. Published in ApJ. Added a reference to data products in v2Subjects: astro-ph.GACreated: 2025-11-07; Updated: 2025-11-11; Datestamp: 2025-11-11
We analyzed the deepest Hubble Space Telescope (HST) F275W ultraviolet (UV) imaging of M87 to obtain the most robust constraints on its STAR FORMATION rate (SFR) and STAR FORMATION history (SFH). After removing the galaxy continuum and globular clusters, we detected an excess of UV point sources near the center. By comparing their colors to young stellar source (YSS) colors generated by stochastically simulated STAR FORMATION (SF) for various SFRs and SFHs, we ruled out their origin as a UV-upturn population and identified them as YSS. We found an extremely low SFR of $\sim 2\times10^{-5}$ M$_\odot$ yr$^{-1}$ in M87, with evidence of a weak starburst $\sim$125 Myr ago that formed $\sim 1000$ M$_\odot$ of stars. Unlike other cool-core clusters where SF is stronger and directly linked to cooling gas, we found no spatial correlation between YSS and H$α$ filaments. Comparing SF activity with M87's AGN outburst history suggests that recent AGN feedback events ($\lesssim$12 Myr ago) neither triggered nor were associated with any detectable SF, however, earlier outbursts may have triggered weak starbursts. We detected UV filaments co-spatial with H$α$ filaments with similar lengths and widths, though they are obscured by dust near the center. These filaments are likely powered by metal-line emission from collisional ionization, suggesting ongoing low-level precipitation of the intracluster medium. Our results indicate that AGN feedback has quenched SF significantly in M87 for at least 200 Myr, even though some precipitation persists. Additionally, we identified a hotspot created by the counterJET, with the spectral index also constrained.
[abstract 36 / 53] (score: 2) - Title: A comprehensive search for Long and Short Periodic Features from an Extremely Active Cycle of FRB 20240114AAuthors: Dengke Zhou, Pei Wang, Jianhua Fang, Weiwei Zhu, Bing Zhang, Di Li, Yi Feng, Yong-Feng Huang, Ke-Jia Lee, Jinlin Han, Yuan-Chuan Zou, Jun-Shuo Zhang, Shuo Xiao, Rui Luo, Long-Xuan Zhang, Tian-Cong Wang, Wanjin Lu, Jinhuang Cao, Wenfei Yu, Bing Li, Chen-Chen Miao, Jintao Xie, Yunchuan Chen, Han Wang, Yuanhong Qu, Huaxi Chen, Yuhao Zhu, Shuo Cao, Xiang-Lei Chen, Chen Du, He Gao, Yu-Xiang Huang, Ye Li, Jian Li, Dong-Zi Li, Lin Lin, Xiaohui Liu, Jia-Wei Luo, Jiarui Niu, Chen-Hui Niu, Qingyue Qu, Shiyan Tian, Chao-Wei Tsai, Fayin Wang, Yi-Dan Wang, Wei-Yang Wang, Bojun Wang, Suming Weng, Qin Wu, Zi-Wei Wu, Heng Xu, Aiyuan Yang, Yuan-Pei Yang, Shihan Yew, Yong-Kun Zhang, Lei Zhang, Chunfeng Zhang, Rushuang Zhao, Dejiang Zhou,Comments: The 2nd of papers from the FAST FRB Key Science Project Collaboration on FRB 20240114A: (quasi-) period searchSubjects: astro-ph.HECreated: 2025-11-08; Updated: 2025-11-11; Datestamp: 2025-11-11
Possible periodic features in fast radio bursts (FRBs) may provide insights into their astrophysical origins. Using extensive observations from the Five-hundred-meter Aperture Spherical radio Telescope (FAST), we conduct a multi-timescale periodicity search for the exceptionally active repeater FRB~20240114A. Our analysis is based on different datasets for different timescales: for short-timescale periodicity in Time of Arrivals (TOAs), we use 57 observations from January to August 2024; for long-timescale periodicity, we employ an extended TOA dataset comprising 111 observations spanning from January 2024 to October 2025; and for burst time series analysis, we utilize individual burst data from the 57 FAST observations. We identify three candidate short-timescale periodic signals (0.673~s, 0.635~s, and 0.536~s) with significances of $3.2σ$--$6σ$, each detected in two independent observations. On longer timescales, we detect a significant $143.40\pm7.19$-day periodicity with $5.2σ$ significance, establishing FRB~20240114A as a periodic repeater. In burst time series, we find quasi-periodic oscillations in the few hundred Hz range ($3.4σ$ and $3.7σ$) and periodic burst trains with periods of several to tens of milliseconds ($3σ$--$3.9σ$), though these periodic features appear transient and short-lived. The detection of periodic signals at these different time scales indicates that FRB 20240114A exhibits intriguing periodic self-similar characteristics. Despite the comprehensive dataset, no definitive periodicity linked to the source's rotation is confirmed, placing stringent constraints on the intrinsic source properties and the modulation mechanisms. All data are available via the Science Data Bank.
[abstract 37 / 53] (score: 2) - Title: Enhanced performance in quasi-isodynamic max-$J$ stellarators with a turbulent particle pinchAuthors: G. G. Plunk, A. G. Goodman, P. Xanthopoulos, P. Costello, H. M. Smith, K. Aleynikova, C. D. Beidler, M. Drevlak, P. Helander,Comments:Subjects: physics.plasm-phCreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
Recent stellarator reactor designs demonstrate mostly outward turbulent particle transport, which, without advanced fueling technology, inhibits the formation of density gradients needed for confinement. We introduce ``SQuID-$τ$'', a self-fueling quasi-isodynamic stellarator capable of sustaining density peaking through inward particle transport caused by turbulence. Temperature and density profile predictions based on high-fidelity gyrokinetic simulations demonstrate enhanced performance, significantly relaxing constraints on the size and MAGNETic field strength for reactor designs.
[abstract 38 / 53] (score: 2) - Title: Exciting Stellar Eccentricity in Gaia BH3 via a Hidden Black Hole BinaryAuthors: Qingru Hu, Bin Liu, Wei Zhu,Comments: 10 pages, 6 figures, accepted to ApJLSubjects: astro-ph.HE astro-ph.GA astro-ph.SRCreated: 2025-11-09; Updated: 2025-11-11; Datestamp: 2025-11-11
We propose that the high eccentricity of the stellar orbit in Gaia BH3 system could be excited through a secular resonance effect if the inner dark object is, in effect, a tight and eccentric BLACK HOLE binary (BHB). During the orbital decay of the inner BHB, the apsidal precession rate of the inner binary matches that of the outer stellar orbit, and this resonance advection can drive the outer eccentricity into some extreme values. For a Gaia BH3-like system, we show that a near equal-mass ($q=0.8$) BHB with an initial semi-major axis of 1--3 au and an initial eccentricity $\gtrsim 0.95$ is able to excite the outer orbit to the observed value, leaving a current BHB with semi-major axis 0.25--0.5 au and eccentricity $\sim 0.8$. The eccentric inner BHB imprints two observable signatures on the outer star: (1) short-term RV modulations with an amplitude $\lesssim 100$ m/s and (2) long-term apsidal precession with a rate $\lesssim 0.1^{\circ}$/yr. Although neither of these is detected in the currently available astrometry and RV data, we show that these signals are detectable with the full Gaia astrometry data and dedicated high-precision and/or long-term RV observations. Our work provides a new perspective on the dynamical formation of Gaia BH3, and the methodology is readily applicable to similar systems such as HD 130298, Gaia BH1, and Gaia BH2.
[abstract 39 / 53] (score: 2) - Title: A test of Amati relation using HII galaxy distancesAuthors: Rikiya Okazaki, Shantanu Desai,Comments: 10 pages, 5 figures. Published in UniverseSubjects: astro-ph.HECreated: 2025-11-09; Updated: 2025-11-11; Datestamp: 2025-11-11
We use model-independent luminosity distances of 186 HII galaxy observations to address the circularity problem in the Amati relation for Gamma-ray Bursts (GRBs). For this purpose, we used Artificial Neural Network based interpolation to reconstruct the luminosity distance corresponding to the GRB redshift. We then use two independent GRB datasets to test the robustness of the Amati relation at redshifts below $z=2.6$. Our best-fit Amati relation parameters are consistent for the same datasets to within $1σ$. The intrinsic scatters which we obtain for the two datasets of about 28\% and 35\%, are comparatively larger. This implies that the Amati relation using HII galaxies as distance anchors cannot be used as a probe of precision cosmology.
[abstract 40 / 53] (score: 2) - Title: About maximum energy acquired by a charged particles in the field of a plane electroMAGNETic waveAuthors: V. A. Balakirev, I. N. Onishchenko,Comments:Subjects: physics.acc-phCreated: 2025-11-07; Updated: 2025-11-11; Datestamp: 2025-11-11
The energy characteristics of a RELATIVISTIC charged particle in the field of a plane electroMAGNETic wave of a given amplitude are studied. The dependence of the particle's energy on its phase coordinate is obtained. The maximum value of the particle's energy during acceleration, as well as the acceleration length and time, are determined. The transverse displacement of the particle over the maximum acceleration length is determined.
[abstract 41 / 53] (score: 2) - Title: ALMASOP: Inner-Envelope Structures of Protostars Driving Nascent JetsAuthors: Somnath Dutta, Chin-Fei Lee, Naomi Hirano, Doug Johnstone, Kee-Tae Kim, Yi-Jehng Kuan, James Di Francesco, Kenichi Tatematsu, Mika Juvela, Chang Won Lee, Alessio Traficante, Vivien Huei-Ru Chen, Manash Ranjan Samal, David Eden, Dipen Sahu, Shih-Ying Hsu, Tie Liu, Sheng-Yuan Liu,Comments: 19 pages, 8 Figures. The paper has been accepted for publication in The Astrophysical Journal (ApJ)Subjects: astro-ph.GACreated: 2025-11-08; Updated: 2025-11-11; Datestamp: 2025-11-11
Protostellar JETs provide valuable insight into the evolutionary stage and formation history of star-forming cores in their earliest phases. We investigated the inner envelope structures of three extremely young protostars, selected for having the shortest dynamical timescales in their outflows and JETs. Our analysis is based on Atacama Large Millimeter/submillimeter Array (ALMA) observations of the N2D+, DCO+, DCN, C18O, CH3OH, and H2CO lines, along with 1.3 mm continuum data, obtained at two spatial resolutions of ~500 AU and 150 AU. By examining molecular depletion and sublimation patterns, emission extents at core-scale and outflow rotational temperatures, we assessed the relative evolutionary stages of the three sources. In G208.68-19.20N1, the absence of N2D+ toward the core-despite a semi-ring-like distribution-and the presence of bright DCN and DCO+ emission cospatial with C18O indicate a warmer envelope, possibly suggesting a more advanced evolutionary state. In contrast, G208.68-19.20N3 shows no dense central structures in C18O, DCN, DCO+, or N2D+, with emission instead appearing scattered around the continuum and along large-scale filaments, consistent with a likely younger stage than G208.68-19.20N1. The third source, G215.87-17.62M, exhibits compact C18O emission at the continuum peak, but spatially extended N2D+, DCN, and DCO+ along the continuum, pointing to a cooler envelope and likely the youngest stage among the three. This comparative analysis across three protostars demonstrates the effectiveness of molecular tracers for evolutionary staging, though variations in luminosity or accretion may also shape chemical morphologies. These results highlight the promise of broader surveys for advancing our understanding of early protostellar evolution.
[abstract 42 / 53] (score: 2) - Title: An XMM-Newton View of the ANdromeda Galaxy as Explored in a Legacy Survey (New-ANGELS) II: Luminosity Function of X-ray SourcesAuthors: Rui Huang, Jiang-Tao Li, Wei Cui, Zhijie Qu, Joel N. Bregman, Xiang-Dong Li, Gabriele Ponti, Q. Daniel Wang,Comments: 25 pages, 17 figuresSubjects: astro-ph.GA astro-ph.HECreated: 2025-11-08; Updated: 2025-11-11; Datestamp: 2025-11-11
As part of the New-ANGELS program, we systematically investigate the X-ray luminosity functions (XLFs) of 4506 X-ray sources projected within a radius of 2.5 deg centering on M31. We construct XLFs for different regions in the disk and halo of M31, accounting for the incompleteness with an effective sensitivity map. Assuming that the halo regions contain (mostly) foreground stars and background ACTIVE GALACTIC NUCLEi, they are taken as "background" for deriving the XLFs of the sources in the disk. Through modeling XLFs, we decompose the X-ray sources into distinct populations for each region. We find that low-mass X-ray binaries are the dominant X-ray population throughout the disk of M31. The XLFs of M31 reveal a consistently lower integrated LMXB luminosity per stellar mass ($α_\mathrm{LMXB}$) compared to other galaxies, likely due to M31's prolonged period of quiescent STAR FORMATION. Variations in the XLF shape and $α_\mathrm{LMXB}$ across different regions of M31 suggest that the relationship between integrated luminosity and stellar mass may vary within the galaxy. Additionally, the relatively low integrated luminosity observed in the inner-arm region provides crucial evidence for a rapid fading of M31's LMXBs around 1 Gyr, a finding consistent with recent observations of other nearby galaxies.
[abstract 43 / 53] (score: 2) - Title: A Universal Framework for Horizon-Scale Tests of Gravity with Black Hole ShadowsAuthors: Wentao Liu, Yang Liu, Di Wu, Yu-Xiao Liu,Comments: 8 pages, 8 figuresSubjects: gr-qcCreated: 2025-11-08; Updated: 2025-11-11; Datestamp: 2025-11-11
In this Letter, we have developed a numerically efficient framework for evaluating parameters in metric theories of gravity, and applied it to constrain the horizon-scale MAGNETic field in the Kerr-Bertotti-Robinson (Kerr-BR) spacetime using the latest EHT observations. The method's adaptive ray-tracing strategy achieves near-linear computational efficiency without loss of numerical accuracy. Owing to this efficiency, the framework enables high precision shadow modeling at minimal computational cost and, for the first time, supports statistically robust inference of BLACK HOLE parameters from horizon-scale observations for arbitrary stationary BLACK HOLEs. The above framework is applied to the recently obtained Kerr-BR BLACK HOLE, an exact MAGNETized and rotating solution to the Einstein field equations. We have evaluated the horizon-scale MAGNETic fields of M87* and Sgr A*, with the latter showing a field strength of $93.3^{+14.7}_{-23.8}G$, consistent with the equipartition estimate of $71G$ from polarized ALMA observations, thereby supporting Einstein's gravity.
[abstract 44 / 53] (score: 2) - Title: AthenaK Simulations of Magnetized Binary Neutron Star MergersAuthors: Jacob Fields, David Radice,Comments: 9 pages, 3 figures, submitted to ASTRONUM-2025 proceedingsSubjects: astro-ph.HE gr-qcCreated: 2025-11-08; Updated: 2025-11-11; Datestamp: 2025-11-11
We present new numerical-relativity simulations of a MAGNETized binary neutron star merger performed with AthenaK. The simulations employ a temperature- and composition-dependent tabulated nuclear equation of state, with initially dipolar fields with a maximum initial strength of ${\sim}10^{16}\ {\rm G}$ which extend outside the stars. We employ adaptive mesh refinement and consider three grid resolutions, with grid spacing down to $Δx_{\rm min} \simeq 92\ {\rm m}$ in the most refined region. When comparing the two highest resolution simulations, we find orbital dephasing of over 7 orbits until merger of only $0.06$ radians. The MAGNETic field is amplified during the merger and we observe the formation of a MAGNETized funnel in the polar region of the remnant. Simulations are continued until about $30$ milliseconds after merger. However, due to significant baryonic pollution, the binary fails to produce a MAGNETically-dominated outflow. Finally, we discuss possible numerical and physical effects that might alter this outcome.
[abstract 45 / 53] (score: 2) - Title: The extended inner shadow of Kerr-Taub-NUT BLACK HOLE with thin disk flowsAuthors: Yu-Yan Wang, Meng-Die Zhao, Xin-Yu Wang, Guo-Ping Li,Comments: 28 pages; 34 figures; 1 tableSubjects: gr-qcCreated: 2025-11-09; Updated: 2025-11-11; Datestamp: 2025-11-11
In this paper, we apply numerical backward ray-tracing to study the observational appearance of Kerr-Taub-NUT (KTN) BLACK HOLEs illuminated by thin accretion disk flows. We obtained the inner shadow, redshift characteristics, and intensity distribution of thin-disk images of the KTN BLACK HOLE, as observed by a common observer located at different positions. The results show that increasing the spin parameter progressively deforms the critical curve into a "D" shape while simultaneously shrinking and distorting the inner shadow. More importantly, for n = 0.3 at theta_o = 80 degrees, the inner shadow develops a novel "duck-cap-like" morphology with a sharply protruding lower-right edge beyond the critical curve. We term this feature the "extended inner shadow", a structure distinct from the Kerr case. Unlike the standard inner shadow, it consists partly of photons absorbed by the horizon and partly of photons that avoid both absorption and crossing the disk plane, thus receiving no emission. Such deviations from Kerr predictions could be tested by future high-precision astronomical observations, potentially offering new evidence for the existence of NUT charge (or the gravitoMAGNETic monopole) in BLACK HOLEs.
[abstract 46 / 53] (score: 2) - Title: MeerKAT observations of the spiral galaxy NGC 2997 in the S band. Detection of high dynamo modesAuthors: A. Damas-Segovia, R. Beck, S. A. Mao, A. Basu, S. Sridhar, E. Barr, A. Brunthaler, S. Buchner, F. Camilo, W. Cotton, A. M. Jacob, C. Kasemann, H. -R. Klöckner, M. Kramer, I. Rammala-Zitha, S. Ranchod, M. R. Rugel, O. Smirnov, J. D. Wagenveld, G. Wieching, O. Wucknitz,Comments:Subjects: astro-ph.GACreated: 2025-11-09; Updated: 2025-11-11; Datestamp: 2025-11-11
We seek to exploit the expanded observational range of the MeerKAT radio telescope with the new S-band receivers (2.0-2.8 GHz). To showcase its enhanced capabilities, we conducted new S-band observations of the galaxy NGC 2997 in full POLARIZATION. The S band is ideal for studying MAGNETic fields in spiral galaxies due to the weak Faraday dePOLARIZATION. Performing a rotation measure (RM) synthesis allowed us to measure Faraday RMs in the galaxy, a signature of regular MAGNETic fields. A fast Fourier transform (FFT) algorithm was used to study the various azimuthal modes found in the RM data of the galaxy. The RM synthesis analysis indicates the direction of the MAGNETic field along the line of sight throughout the entire disk. Leveraging the sensitivity and high resolution provided by MeerKAT's S-band capability, this study achieves an unprecedented level of detail of the MAGNETic field structure. Our sector-based analysis of the RMs across azimuthal regions reveals the existence of modes of the large-scale MAGNETic field in NGC 2997. The variations in the RM values along the azimuthal angle reveal smoothly changing phase shifts between the rings, without the previously reported field reversal at about 3 kpc radius between the central region and disk. In this work, for the first time, a Fourier analysis has been applied to RM data averaged in sectors of rings in the disk plane of a spiral galaxy. Our Fourier analysis of the RM map shows three different large-scale field modes detected in the disk of NGC 2997. After applying a geometric modification, even multiples of the first mode were detected, as predicted from theoretical studies of dynamo action in a spiral galaxy with symmetric spiral structure. Our new method opens up new possibilities for investigating MAGNETic fields in spiral galaxies.
[abstract 47 / 53] (score: 2) - Title: Conceptual design of Thomson scattering system with high wavelength resolution in MAGNETically confined plasmas for electron phase-space measurementsAuthors: Kentaro Sakai, Kentaro Tomita, Takeo Hoshi, Akito Nakano, Motoshi Goto, Kenichi Nagaoka, Ryo Yasuhara,Comments: 13 pages, 11 figures, 1 tableSubjects: physics.plasm-phCreated: 2025-11-09; Updated: 2025-11-11; Datestamp: 2025-11-11
We discuss the conceptual design of a spatially-resolved spectroscopy system of Thomson scattering with high wavelength resolution capable of measuring the shape of electron velocity distribution functions in MAGNETically confined plasmas. We design a spatially-resolved spectrometer with 2560 wavelength channels. The estimated number of scattered photons in a single spectrometer channel is much larger than unity under the setup and plasma parameters at the Compact Helical Device (CHD), indicating that the shape of scattered spectra can be directly observed. We calculate the synthetic spectra with various plasma parameters and electron velocity distribution functions. The signal-to-noise ratio and accuracy of the estimated parameter are examined using the synthetic spectra assuming Maxwellian electron velocity distribution functions. We also discuss the feasibility of detecting non-Maxwellian electron velocity distribution functions with the high wavelength resolution spectrometer.
[abstract 48 / 53] (score: 2) - Title: Total solar eclipse 2024 modelling with COCONUTAuthors: Tinatin Baratashvili, Haopeng Wang, Daria Sorokina, Andrea Lani, Stefaan Poedts,Comments: 11 pages, 9 figuresSubjects: astro-ph.SRCreated: 2025-11-09; Updated: 2025-11-11; Datestamp: 2025-11-11
Coronal modelling is crucial for a better understanding of solar and helio-physics. Due to the strong brightness of the Sun and the lack of white light observations of the solar atmosphere and low corona (1-1.5R$_\odot$), total solar eclipses have become a standard approach for validating the coronal models. In this study, we validate the COCONUT coronal model by predicting the coronal configuration during the total solar eclipse on April 8, 2024. We aim to predict the accurate configuration of the solar corona during the total solar eclipse on April 8, 2024. We utilise the full 3D MHD model to reconstruct the solar corona from the solar surface to $30\;R_\odot$. The upcoming total solar eclipse predictions were conducted in three different regimes: quasi-steady driving of the inner boundary conditions (BCs) with a daily cadence and dynamic driving of the inner BCs with both daily and hourly cadences. The results from all the simulations are compared to the total solar eclipse images. Additionally, the synthetic white-light (WL) images are generated from the STEREO-A field of view and compared to COR2 observed images. Normalised polarised brightness is compared in the COR2 and synthetic WL images. The predicted solar corona does not vary significantly in the first half of the prediction window. The dynamic simulations yielded better results than the quasi-steady predictions. The west limb was reconstructed better in the simulations than the east limb. We have predicted the total solar eclipse coronal configuration 18 days before the total solar eclipse. We can conclude that the dynamic simulations produced more accurate predictions. The availability of comprehensive observations is crucial, as the emergence of the active region on the east limb made it difficult to accurately predict the east limb coronal configuration due to incorrect input of MAGNETic field data.
[abstract 49 / 53] (score: 2) - Title: Implication of multiple source populations of Galactic COSMIC RAYs from proton and helium spectraAuthors: Qiang Yuan,Comments: 7 pages, 5 figures, 3 tablesSubjects: astro-ph.HECreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
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.
[abstract 50 / 53] (score: 2) - Title: Reduced kinetic model for ion temperature gradient instability in tokamaks with reversed MAGNETic shearAuthors: B. Jia, Q. Zhong, Y. Li, Y. Xiao,Comments:Subjects: physics.plasm-phCreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
Using the averaged MAGNETic drift model and a first-order finite Larmor radius (FLR) expansion, the eigenvalue equation for the ion temperature gradient (ITG) mode in tokamak plasmas is reduced to a Schrödinger-type differential equation. By invoking generalized translational invariance, the model is extended to reversed MAGNETic shear (RMS) configurations and benchmarked against global gyrokinetic simulations from GTC, showing good quantitative agreement. The analysis reveals a characteristic double-well potential unique to RMS profiles, which gives rise to the degeneracy between the lowest-order even and first-order odd eigenmodes when the two potential wells are sufficiently separated radially. The ITG instability is also found to resonate with the MAGNETic drift frequency, and its maximum growth occurs when the two rational surfaces are slightly separated. These results provide new physical insight into ITG mode behavior under reversed MAGNETic shear and offer a compact, accurate theoretical framework that bridges simplified analytic models and global simulations.
[abstract 51 / 53] (score: 2) - Title: Probing spectral line asymmetries due to the propagating transverse waves in the solar coronaAuthors: Ambika Saxena, Vaibhav Pant, Tom Van Doorsselaere, M. Saleem Khan,Comments: Accepted for the publication in ApJSubjects: astro-ph.SRCreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
Decades-long studies of asymmetric spectral lines in the solar corona suggest mass and energy transport from lower atmospheric layers to the corona. While slow MAGNEToacoustic waves and plasma flows are recognized as drivers of these spectral line asymmetries, the role of transverse MHD waves remains largely unexplored. Previous simulations have shown that unidirectionally propagating kink waves, in the presence of perpendicular density inhomogeneities, can produce a turbulence-like phenomenon called ``uniturbulence''. However, the spectroscopic signatures of this effect have not been investigated until now. Due to varying Doppler shifts from the plasma elements with different emissions, we expect to observe signatures of both blueward and redward asymmetries. Past instruments like EIS may have missed these signatures due to resolution limitations, but current instruments like DKIST offer a better opportunity for detection. We conducted 3D MHD simulations of transverse waves in a polar plume with density inhomogeneities and performed forward modeling for the Fe XIII emission line at 10749 Å. Our findings show that transverse waves and uniturbulence induce alternating red and blueward asymmetries, with magnitudes reaching up to 20\% of peak intensity and secondary peak velocities between 30 and 40 km s$^{-1}$, remaining under 100 km s$^{-1}$. These asymmetries propagate with the transverse waves, and even at DKIST resolution, similar signatures can be detected. Our study suggests that spectral line asymmetries can serve as a diagnostic tool for detecting transverse wave-induced uniturbulence.
[abstract 52 / 53] (score: 2) - Title: Identifying the physical periods in the radio emission from the $γ$-ray emitting binary LS I +61 303Authors: Frédéric Jaron, Valentí Bosch-Ramon,Comments: 13 pages, 10 Figures, 1 Table, accepted for publication in Astronomy & AstrophysicsSubjects: astro-ph.HECreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
The $γ$-ray emitting binary LS I +61 303 exhibits periodic emission across the electroMAGNETic spectrum, from radio up to the very-high-energy regime. The most prominent features are the three periods $P_1 = 26.5$ d, $P_2 = 26.9$ d, and $P_{\rm long} = 4.6$ years. Occasionally, a fourth period of 26.7 d is also detected. Mathematically, these four periods are interrelated via the interference pattern of a beating. Competing scenarios that seek to determine which of these periods are physical and which are secondary are under debate. The detection of a fifth period, $P_3 = 26.3$ d, was recently claimed. Our aim is to determine which of these periods are intrinsic (likely related to physical processes) and which of these are secondary (resulting from interference). We avoided any assumption about the physical scenario and restricted our analysis to the phenomenology of the radio emission variability. We selected intervals from archival radio data and applied the generalized Lomb-Scargle periodogram. We fit the observational data to generate synthetic data that only contain specific signals. We analyzed these synthetic data to assess the impact of these signals and their interference on the light curves and the periodogram. The two-peaked profile, consisting of $P_1$ and $P_2$, was detected in the periodogram of the actual data for intervals that are significantly shorter than $P_{\rm long}$, provided that these intervals contain a minimum of the long-term modulation. The characteristics of the observational data and their periodogram could only be reproduced with synthetic data if these explicitly included all three periods $P_1$, $P_2$, and $P_{\rm long}$, the residuals being limited by noise. We have found that all three periods, i.e., $P_1$, $P_2$, and $P_{\rm long}$, could correspond to physically real processes occurring in LS I +61 303.
[abstract 53 / 53] (score: 2) - Title: Design and operation of APEX-LD: a compact levitated dipole for the confinement of electron-positron pair plasmasAuthors: A. Card, M. R. Stoneking, A. Deller, E. V. Stenson,Comments: 11 pages, 12 figuresSubjects: physics.plasm-phCreated: 2025-11-10; Updated: 2025-11-11; Datestamp: 2025-11-11
The objective of the APEX (A Positron-Electron eXperiment) project is to MAGNETically confine and study electron--positron pair plasmas. For this purpose, a levitated dipole trap (APEX-LD) has been constructed. The MAGNETically levitated, compact (7.5-cm radius), closed-loop, high-temperature superconducting (HTS) floating (F-)coil consists exclusively of a No-Insulation (NI) Rare-earth Barium Copper Oxide (ReBCO) winding pack, solder-potted in a gold-plated-copper case. A resealable in-vacuum cryostat facilitates cooling (via helium gas) and inductive charging of the F-coil. The 70-minute preparation cycle reliably generates persistent currents of ~60 kA-turns and an axial MAGNETic flux density of B_0 ~ 0.5 T. We demonstrate levitation times in excess of three hours with a vertical stability of sigma_z < 20 um. Despite being subjected to routine quenches (and occasional mechanical shocks), the F-coil has proven remarkably robust. We present the results of preliminary experiments with electrons, and outline the next steps for injecting positron bunches into the device.
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