Current date: 2026-07-27
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Datestamp limit: 2026-07-27 (0 days ago)
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Scoring abstracts
Number of records retrieved: 585
Keyword score statistics
score 12 -- 1 abstracts
score 10 -- 1 abstracts
score 9 -- 1 abstracts
score 8 -- 1 abstracts
score 7 -- 1 abstracts
score 5 -- 3 abstracts
score 4 -- 4 abstracts
score 3 -- 6 abstracts
score 2 -- 15 abstracts
in total -- 33 abstracts
Articles that appeared on 2026-07-27
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[abstract 1 / 33] Wow! (score: 12)
- Title: Comparison of Polarized Radiative Transfer Codes used by the EHT CollaborationAuthors: Cora Prather, Jason Dexter, Monika Moscibrodzka, Hung-Yi Pu, Thomas Bronzwaer, Jordy Davelaar, Ziri Younsi, Charles F. Gammie, Roman Gold, George N. Wong, Kazunori Akiyama, Antxon Alberdi, Walter Alef, Juan Carlos Algaba, Richard Anantua, Keiichi Asada, Rebecca Azulay, Uwe Bach, Anne-Kathrin Baczko, David Ball, Mislav Baloković, John Barrett, Michi Bauböck, Bradford A. Benson, Dan Bintley, Lindy Blackburn, Raymond Blundell, Katherine L. Bouman, Geoffrey C. Bower, Hope Boyce, Michael Bremer, Christiaan D. Brinkerink, Roger Brissenden, Silke Britzen, Avery E. Broderick, Dominique Broguiere, Sandra Bustamante, Do-Young Byun, John E. Carlstrom, Chiara Ceccobello, Andrew Chael, Chi-kwan Chan, Dominic O. Chang, Koushik Chatterjee, Shami Chatterjee, Ming-Tang Chen, Yongjun Chen, Xiaopeng Cheng, Ilje Cho, Pierre Christian, Nicholas S. Conroy, John E. Conway, James M. Cordes, Thomas M. Crawford, Geoffrey B. Crew, Alejandro Cruz-Osorio, Yuzhu Cui, Mariafelicia De Laurentis, Roger Deane, Jessica Dempsey, Gregory Desvignes, Vedant Dhruv, Sheperd S. Doeleman, Sean Dougal, Sergio A. Dzib, Ralph P. Eatough, Razieh Emami, Heino Falcke, Joseph Farah, Vincent L. Fish, Ed Fomalont, H. Alyson Ford, Raquel Fraga-Encinas, William T. Freeman, Per Friberg, Christian M. Fromm, Antonio Fuentes, Peter Galison, Roberto García, Olivier Gentaz, Boris Georgiev, Ciriaco Goddi, Arturo I. Gómez-Ruiz, José L. Gómez, Minfeng Gu, Mark Gurwell, Kazuhiro Hada, Daryl Haggard, Kari Haworth, Michael H. Hecht, Ronald Hesper, Dirk Heumann, Luis C. Ho, Paul Ho, Mareki Honma, Chih-Wei L. Huang, Lei Huang, David H. Hughes, Shiro Ikeda, C. M. Violette Impellizzeri, Makoto Inoue, Sara Issaoun, David J. James, Buell T. Jannuzi, Michael Janssen, Britton Jeter, Wu Jiang, Alejandra Jiménez-Rosales, Michael D. Johnson, Svetlana Jorstad, Abhishek V. Joshi, Taehyun Jung, Mansour Karami, Ramesh Karuppusamy, Tomohisa Kawashima, Garrett K. Keating, Mark Kettenis, Dong-Jin Kim, Jae-Young Kim, Jongsoo Kim, Junhan Kim, Motoki Kino, Jun Yi Koay, Prashant Kocherlakota, Yutaro Kofuji, Shoko Koyama, Carsten Kramer, Michael Kramer, Thomas P. Krichbaum, Cheng-Yu Kuo, Noemi La Bella, Tod R. Lauer, Daeyoung Lee, Sang-Sung Lee, Po Kin Leung, Aviad Levis, Zhiyuan Li, Rocco Lico, Greg Lindahl, Michael Lindqvist, Mikhail Lisakov, Jun Liu, Kuo Liu, Elisabetta Liuzzo, Wen-Ping Lo, Andrei P. Lobanov, Laurent Loinard, Colin J. Lonsdale, Ru-Sen Lu, Nicholas R. MacDonald, Jirong Mao, Nicola Marchili, Sera Markoff, Daniel P. Marrone, Alan P. Marscher, Iván Martí-Vidal, Satoki Matsushita, Lynn D. Matthews, Lia Medeiros, Karl M. Menten, Daniel Michalik, Izumi Mizuno, Yosuke Mizuno, James M. Moran, Kotaro Moriyama, Cornelia Müller, Alejandro Mus, Gibwa Musoke, Ioannis Myserlis, Andrew Nadolski, Hiroshi Nagai, Neil M. Nagar, Masanori Nakamura, Ramesh Narayan, Gopal Narayanan, Iniyan Natarajan, Antonios Nathanail, Santiago Navarro Fuentes, Joey Neilsen, Roberto Neri, Chunchong Ni, Aristeidis Noutsos, Michael A. Nowak, Junghwan Oh, Hiroki Okino, Héctor Olivares, Gisela N. Ortiz-León, Tomoaki Oyama, Feryal Özel, Daniel C. M. Palumbo, Georgios Filippos Paraschos, Jongho Park, Harriet Parsons, Nimesh Patel, Ue-Li Pen, Dominic W. Pesce, Vincent Piétu, Richard Plambeck, Aleksandar PopStefanija, Oliver Porth, Felix M. Pötzl, Jorge A. Preciado-López, Dimitrios Psaltis, Venkatessh Ramakrishnan, Ramprasad Rao, Mark G. Rawlings, Alexander W. Raymond, Luciano Rezzolla, Angelo Ricarte, Bart Ripperda, Freek Roelofs, Alan Rogers, Eduardo Ros, Cristina Romero-Cañizales, Arash Roshanineshat, Helge Rottmann, Alan L. Roy, Ignacio Ruiz, Chet Ruszczyk, Kazi L. J. Rygl, Salvador Sánchez, David Sánchez-Argüelles, Miguel Sánchez-Portal, Mahito Sasada, Kaushik Satapathy, Tuomas Savolainen, F. Peter Schloerb, Jonathan Schonfeld, Karl-Friedrich Schuster, Lijing Shao, Zhiqiang Shen, Des Small, Bong Won Sohn, Jason SooHoo, Kamal Souccar, He Sun, Fumie Tazaki, Alexandra J. Tetarenko, Paul Tiede, Remo P. J. Tilanus, Michael Titus, Pablo Torne, Efthalia Traianou, Tyler Trent, Sascha Trippe, Matthew Turk, Ilse van Bemmel, Huib Jan van Langevelde, Daniel R. van Rossum, Jesse Vos, Jan Wagner, Derek Ward-Thompson, John Wardle, Jonathan Weintroub, Norbert Wex, Robert Wharton, Maciek Wielgus, Kaj Wiik, Gunther Witzel, Michael F. Wondrak, Qingwen Wu, Paul Yamaguchi, Aristomenis Yfantis, Doosoo Yoon, André Young, Ken Young, Wei Yu, Feng Yuan, Ye-Fei Yuan, J. Anton Zensus, Shuo Zhang, Guang-Yao Zhao, Shan-Shan Zhao,Comments: Accepted for publication in ApJSubjects: astro-ph.HECreated: 2026-07-23; Updated: 2026-07-27; Datestamp: 2026-07-27
Interpretation of resolved polarized images of BLACK HOLEs by the Event Horizon Telescope (EHT) requires predictions of the polarized emission observable by an Earth-based instrument for a particular model of the BLACK HOLE accretion system. Such predictions are generated by general RELATIVISTIC radiative transfer (GRRT) codes, which integrate the equations of polarized radiative transfer in curved spacetime. A selection of ray-tracing GRRT codes used within the EHT collaboration is evaluated for accuracy and consistency in producing a selection of test images, demonstrating that the various methods and implementations of radiative transfer calculations are highly consistent. When imaging an analytic accretion model, we find that all codes produce images similar within a pixel-wise normalized mean squared error (NMSE) of 0.012 in the worst case. When imaging a snapshot from a cell-based MAGNETohydrodynamic simulation, we find all test images to be similar within NMSEs of 0.02, 0.04, 0.04, and 0.12 in Stokes I, Q, U , and V respectively. We additionally find the values of several image metrics relevant to published EHT results to be in agreement to much better precision than measurement uncertainties.
[abstract 2 / 33] Wow! (score: 10) - Title: Winds Versus Jets in Active Galactic NucleiAuthors: David Garofalo, Chandra B. Singh, Atticus Magerko, Marco Botello, Sophia Soto, Max North,Comments: 17 pages, 3 figures, 2 tables, Accepted for publication in the Galaxies journalSubjects: astro-ph.HE astro-ph.GACreated: 2026-07-24; Updated: 2026-07-27; Datestamp: 2026-07-27
The well-established anti-correlation between disk winds and RELATIVISTIC JETs in X-ray binaries is often interpreted in a scale-invariant BLACK HOLE accretion context. If so, ACTIVE GALACTIC NUCLEi (AGN) should exhibit a direct mass-scaled analog. We test this prediction across FRII radio QUASARs, radio-quiet QUASARs, and JETted and non-JETted Narrow Line Seyfert 1 galaxies (NLS1) in spirals, among others. They exclude simple scale invariance. The highest-velocity winds occur exclusively in radio-quiet QUASARs, while powerful FRII QUASARs host systematically weaker winds despite equally large BLACK HOLE masses. Jetted NLS1s show strong wind suppression consistent with X-ray binary behavior, whereas FRII QUASARs occupy a distinct regime in which JETs and winds coexist. Black hole mass and spin magnitude alone cannot account for this dichotomy. We argue that the angular momentum direction of the disk relative to that of the BLACK HOLE (aligned versus anti-aligned or co-rotation versus counter-rotation) is the critical parameter: secularly fueled spiral systems and most post-merger systems favor co-rotation, which is associated with compact ISCO radii, high radiative efficiency, strong winds, and JET suppression, while the counter-rotating subset of merger-influenced ellipticals can sustain powerful JETs alongside moderate winds. Moreover, while spiral AGN and merger-driven radio-quiet QUASARs experience similar strong JET/wind anti-correlation, they cannot be treated as strict scaled analogs of X-ray binaries, which undergo rapid state transitions involving MAGNETic flux redistribution absent in AGN. At least two distinct wind-JET regimes therefore operate across the mass scale. We identify the details of this behavior across AGN subclasses.
[abstract 3 / 33] Wow! (score: 9) - Title: Radio Core Size of Low-luminosity Active Galactic Nuclei under the MAD-JET modelAuthors: Yue Xu, Fu-Guo Xie,Comments: 14 pages, 10 figures, 1 table. To appear in ApJSubjects: astro-ph.HE astro-ph.GACreated: 2026-07-24; Updated: 2026-07-27; Datestamp: 2026-07-27
After decades of efforts, there are now fruitful high-resolution radio observations of low-luminosity ACTIVE GALACTIC NUCLEi (LLAGNs), and the observed frequency has extended from $\sim$10 GHz up to $\sim$200 GHz. In this work, based on a model that combines a MAGNETically arrested disk (MAD) and a Blandford-Znajek-like JET, we carried out detailed analysis on size and location of the radio core of LLAGNs. The radio core size of nearby LLAGN M104 is re-visited based on this new model. We successfully reproduce a $size\proptoν^{-1}$ scaling between 1 GHz and tens of GHz, if more than $50\%$ of electrons in JET follow a power-law (PL) distribution. We further confirm that, at high radio frequencies emission from MAD exceeds that from JET, and a flatter size-frequency slope is observed. The impact of PL electrons in MAD is also investigated. For those $L_{\rm bol}/L_{\rm Edd} \gtrsim (3-8)\times 10^{-6}$ LLAGNs and BLACK HOLE binaries in their hard state, PL electrons are expected to be highly suppressed due to strong radiative cooling (so-called `SYNCHROTRON boiler' effect).
[abstract 4 / 33] Wow! (score: 8) - Title: Observation of Wobbling and Precessing Jet Signatures in Gamma-Ray Emission from Blazar PKS 1424-41Authors: Ajay Sharma, Debanjan Bose,Comments: 13 pages and 9 Figures The manuscript under review in The Astrophysical JournalSubjects: astro-ph.HECreated: 2026-07-24; Updated: 2026-07-27; Datestamp: 2026-07-27
We report a clear observational evidence for JET precession and nutation manifested in the gamma-ray emissions of the BLAZAR PKS 1424$-$41. An analysis of $\sim$16 yr of \emph{FERMI}-LAT observations reveals three distinct and superimposed quasi-periodic oscillations (QPOs), with characteristic timescales of $\sim$5.26 yr, $\sim$0.96 yr and $\sim$1.3 yr. The longer timescale is detected with a local significance of $\sim 4.1σ$ ($99.9958\%$ confidence) and a global significance of $\sim 2.45σ$ ($98.5714\%$ confidence). The shorter timescales ($\sim 0.96$ yr and $\sim 1.3$ yr) both show local significances exceeding $3σ$. To interpret the origin of these modulations, we examine two physically motivated scenarios: Lense-Thirring precession of a misaligned accretion disk and orbital-driven JET precession in a binary supermassive BLACK HOLE (BSBH) system. We model the gamma-ray variability using a compound framework that incorporates JET precession together with intrinsic JET rotation (nutation), which successfully reproduces the observed year-like QPOs. Our results indicate that the long-term, persistent $\sim$5.26 yr oscillation is most consistent with a BSBH origin, while the shorter year-like QPO modulation can be naturally attributed to rotation or wobbling of the JET axis. If PKS 1424$-$41 hosts a supermassive BLACK HOLE binary, it represents a promising target for future space-borne gravitational-wave observatories such as the Laser Interferometer Space Antenna (LISA), providing an independent probe of supermassive BLACK HOLE binaries.
[abstract 5 / 33] Wow! (score: 7) - Title: Iharm3D: Vectorized General Relativistic MagnetohydrodynamicsAuthors: Cora Prather, George N. Wong, Vedant Dhruv, Benjamin R. Ryan, Joshua C. Dolence, Sean M. Ressler, Charles F. Gammie,Comments: 4 pages, 2 figures. Associated code at https://github.com/AFD-Illinois/iharm3dSubjects: astro-ph.HE astro-ph.IM physics.plasm-phCreated: 2026-07-23; Updated: 2026-07-27; Datestamp: 2026-07-27
Iharm3D is an open-source C code for simulating BLACK HOLE accretion systems in arbitrary stationary spacetimes using ideal general-RELATIVISTIC MAGNETohydrodynamics (GRMHD). It is an implementation of the HARM ("High Accuracy Relativistic Magnetohydrodynamics") algorithm outlined in Gammie et al. (2003) with updates as outlined in McKinney & Gammie (2004) and Noble et al. (2006). The code is most directly derived from Ryan et al. (2015) but with radiative transfer portions removed. HARM is a conservative finite-volume scheme for solving the equations of ideal GRMHD, a hyperbolic system of partial differential equations, on a logically Cartesian mesh in arbitrary coordinates.
[abstract 6 / 33] Yes (score: 5) - Title: Searches for Binary Mergers with Sub-solar Mass Components in Data from the First Part of LIGO--Virgo--KAGRA's Fourth Observing RunAuthors: The LIGO Scientific Collaboration, the Virgo Collaboration, the KAGRA Collaboration, A. G. Abac, I. Abouelfettouh, F. Acernese, K. Ackley, A. Adam, 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, E. Alberici, L. Albers, 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, C. Anand, A. Ananyeva, S. B. Anderson, W. G. Anderson, M. Andia, M. Ando, M. Andrés-Carcasona, J. L. Andrey, T. Andrić, J. Anglin, J. Anna, S. Ansoldi, J. M. Antelis, S. Antier, M. Aoumi, E. Z. Appavuravther, S. Appert, S. K. Apple, K. Arai, A. Araya, M. C. Araya, M. Arca Sedda, F. Arciprete, J. S. Areeda, N. Aritomi, F. Armato, S. Armstrong, N. Arnaud, M. Arogeti, S. M. Aronson, 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, K. A. Baker, T. Baker, G. Balbi, 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, K. Baric, B. C. Barish, D. Barker, N. Barman, P. Barneo, F. Barone, B. Barr, M. Barrios, L. Barsotti, M. Barsuglia, D. Barta, 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, C. Bellani, L. Bellizzi, D. Beltran-Martinez, W. Benoit, I. Bentara, M. Ben Yaala, S. Bera, F. Bergamin, B. K. Berger, S. Bernuzzi, M. Beroiz, C. P. L. Berry, I. Berry, D. Bersanetti, T. Bertheas, A. Bertolini, J. Betzwieser, D. Beveridge, G. Bevilacqua, N. Bevins, R. Bhandare, R. Bhatt, A. Bhattacharjee, D. Bhattacharjee, S. Bhattacharyya, S. Bhaumik, V. Biancalana, A. Bianchi, F. 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, P. Bogdan, G. Boileau, M. Boldrini, G. N. Bolingbroke, A. Bolliand, L. D. Bonavena, R. Bondarescu, F. Bondu, V. A. Bonhomme, E. Bonilla, M. S. Bonilla, A. Bonino, R. Bonnand, A. Borchers, N. Borghi, V. Boschi, S. Bose, V. Bossilkov, Y. Bothra, A. Boudon, M. Boyle, A. Bozzi, C. Bradaschia, M. J. Brady, P. R. Brady, A. Branch, M. Branchesi, 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, R. Cabrita, V. Cáceres-Barbosa, L. Cadonati, G. Cagnoli, C. Cahillane, A. Calafat, T. A. Callister, E. Calloni, S. R. Callos, G. Caneva Santoro, K. C. Cannon, H. Cao, L. A. Capistran, E. Capocasa, G. Capoccia, E. Capote, G. Capurri, G. Carapella, F. Carbognani, K. J. Cardona-Martínez, 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. Caudill, M. Cavaglià, R. Cavalieri, G. Cella, S. Cepic, P. Cerdá-Durán, E. Cesarini, N. Chabbra, W. Chaibi, A. Chakraborty, P. Chakraborty, S. Chakraborty, S. Chalathadka Subrahmanya, R. Chalmers, C. Chan, J. C. L. Chan, M. Chan, K. Chang, P. Charlton, E. Chassande-Mottin, C. Chatterjee, Debarati Chatterjee, Deep Chatterjee, M. Chaturvedi, S. Chaty, A. Chen, A. H. -Y. Chen, D. Chen, H. Chen, H. Y. Chen, S. Chen, Y. Chen, G. Cheng, H. P. Cheng, P. Chessa, T. Cheunchitra, H. T. Cheung, S. Y. Cheung, F. Chiadini, G. Chiarini, A. Chiba, A. Chincarini, D. Chintala, 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, S. M. Clyne, E. Coccia, E. Codazzo, P. -F. Cohadon, D. E. Cohen, S. Colace, E. Colangeli, O. Cole, 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, L. A. Corubolo, L. Cotnoir, R. Cottingham, M. W. Coughlin, P. Couvares, D. M. Coward, D. C. Coyne, R. Coyne, A. Cozzumbo, J. D. E. Creighton, T. D. Creighton, 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. Dall'Osso, S. Dal Pra, G. Dálya, O. Dan, Y. Dang, B. D'Angelo, S. Danilishin, S. D'Antonio, K. Danzmann, K. E. Darroch, L. P. Dartez, R. Das, A. Dasgupta, V. Dattilo, A. Daumas, 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, C. J. Delgado Mendez, F. De Lillo, S. Della Torre, W. Del Pozzo, O. M. del Rio, 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, V. Deshmukh, R. De Simone, S. Determan, A. Dhani, R. Dhurkunde, R. Diab, C. Diaz, M. C. Díaz, 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, F. Dosopoulou, W. J. D. Doyle, M. Drago, J. C. Driggers, M. Dubois, R. R. Dumbreck, L. Dunn, U. Dupletsa, D. D'Urso, P. Dutta Roy, H. Duval, P. -A. Duverne, S. E. Dwyer, C. Eassa, M. Eberhardt, M. Ebersold, T. Eckhardt, G. Eddolls, A. Effler, J. Eichholz, H. Einsle, M. Eisenmann, R. A. Eisenstein, 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, X. Fan, A. M. Farah, B. Farr, W. M. Farr, M. Favata, M. Fays, M. Fazio, J. Feicht, M. M. Fejer, J. Feldhusen, E. Fenyvesi, J. Fernandes, T. Fernandes, D. Fernando, S. Ferraiuolo, T. A. Ferreira, M. Ferrer, F. Fidecaro, P. Figura, A. Fiori, I. Fiori, M. Fishbach, 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, P. W. F. Forsyth, K. Franceschetti, A. Franco-Ordovas, F. Frappez, S. Frasca, F. Frasconi, A. Frattale Mascioli, J. P. Freed, Z. Frei, A. Freise, O. Freitas, R. Frey, W. Frischhertz, P. Fritschel, V. V. Frolov, 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, A. Ganguly, B. Garaventa, P. García Abia, J. García-Bellido, C. García-Quirós, J. W. 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, Archisman Ghosh, 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, G. González, P. Goodarzi, S. Goode, A. Goodwin-Jones, M. Gosselin, C. Gostiaux, R. Gouaty, D. W. Gould, K. Govorkova, A. Grado, A. E. Granados, M. Granata, V. Granata, S. Gras, P. Grassia, C. Gray, R. Gray, G. Greco, A. C. Green, L. Green, S. M. Green, S. R. Green, A. M. Gretarsson, E. M. Gretarsson, H. K. Griffin, D. Griffith, H. L. Griggs, G. Grignani, C. Grimaud, H. Grote, S. Grunewald, D. Guerra, A. G. Guerrero, D. Guetta, G. M. Guidi, T. Guidry, H. K. Gulati, F. Gulminelli, A. M. Gunny, 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, R. Hamburg, E. Z. Hamilton, G. Hammond, M. Haney, J. Hanks, C. Hanna, M. D. Hannam, O. A. Hannuksela, H. Hansen, J. Hanson, R. Harada, A. R. Hardison, S. Harikumar, K. Haris, I. Harley-Trochimczyk, T. Harmark, J. Harms, G. M. Harry, I. W. Harry, J. Hart, M. T. Hartman, B. Haskell, C. J. Haster, K. Haughian, H. Hayakawa, K. Hayama, A. Heffernan, D. Hegde, M. C. Heintze, J. Heinze, J. Heinzel, H. Heitmann, F. Hellman, A. F. Helmling-Cornell, G. Hemming, O. 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Vardaro, A. F. Vargas, V. Varma, A. Vecchio, G. Vedovato, J. Veitch, P. J. Veitch, S. Venikoudis, J. Venneberg, R. C. Venterea, P. Verdier, M. Vereecken, D. Verkindt, B. Verma, Y. Verma, S. M. Vermeulen, F. Vetrano, A. Veutro, A. Viceré, S. Vidyant, A. D. Viets, A. Vijaykumar, A. Vilkha, N. Villanueva Espinosa, V. Villa-Ortega, E. T. Vincent, J. -Y. Vinet, S. Viret, S. Vitale, A. Vives, L. Vizmeg, H. Vocca, D. Voigt, E. R. G. von Reis, J. S. A. von Wrangel, W. E. Vossius, L. Vujeva, S. P. Vyatchanin, J. Wack, L. E. Wade, M. Wade, K. J. Wagner, L. Wallace, E. J. Wang, H. Wang, W. H. Wang, Y. F. Wang, Z. Wang, G. Waratkar, J. Warner, M. Was, T. Washimi, N. Y. Washington, D. Watarai, B. Weaver, S. A. Webster, N. L. Weickhardt, M. Weinert, A. J. Weinstein, R. Weiss, L. Wen, K. Wette, C. Wheeler, J. T. Whelan, B. F. Whiting, E. G. Wickens, D. Wilken, B. M. Williams, D. Williams, M. J. Williams, N. S. Williams, J. L. Willis, B. Willke, M. Wils, L. Wilson, C. W. Winborn, J. Winterflood, C. C. Wipf, G. Woan, J. Woehler, N. E. Wolfe, H. T. Wong, I. C. F. Wong, K. Wong, T. Wouters, J. L. Wright, M. Wright, B. Wu, C. Wu, D. S. Wu, H. Wu, K. Wu, Q. Wu, Z. Wu, E. Wuchner, D. M. Wysocki, V. A. Xu, Y. Xu, N. Yadav, H. Yamamoto, K. Yamamoto, T. S. Yamamoto, T. Yamamoto, R. Yamazaki, T. Yan, H. Yang, K. Z. Yang, Y. Yang, Z. Yarbrough, J. Yebana, S. -W. Yeh, A. B. Yelikar, X. Yin, J. Yokoyama, T. Yokozawa, S. Yuan, H. Yuzurihara, M. Zanolin, M. Zeeshan, T. Zelenova, J. -P. Zendri, M. Zeoli, M. Zerrad, M. Zevin, H. Zhang, L. Zhang, N. Zhang, R. Zhang, T. Zhang, C. Zhao, Yue Zhao, Yuhang Zhao, Z. -C. Zhao, Y. Zheng, H. Zhong, H. Zhou, H. O. Zhu, Z. -H. Zhu, Z. Zhu, A. B. Zimmerman, L. Zimmermann, M. E. Zucker, J. Black, S. Shandera, D. Jeong,Comments:Subjects: astro-ph.HE astro-ph.COCreated: 2026-07-23; Updated: 2026-07-27; Datestamp: 2026-07-27
We report on a gravitational wave search for compact binary coalescences involving at least one component with mass between $0.2\,M_\odot$ to $1\,M_\odot$, and ratio of component masses between 0.1 and 1. The analysis uses data collected by the LIGO detectors between May 24 2023 15:00 UTC and January 16 2024 16:00 UTC. No statistically significant sub-solar mass candidates were identified by the participating search algorithms. We report the detection sensitivity of the current searches to the target sub-solar mass BLACK HOLE population. With the absence of detections, we place upper limits on the merger rate of sub-solar mass BLACK HOLEs, ranging from 110 ${\rm Gpc^{-3}\,yr^{-1}}$ to 10000 ${\rm Gpc^{-3}\,yr^{-1}}$ at 90\% confidence. We constrain two illustrative DARK MATTER scenarios that can form sub-solar mass compact objects with these searches: primordial BLACK HOLEs, and dark BLACK HOLEs forming in a dissipative DARK MATTER model. For late-forming primordial BLACK HOLE binaries, our search excludes the fraction of DARK MATTER in primordial BLACK HOLEs to be $\leq 1$ only for masses above $0.9\,M_\odot$. In the early-formation scenario, we limit this fraction to be $\leq 7\%$ at $1\,M_\odot$, and $\leq 40\%a$ at $0.35\,M_\odot$. For the dissipative model, the excluded region in the parameter space of DARK MATTER fraction in dark BLACK HOLEs and their minimum possible mass extends down to (0.9 to 1.2) $\times 10^{-5}$ at $1\,M_\odot$ with no constraints below $0.02\,M_\odot$. For the first time, we report the detection sensitivity of our searches to binaries with sub-solar mass neutron stars, and place the 90\% confidence merger rate limit at (570 to 710) ${\rm Gpc^{-3}\,yr^{-1}}$ for a population with component masses distributed uniformly down to $0.5\,M_\odot$.
[abstract 7 / 33] Yes (score: 5) - Title: Viscosity effects on the shadow of a non-rotating BLACK HOLEAuthors: Sayantani Lahiri, Sergio Gimeno-Soler, Alejandro Cruz-Osorio, José A. Font, Ziri Younsi,Comments: 12 pages, 7 figuresSubjects: gr-qc astro-ph.HECreated: 2026-07-23; Updated: 2026-07-27; Datestamp: 2026-07-27
We study the effect of shear viscosity in stationary MAGNETized accretion tori on synthetic images of non-rotating BLACK HOLE shadows. Shear viscosity and spacetime-curvature contributions are introduced perturbatively in the tori through first and second-order transport coefficients within a second-order causal theory of non-ideal RELATIVISTIC hydrodynamics. Synthetic BLACK HOLE shadow images at 230\,GHz are obtained via general RELATIVISTIC radiative transfer computations assuming thermal SYNCHROTRON emission and for a wide range of plasma MAGNETization parameters, viewing inclination angles, electron-temperature prescriptions, and viscosity parameters. A comparative pixel-by-pixel analysis using two normalized metrics shows that the largest image differences occur for strongly MAGNETized tori. While shear viscosity induces only minor changes in the overall shadow morphology, its combined effects with spacetime curvature are more evident in localized modifications of the SYNCHROTRON emission and pixel-wise flux distribution. These effects become increasingly pronounced at higher inclination angles, with the largest brightness differences between viscous and non-viscous configurations occurring for larger values of the electron-temperature parameter. Overall, our results indicate that shear viscosity and spacetime curvature leave only modest imprints on BLACK HOLE shadow images produced by stationary thick disks, with differences remaining at the level of a few $μ$Jy. Since our analysis is limited to stationary tori, the effects of shear viscosity might however be more significant in fully dynamical accretion systems.
[abstract 8 / 33] Yes (score: 5) - Title: A GRMHD-Calibrated Semi-Analytical Model for Hot Sub-Keplerian Accretion Flows in Kerr SpacetimeAuthors: Nabin Bhushal, Manil Khatiwada, Yogesh Maharjan, David Garofalo, Chandra B. Singh,Comments: 20 pages, 9 Figures, 8 tablesSubjects: astro-ph.HE astro-ph.GACreated: 2026-07-23; Updated: 2026-07-27; Datestamp: 2026-07-27
We develop a simple, semi-analytical, kinematic model for hot, thick accretion flows, constructed by interpolating between Keplerian and free-fall geodesic solutions in the Kerr metric. Unlike self-consistent general RELATIVISTIC MAGNETohydrodynamics (GRMHD) frameworks, our model contains no explicit MAGNETic fields or stress terms; instead, it uses a smooth, radially varying transition function T(r) to connect the velocity components from near-Keplerian rotation at large distances to a free-fall state near the event horizon. While the coefficients $α$ and $β$ remain constant, the transition function is a true function of radius, allowing the flow properties to vary smoothly with radius. We calibrate and validate this model against time- and azimuthally averaged profiles from long-duration MAGNETically arrested disk (MAD) simulations spanning a wide range of BLACK HOLE spins ($a=-0.9$ to $+0.9$). The model successfully captures the properties of accretion flow parameters across both prograde and retrograde configurations. Quantitatively, the predicted radial velocity, angular velocity, and density profiles match the simulation data to within an average factor of approximately 1.8, 1.6, and 1.6, respectively, while the specific angular momentum exhibits the closest agreement, remaining within a factor of approximately 1.2. This fast semi-analytical prescription gives significantly lower errors than previous constant-coefficient models and it is a computationally affordable tool for various applications such as ray tracing, accretion parameter exploration, and spectral modelling.
[abstract 9 / 33] Yes (score: 4) - Title: KHARMA: Flexible, Portable Performance for GRMHDAuthors: Cora Prather,Comments: Chapter submitted to "New Frontiers in GRMHD Simulations of Accreting Black Holes," Springer Nature Singapore, ed. Cosimo Bambi, Yosuke Mizuno, Swarnim Shashank and Feng Yuan. Document released under LA-UR-23-23232Subjects: astro-ph.HECreated: 2026-07-23; Updated: 2026-07-27; Datestamp: 2026-07-27
KHARMA (an acronym for "Kokkos-based High-Accuracy Relativistic Magnetohydrodynamics with Adaptive mesh refinement") is a new open-source code for conducting general-RELATIVISTIC MAGNETohydrodynamic simulations in stationary spacetimes, primarily of accretion systems. It implements among other options the High-Accuracy Relativistic Magnetohydrodynamics (HARM) scheme, but is written from scratch in C++ with the Kokkos programming model in order to run efficiently on both CPUs and GPUs. In addition to being fast, KHARMA is written to be readable, modular, and extensible, separating functionality into "packages," representing, e.g., algorithmic components or physics extensions. Components of the core ideal GRMHD scheme can be swapped at runtime, and additional packages are included to simulate electron temperature evolution, viscous hydrodynamics, and for designing chained multi-scale "bridged" simulations. This chapter presents the computational environment and requirements for KHARMA, features and design which meet these requirements, and finally, validation and performance data.
[abstract 10 / 33] Yes (score: 4) - Title: Reconnection-induced electron energization in MAGNETospheric Kelvin-Helmholtz dynamicsAuthors: Silvia Ferro, Fabio Bacchini, Giuseppe Arrò, Francesco Pucci, Pierre Henri,Comments: Submitted to ApJLSubjects: physics.plasm-ph physics.space-phCreated: 2026-07-24; Updated: 2026-07-27; Datestamp: 2026-07-27
The Kelvin-Helmholtz instability (KHI) is a major driver of multiscale plasma dynamics at velocity shear layers, where it can promote the formation of current sheets and the onset of MAGNETic RECONNECTion as well as drive plasma energization. While recent kinetic studies have shown efficient electron heating during nonlinear KH evolution, the connection between RECONNECTion dynamics and localized electron energization is still not fully understood. We investigate this link using two-dimensional fully kinetic simulations of KHI developing in a double-periodic system with two velocity shear layers and a uniform guide field, initialized from a finite-Larmor-radius equilibrium. During the nonlinear stage, initially coherent vortices evolve into layers populated by fragmented current sheets containing active MAGNETic RECONNECTion sites. The global energetics reveal distinct species-dependent energization pathways. Ions act as the primary energy reservoir, transferring energy to the electroMAGNETic fields, while electrons receive the dominant net positive energy input. Electron energization is strongly anisotropic ($T_{\parallel,e} > T_{\perp,e}$) and localized within intermittent RECONNECTing current sheets associated with enhanced field-particle energy exchange and elevated agyrotropy. These regions also show the development of suprathermal tails in the electron energy distributions, providing evidence for nonthermal electron energization. Despite opposite vorticity orientations, the two shear layers exhibit similar statistical behavior. Together, these results establish a direct connection between RECONNECTion-associated current structures and localized electron energization in collisionless KHI dynamics.
[abstract 11 / 33] Yes (score: 4) - Title: On the astrophysical origin of COSMIC RAYs: Constraining the Ultra-High-Energy Cosmic Ray Horizon through Nearby Galaxy DistributionsAuthors: F. Dávila-Kurbán, F. Duplancic, D. Garcia Lambas,Comments: 18 pages, 10 figures, submitted to Physical Review D after referee reviewSubjects: astro-ph.HE astro-ph.CO astro-ph.GACreated: 2026-07-23; Updated: 2026-07-27; Datestamp: 2026-07-27
The origin of ultra-high-energy COSMIC RAYs (UHECR) remains a central open problem in astroparticle physics. The observed large-scale anisotropy of UHECR arrival directions above several EeV, together with the spectral suppression at the highest energies, suggests extragalactic sources confined to a limited volume of the nearby Universe, though the effective spatial scale of this contribution remains poorly constrained. We aim to constrain the effective propagation horizon of UHECR with energies E >= 8 EeV by studying how well the observed large-scale anisotropy is reproduced by the distribution of nearby galaxies at different distances, accounting for Galactic MAGNETic-field deflections. We construct volume-limited galaxy samples from the GLADE+ catalogue extending to 10000 km/s (~150 Mpc) and use both dipole comparisons and angular cross-correlation analyses with the Pierre Auger Observatory UHECR flux map (E >= 8 EeV) to characterize the distance dependence of the anisotropy signal, further weighting the galaxy-UHECR correlations using deflection maps derived from a Galactic MAGNETic field model. We find that the angular separation between the galaxy and UHECR dipoles is minimized for galaxies within cz < 4000 km/s (< 60 Mpc), where the galaxy dipole amplitude is also maximal. The galaxy-UHECR cross-correlation signal is dominated by this nearby population and weakens rapidly at larger distances. Accounting for Galactic MAGNETic field deflections enhances the correlation amplitude by more than a factor of two, indicating that MAGNETic effects significantly shape the observed anisotropy. Our results indicate that the observed anisotropy of UHECR of 8 EeV and above is primarily driven by sources within ~50-60 Mpc, consistent with expectations from energy losses and MAGNETic deflections, retaining a measurable imprint of the nearby extragalactic matter distribution.
[abstract 12 / 33] Yes (score: 4) - Title: Where Do Quasars Live? DESI DR1 Constraints from PAC MeasurementsAuthors: Shanquan Gui, Kun Xu, Donghai Zhao,Comments: 10 pages, 10 figures, 1 table. Submitted to A&ASubjects: astro-ph.GACreated: 2026-07-23; Updated: 2026-07-27; Datestamp: 2026-07-27
Quasar environments connect the growth of supermassive BLACK HOLEs, ACTIVE GALACTIC NUCLEus feedback, and galaxy evolution. Small-scale QUASAR clustering probes the one-halo regime and can test whether QUASAR activity depends on central--satellite status. We seek to obtain precise small-scale measurements of QUASAR environments at $0.8
[abstract 13 / 33] (score: 3) - Title: The failed failed-SUPERNOVA scenario of M31-2014-DS1Authors: Noam Soker,Comments: Published in the Open Journal of AstrophysicsSubjects: astro-ph.HECreated: 2026-07-23; Updated: 2026-07-27; Datestamp: 2026-07-27
I examine a recently proposed failed-SUPERNOVA scenario for the fading of the yellow supergiant event M31-2014-DS1, and find that it requires unlikely fine-tuned parameters to work, if at all. In the failed-SUPERNOVA scenario, most of the yellow supergiant collapsed to form a BLACK HOLE. Due to the energy carried by neutrinos from the cooling, collapsing core, gravity decreases, leading to the ejection of a small fraction of the outer envelope, some of which remains bound. The fallback accreted gas possesses large angular-momentum fluctuations due to the pre-collapse envelope convection. The fallback material forms intermittent accretion disks around the BLACK HOLE that launch JETs (or disk wind), which unbind most of the bound material. The failed-SUPERNOVA scenario for M31-2014-DS1 requires that only <1% of the bound material be accreted by the BLACK HOLE, but the JETs do not shut down the backflow for over 10 years. I find this fine-tuned requirement unlikely. I also find that, due to the rapid radiative cooling of the outflow interaction zone with the outer gas, the expected radiation is about an order of magnitude or more above the observed value. These, as well as earlier challenges raised against the failed-SUPERNOVA scenario, make the alternative type II intermediate-luminosity optical transient scenario, in which fading is due to dust ejection in a violent binary interaction, more likely. The fading event M31-2014-DS1 does not support the failed-SUPERNOVA scenario predicted by the neutrino-driven explosion mechanism of core-collapse SUPERNOVAe.
[abstract 14 / 33] (score: 3) - Title: Infrared Echoes of Precessing Tidal Disruption EventsAuthors: Hong-Zhou Wu, Shao-Yu Fu, Wen-Long Xu, Chang Zhou, Wei-Hua Lei,Comments: 16 pages,7 figures,accepted by ApJSubjects: astro-ph.HECreated: 2026-07-24; Updated: 2026-07-27; Datestamp: 2026-07-27
A tidal disruption event (TDE) occurs when a star is torn apart by a supermassive BLACK HOLE. The resulting UV/optical flare irradiates parsec-scale dust, producing delayed mid-infrared echoes that persist for years. These echoes provide unique calorimetric probes of the total radiated energy and dust geometry.Existing models usually assume static axisymmetric illumination patterns. However, the TDE accretion disk is likely misaligned and undergoes RELATIVISTIC precession.In this work, we present a theoretical framework for infrared dust echoes from a precessing TDE disk. The precession will lead to highly variable infrared light curves, which can be revealed by high-cadence observations. The overall profile of the infrared light curves shows double-peaked to single-peaked pattern transitions as a result of the changes in the viewing angle or precession angle.The results indicate that infrared echoes are dynamic tracers of the evolving lighting patterns of the central engine.
[abstract 15 / 33] (score: 3) - Title: Outflows in super-Eddington QUASARs drive clumpy circumgalactic medium and extended H$α$ nebulae at $z \gtrsim 6$Authors: Lucas Tortora, Tiago Costa, Debora Sijacki, Jake S. Bennett,Comments: 26 pages, 15 figures, submitted to MNRASSubjects: astro-ph.GACreated: 2026-07-23; Updated: 2026-07-27; Datestamp: 2026-07-27
The discovery of gargantuan BLACK HOLEs with masses exceeding a billion solar masses at $z\gtrsim6$ suggests rapid BLACK HOLE growth and significant energy input into their host galaxies in the early Universe. With JWST probing previously unseen phases of the interstellar (ISM) and circumgalactic (CGM) medium around $z > 6$ QUASARs, detailed theoretical studies can now be directly confronted with observations. We use zoom-in simulations of a massive protocluster at $z\sim6$, employing both the fiducial FABLE galaxy formation model and modifications that allow earlier BLACK HOLE seeding and mildly super-Eddington accretion. The central QUASAR remains Compton-thick throughout most of its evolution, with the obscuration arising from the ISM of its compact host galaxy. The onset of sufficiently strong QUASAR feedback drives a 'blow-out' episode, clearing out escape channels for ionizing radiation and leaving the central engine unobscured. This leads to a complete transformation of the CGM, whereby powerful, metal-enriched outflows produce a population of cold, fast, neutral clumps, significantly increasing the covering fraction of neutral hydrogen in the host halo. Radiative transfer calculations performed with a new ray-tracing code show that the CGM responds to QUASAR activity through the formation of H$α$ nebulae, whose size and luminosity increase with the strength of QUASAR feedback and decrease with obscuration level. Enhanced early BLACK HOLE growth thus fundamentally reshapes the ISM and CGM of $z\sim6$ QUASARs, leaving clear observable signatures in their obscuration, neutral hydrogen distribution, and extended H$α$ emission.
[abstract 16 / 33] (score: 3) - Title: JWST/MIRI Reveals the Evolution from Molecular to Atomic Disk WindsAuthors: Naman S. Bajaj, Ilaria Pascucci, Sylvie Cabrit, Suzan Edwards, Gabriele Cugno, Andrew D. Sellek, Joan R. Najita, Ke Zhang, Richard Alexander, Gregory J. Herczeg, Uma Gorti, Sophie C. Clark, Tracy L. Beck,Comments: Accepted for publication in the Astronomical Journal (AJ, AAS)Subjects: astro-ph.EPCreated: 2026-07-23; Updated: 2026-07-27; Datestamp: 2026-07-27
The evolution and dispersal of protoplanetary disks--governed by accretion, MAGNETically launched JETs and winds, and photoevaporative winds--fundamentally shape planetary systems. Determining how these mass-loss processes co-evolve is crucial for constraining planet formation pathways. We analyze archival JWST/MIRI/IFU data of 72 inclined (i>40deg) mostly ClassII disks to identify and characterize spatially resolved JETs and winds, focusing on [NeII] and H2 lines. Extended emission in H2 S(1), S(3), S(5), S(7) and/or [NeII] is detected toward 66 disks, revealing diverse morphologies. We develop a framework to identify conical H2 winds and high-velocity [NeII] JETs perpendicular to the disk, detecting them toward 46 and 40 disks, respectively. All sources with [NeII] JETs exhibit a corresponding wind traced in either H2 (85%) or [OI], establishing a connection between JETs and winds. The detection fractions of [NeII]-JETs and H2-winds correlate positively with mass accretion rate, with no dependence on disk inclination or stellar mass. Conversely, marginally resolved low-velocity [NeII] winds are found preferentially toward lower accretors. Among sources with H2 winds, detection of hotter winds traced by S(7) and S(5) declines more rapidly with decreasing accretion rate than the colder S(1) component. Comparison with high-resolution [OI]6300\textÅ spectroscopy reveals [OI] LVC and extended H2 wind detections preferentially toward moderate-to-high accretors (>~10^{-8.5}~Msun/yr), whereas lower accretors exhibit only [OI] and [NeII] winds. Together, these results indicate that atomic JETs and atomic+molecular winds, consistent with an MHD disk-wind origin, dominate during early, actively accreting disk phases, while at lower accretion rates, JETs weaken and winds become predominantly atomic.
[abstract 17 / 33] (score: 3) - Title: Stacked Reverberation Mapping of High Redshift Quasars in DESI. I. Feasibility AnalysisAuthors: Rahma Alfarsy, R. E. A. Canning, Eva-Maria Mueller, Jessica Aguilar, Steven Ahlen, David Alexander, Davide Bianchi, David Brooks, Peter Clark, Todd Claybaugh, Andrei Cuceu, Tamara Davis, Axel de la Macorra, Saisrinivas Dhavala, Victoria A. Fawcett, Benjamin Floyd, Andreu Font-Ribera, Jaime Forero-Romero, Enrique Gaztañaga, Wei-Jian Guo, Gaston Gutierrez, Klaus Honscheid, Richard Joyce, Stephanie Juneau, David Kirkby, Theodore Kisner, Anthony Kremin, Claire Lamman, Martin Landriau, Laurent Le Guillou, Paul Martini, Hugh McDougall, Aaron Meisner, Ramon Miquel, John Moustakas, Seshadri Nadathur, Nathalie Palanque-Delabrouille, Zhiwei Pan, Swayamtrupta Panda, Ignasi Pérez-Ràfols, Francisco Prada, Ragadeepika Pucha, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Tom Shanks, Małgorzata Siudek, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Hu Zou,Comments: 28 pages, 29 figures, Accepted by MNRASSubjects: astro-ph.GACreated: 2026-07-23; Updated: 2026-07-27; Datestamp: 2026-07-27
The broad line region of QUASARs has long been probed by reverberation mapping techniques that measure time lags between continuum and broad emission line variations. Stacked reverberation mapping has been proposed as a less observationally expensive alternative to traditional methods. This ensemble approach also reduces biases from small-number statistics. The Dark Energy Spectroscopic Instrument (DESI) is conducting the most extensive spectroscopic survey of QUASARs to date. We create mock light curves emulating expected DESI QUASAR observations at redshifts $1.48
[abstract 18 / 33] (score: 3) - Title: A post-hypercritical accretion small-scale dynamo in newborn neutron starsAuthors: David F. Bambague, Cristian G. Bernal, J. A. Rueda,Comments:Subjects: astro-ph.HECreated: 2026-07-24; Updated: 2026-07-27; Datestamp: 2026-07-27
Hypercritical fallback accretion can advect the surface MAGNETic field of a newborn neutron star into the newly accreted outer layers. Before this material joins the solid crust and enters the Hall-Ohmic regime, part of it may remain hot, dense, and liquid, allowing turbulent MAGNETic amplification. We investigate whether a small-scale dynamo (SSD) can operate under these conditions using six local 3D resistive MHD simulations performed with FLASH 4.7 in a periodic domain with externally forced subsonic turbulence. We explore MAGNETic Reynolds numbers from about 700 to 3700 and examine the effects of the equation of state, neutrino cooling, and numerical resolution. The MAGNETic field grows exponentially from an initial strength of 1e12 G and saturates at about (3-7)e13 G within milliseconds. The saturated MAGNETic energy remains below equipartition, with MAGNETic-to-kinetic energy ratios of about 0.2-0.3, consistent with SSD behavior for MAGNETic Prandtl number near unity. The reference simulations at 128^3 and 256^3 resolution agree within a few percent. Neutrino cooling has little effect over the simulated times, while the equation of state only weakly modifies the dynamo properties. These results indicate that a local SSD can efficiently amplify MAGNETic fields in the liquid post-hypercritical accretion layer and support scenarios for MAGNETic field reemergence in newborn neutron stars.
[abstract 19 / 33] (score: 2) - Title: On local and non-local energy transfers in Hall MAGNETohydrodynamic turbulenceAuthors: Arijit Halder, Supratik Banerjee, Pablo D. Mininni, Manohar K. Sharma,Comments: 22 pages, 11 figuresSubjects: physics.plasm-ph physics.flu-dynCreated: 2026-07-23; Updated: 2026-07-27; Datestamp: 2026-07-27
A systematic study of inertial energy cascade in three-dimensional incompressible Hall MAGNETohydrodynamic turbulence is conducted to probe into the locality of energy conserving triads and the subsequent transfers. Based on the nature of triadic conservations, the energy transfer due to the Hall term is further decomposed into two channels BB and JB corresponding to the terms $d_i ({\bf j}\cdot\nabla){\bf b}$ and $ d_i ({\bf b}\cdot\nabla){\bf j}$, respectively (Halder et al., 2023; Banerjee and Halder,2024). Here ${\bf b}$ and ${\bf j}$ represent the MAGNETic field and the current in Alfvén units, whereas $d_i$ is the ion inertial scale. Using direct numerical simulations, we calculate the shell-to-shell energy transfer rates corresponding to both the channels, and convincingly show each of them to comprise a combination of local and non-local energy transfers. A local inverse transfer is consistently observed at all scales of the channel BB whereas for the channel JB, the local exchange of energy is associated with a gradual increase in strength as the scale is decreased, together with a transition from inverse to direct transfer across the Hall wavenumber, characterized by the ion inertial length $d_i$. Calculating mediator-specific transfer rates, we also conclude that a considerable amount of the local energy transfer is mediated by the non-local triads, especially at small scales of the channel JB. The observed results can be explained using the power-law behaviour of the modal fields. The present study captures the intricate dynamics of energy transfer due to the Hall term and hence can be used to develop more insightful analytical models (shell models, for example) for Hall MAGNETohydrodynamic cascade. The framework can be extended to segregate the local and the nonlocal heating in various turbulent flows including ferrofluids, binary fluids, etc.
[abstract 20 / 33] (score: 2) - Title: Revisiting PBH accretion, evaporation and their cosmological consequencesAuthors: Jitumani Kalita, Debaprasad Maity,Comments: 38 pages, 14 figures, published in JCAPSubjects: astro-ph.HE astro-ph.CO gr-qc hep-thCreated: 2026-07-24; Updated: 2026-07-27; Datestamp: 2026-07-27
Primordial BLACK HOLEs (PBHs) provide a unique probe of the early Universe. Their cosmological evolution is governed by the competition between mass accretion and Hawking evaporation. In this paper we look into the details impact of accretion. Most of the earlier analysis relied on non-RELATIVISTIC accretion models. In this work, we reinvestigate this in a fully RELATIVISTIC framework for Kerr PBHs in the radiation-dominated era. We derive RELATIVISTIC accretion rate and compute spin-dependent efficiency $λ_{\text{Kerr}}(a_*)$. Using this result, we construct coupled evolution equations for the PBH mass and spin that include both RELATIVISTIC accretion and spin-dependent evaporation. Our analysis shows that RELATIVISTIC accretion significantly increases PBH masses and consequently suppresses their spins, causing all PBHs to become effectively Schwarzschild well before evaporation. These effects strengthen the Big Bang Nucleosynthesis (BBN) bound on the initial PBH mass by a factor of $\sim 4$--$5$, reduce the mass required for survival to the present epoch to $\sim 2.7\times 10^{14}\,\mathrm{g}$, and shift the viable particle like DM parameter space. Notably the early accretion induced spin-down effect further washes out the well known high-frequency, spin-induced feature in the high frequency stochastic gravitational-wave background, modifying predictions for future detectors.
[abstract 21 / 33] (score: 2) - Title: Gravitational instability in partially ionized plasmas: A two-fluid approachAuthors: A. P. Misra, V. Krishan,Comments: 8 pages, 2 figures; Revised throughout the text, Figure 1 added, and typos rectifiedSubjects: physics.plasm-ph astro-ph.SRCreated: 2026-07-24; Updated: 2026-07-27; Datestamp: 2026-07-27
We propose a new two-fluid model for a partially ionized MAGNEToplasma under gravity, in which electrons and neutrals are treated as a single fluid, while singly charged positive ions are a separate fluid. We observe that the classical result of gravitational instability (also known as Rayleigh-Taylor instability) in fully ionized plasmas becomes significantly modified by the influence of ion-neutral collisions (with frequency $ν_{\rm{in}}$) and transverse wave numbers ($k_x$ and $k_y$). The instability growth rate can be enhanced or decreased depending on the values of the ratios $κ\equiv k_x/k_y$ and $f\equivν_{\rm{in}}/Ω_{\rm{ci}}$, where $Ω_{\rm{ci}}$ is the ion-cyclotron frequency. We also estimate the growth rates relevant to the ionospheric E-region and solar atmosphere, noting that such growth rates can have a maximum for $κ,~f\ll1$, or for $κ>1$ and $f\sim0.64$, and minimized for $f\gg1$ irrespective of the value of $κ$. Furthermore, the timescale of instability ranges from $1$ minute to $2$ minutes in the solar atmosphere, while in the E region, it ranges from $1$ minute to $80$ minutes. The latter can be a satisfactory result for the reported lifetime of solar prominence threads.
[abstract 22 / 33] (score: 2) - Title: Fingerprints of Individual Supermassive Black Hole Binaries in Pulsar Timing ArraysAuthors: Chiara M. F. Mingarelli, Bjorn Larsen, Ellis Eisenberg, Qinyuan Zheng, Forrest Hutchison,Comments: 14 pages, 4 appendices, 6 figures. SubmittedSubjects: astro-ph.HECreated: 2026-07-23; Updated: 2026-07-27; Datestamp: 2026-07-27
With evidence for a nanoHertz gravitational-wave background now established by Pulsar Timing Arrays, the search focuses on identifying individual supermassive BLACK HOLE binaries. We show that these binaries produce a distinct spatial correlation pattern across the array, acting as a deterministic analogue to the stochastic Hellings \& Downs curve. We derive a closed analytic expression for this single-source overlap reduction function, $Υ_{ab}$, factorizing the signal into a source-dependent amplitude and a purely geometric fingerprint. Using simulated datasets, we demonstrate that this fingerprint breaks the degeneracy between an individual binary and a stochastic background. Including these cross-correlations yields Bayes factors of $1611$ favoring the continuous-wave model over a Hellings \& Downs correlated background model and $159$ favoring the continuous-wave model over an uncorrelated red-noise model. Furthermore, these new cross-correlations improve sky localization by a factor of $11\times$ over an uncorrelated search. Finally, while coherent matched filtering offers higher theoretical sensitivity, we argue that a cross-correlation-based search for individual binaries provides a robust alternative that hedges against the possibility of overfitting to noise fluctuations by focusing on the evidence for the correlations. Indeed, the geometric fingerprints we present here show that spatial correlations can also be used to identify the first nanoHertz gravitational-wave sources.
[abstract 23 / 33] (score: 2) - Title: Thermodynamics of Kerr-Bertotti-Robinson BLACK HOLEAuthors: Li Hu, Rong-Gen Cai, Shao-Jiang Wang,Comments: v1, 7 pages, no figure; v2, version accepted for publication in Physical Review D as a LetterSubjects: gr-qcCreated: 2026-07-24; Updated: 2026-07-27; Datestamp: 2026-07-27
We investigate the thermodynamic properties of the Kerr-Bertotti-Robinson BLACK HOLE, an exact Petrov type D solution of Einstein-Maxwell theory describing a rotating BLACK HOLE immersed in an external electroMAGNETic field. While the conserved angular momentum and electric charge can be computed straightforwardly, the conserved mass cannot be obtained through standard integrability methods due to the nontrivial asymptotically uniform external electroMAGNETic field. To overcome this difficulty, we adopt the Christodoulou-Ruffini mass relation as a thermodynamic definition of the conserved mass, and identify the associated generator, thereby fixing the ambiguity in defining this conserved mass and constructing the thermodynamic potentials. These thermodynamic quantities naturally satisfy the first law of black-hole thermodynamics as well as the Smarr formula.
[abstract 24 / 33] (score: 2) - Title: Extending asteroseismic MAGNETometry across the diverse landscape of MAGNETic structuresAuthors: Nicholas Z. Rui, J. M. Joel Ong, Armand Leclerc, Daniel Lecoanet, Lisa Bugnet, Janosz W. Dewberry, Bastien Liagre, Stéphane Mathis,Comments: 20 pages, 11+2 figures, accepted to MNRAS. Animated figures included in an associated Zenodo upload: https://zenodo.org/records/20561425Subjects: astro-ph.SRCreated: 2026-07-24; Updated: 2026-07-27; Datestamp: 2026-07-27
Magnetic fields have now been asteroseismically measured in the cores of many red giants. However, most interpretations of these measurements assume that the MAGNETic field is far below the critical field strength known to be exceeded by red giants exhibiting gravity-mode suppression. A recent method based on the traditional approximation of rotation and MAGNETism accurately predicts mode frequencies under fields up to this critical value by modeling gravity waves as individual MAGNETogravity ``POLARIZATIONs'' which propagate through a waveguide-like mode cavity. So far, this formalism has been limited to MAGNETic fields which are axisymmetric about the rotation axis. In this study, we extend this approach by calculating the POLARIZATIONs of MAGNETogravity waves under arbitrarily shaped MAGNETic fields under potentially rapid rotation. We consider the special cases of a dipolar MAGNETic field misaligned with the rotation axis as well as a dipole-plus-quadrupole MAGNETic field with no rotational symmetry. We show that non-axisymmetric field configurations can induce avoided crossings between POLARIZATIONs, and that waves in such systems can convert between MAGNETogravity POLARIZATIONs as they propagate, especially when the MAGNETic field strength is locally below a stratification-dependent threshold value. This threshold is distinct from the critical field strength for gravity-mode suppression, and is instead similar to the MAGNETic field strength at which perturbation theory breaks down.
[abstract 25 / 33] (score: 2) - Title: Fortifying gravitational-wave population inference with normalizing flowsAuthors: Christian Adamcewicz, Hugh McDougall, Paul D. Lasky, Eric Thrane,Comments: 23 pages, 13 figuresSubjects: astro-ph.HECreated: 2026-07-24; Updated: 2026-07-27; Datestamp: 2026-07-27
As the LIGO-Virgo-KAGRA collaboration's (LVK's) gravitational-wave transient catalog grows, we are learning a wealth of information from the population properties of binary BLACK HOLE mergers. Events in the catalog are represented with posterior samples describing the astrophysical parameters for each event. Population studies combine these samples to measure the distribution of astrophysical parameters such as BLACK HOLE masses and spins. However, the posterior-sample representation of each event is only approximate. We construct a mock population with masses drawn from an astrophysically-motivated distribution with sharp features. Using this, we demonstrate that when $\gtrsim 300$ events are combined, even with each event's posterior represented by $1 \times 10^4 {-} 2 \times 10^4$ samples, the numerical error can become large enough that the resulting population inference is unreliable. We consider two solutions. In the short term, we show that nested samples (already produced by LVK analyses) can be used to more accurately describe each event in population studies. But this will only grant a temporary reprieve until the nested-sample representation becomes inadequate. In the longer term, we propose to represent each event with a normalizing flow. In order to represent each event with sufficient accuracy, each normalizing flow can be used to generate an arbitrarily large number of new posterior samples with a significantly reduced computational cost relative to traditional sampling methods. When compared to nested sampling, our normalizing flows produce posterior draws with a median of $\approx 80\%$ fewer likelihood evaluations per sample, while also providing greater opportunity for parallelization. We believe refinement of normalizing flow architectures and training techniques in future works could further reduce this per-sample cost significantly.
[abstract 26 / 33] (score: 2) - Title: Experimental Demonstration of a Two-Dimensional Nonlinear Integrable System in a Particle AcceleratorAuthors: John Wieland, Alexander Valishev, Aleksandr Romanov, Nikita Kuklev, Giulio Stancari, Sergei Nagaitsev, Sebastian Szustkowski,Comments: 6 pages, 6 figuresSubjects: physics.acc-phCreated: 2026-07-23; Updated: 2026-07-27; Datestamp: 2026-07-27
A two-dimensional nonlinear integrable system was experimentally demonstrated at the FERMIlab Integrable Optics Test Accelerator. The system was implemented by inserting a special nonlinear MAGNET in a conventional accelerator lattice. We characterized the system by measuring lifetimes, transverse profiles and transverse oscillation frequencies of the 150-MeV electron beam as a function of the strength of the nonlinear insert. The measured shift of the working point and the amplitude-dependent detuning were consistent with theoretical predictions. We also observed the predicted bifurcation of the stable closed orbit. A striking consequence of the system's implementation was the possibility to operate the storage ring with integer tunes without lifetime degradation. This research opens up novel ways to design particle accelerators and to stabilize particle beams.
[abstract 27 / 33] (score: 2) - Title: Spectral evolution of mildly RELATIVISTIC electrons in solar flaresAuthors: Gregory D. Fleishman, Tatyana Kaltman, Sijie Yu, Gelu Nita,Comments: 23 pages, 13 pages, accepted to ApJSubjects: astro-ph.SR astro-ph.HECreated: 2026-07-24; Updated: 2026-07-27; Datestamp: 2026-07-27
Solar flares are a powerful engine capable of accelerating ambient plasma particles to high nonthermal energies. A key characteristic of these particles is their energy spectrum. Numerous studies of nonthermal hard X-ray emission established that a typical spectral evolution of the nonthermal electrons with energies of dozens keV follows a soft-hard-soft pattern in impulsive events and soft-hard-harder pattern in some long-duration events. Here we extend the study of the spectral evolution to the case of flare-accelerated mildly RELATIVISTIC electrons primarily responsible for the flare microwave emission. We examine the spatially resolved microwave emission observed with the Expanded Owens Valley Solar Array in twelve solar flares and find that they also typically follow a soft-hard-soft spectral evolution. However, the revealed spectral evolution of the mildly RELATIVISTIC electrons covers the spectral index range from 2-4 to 15 or more and, thus, is much more prominent than for the X-ray-producing electrons. The evolution of the spectral index is closely correlated with the emission flux and does not show any noticeable time delay. The spectral index displays a prominent correlation with the brightness temperature with a pattern similar to all events considered. We conclude that the revealed relationships and the evolutionary pattern is an inherent property of particle acceleration in the solar flares.
[abstract 28 / 33] (score: 2) - Title: The Distinctive Evolution and Spectral Energy Distribution of Binary Massive Black Hole AccretionAuthors: Yue Xu, Fu-Guo Xie, Ya-Ping Li, Yinhao Wu, Luis C. Ho,Comments: 21 pages, 10 figures, 2 tables, to appear in ApJSubjects: astro-ph.HE astro-ph.GACreated: 2026-07-24; Updated: 2026-07-27; Datestamp: 2026-07-27
Binary (super-)massive BLACK HOLEs (BHs) are expected to reside in the center of some galaxies. In this work, we re-visit accretion onto binary massive BHs, incorporating recent advances in both accretion theory and the mass transfer rate between the two massive BHs. We focus on relatively bright systems with an Eddington ratio of 0.1 for a binary with total BH mass $10^8\,M_\odot$, but consider a wide range of mass ratios $10^{-4} \le q \le 0.5$. The binary system consists of two mini-disks surrounding two individual BHs and a circumbinary disk surrounding the mass center of binary BHs. Depending on the mass ratio, the two mini-disks can be hot accretion flows, standard thin (cold) disks, or Slim disks. The radiative contributions from all three disks, each potentially in different accretion modes, are taken into account self-consistently. The spectral energy distributions of the binary BH system show universal ``notch'' features from the near-infrared to ultraviolet bands, caused by the gap or cavity in the accretion disk, consistent with previous studies. Binary with different mass ratios exhibit distinct spectral energy distribution properties, offering opportunities for testing (identifying candidates) with future broad band (infrared up to X-rays) observations. We also investigate the evolution of these binary systems, and find that, for systems with initial mass ratios $q \lesssim \text{a few} \times 10^{-3}$, the mass ratio evolves toward an equilibrium value $q \sim 10^{-3}$. For binary BH systems with a larger initial mass ratio, their mass ratio instead evolves toward unity.
[abstract 29 / 33] (score: 2) - Title: Bubble bursting in a sessile dropletAuthors: U. J. Gutiérrez-Hernández, B. Muñoz-Sánchez, A. Agúndez-Cruz, J. M. Montanero, D. Fernández Rivas, M. G. Cabezas,Comments:Subjects: physics.flu-dynCreated: 2026-07-24; Updated: 2026-07-27; Datestamp: 2026-07-27
We analyzed experimentally and numerically the bursting of a bubble within a sessile droplet. Our experiments show that both sessile droplet curvature and confinement enhance the energy focusing. In the low-viscosity regime, this effect results in thinner, faster Worthington JETs. In the high-viscosity regime, droplets are ejected for values of the Laplace number (the Reynolds number based on the visco-capillary velocity) smaller than the threshold for a bubble in an infinite liquid bath. This is probably the major result of the present work. Numerical simulations show the critical role of the additional pressure gradient arising from the curvature of the sessile droplet interface. The resulting force drives the liquid towards the bottom of the cavity, compressing it and accelerating JET formation. In the low-viscosity limit, the bottom of the cavity becomes smoother before JET ejection. This effect resembles the energy-focusing enhancement that occurs in an infinite liquid bath at the critical Laplace number, where short-wavelength waves are damped by viscosity.
[abstract 30 / 33] (score: 2) - Title: Full 3D Maxwell solver for Inertial Electrostatic Confinement devicesAuthors: Victor-Otto de Haan, Niels Geerits,Comments: 9 pages; 11 figuresSubjects: physics.plasm-phCreated: 2026-07-24; Updated: 2026-07-27; Datestamp: 2026-07-27
Results of a full 3D electroMAGNETic plasma fusion simulator are presented. It will enable investigations into the influence of structured electroMAGNETic potentials, anomalous MAGNETic moments, or charge cluster structures on the fusion yield. The simulator calculates fusion yields similar to those found in real world fusors. In addition, the ion energy and density are accurately simulated. Given that the ion properties arise from a full Maxwell solver there is ample evidence that this part of the simulation is accurate. Concluded with a recommendation for continued research.
[abstract 31 / 33] (score: 2) - Title: Discovery of a radio-flaring M dwarf in a commensal transient search of the LADUMA fieldAuthors: Moses Mlangeni, Patrick A. Woudt, Paul J. Groot, Alex Andersson, Zwidofhela N. Khangale, Francesco Cavallaro, Steven Bloemen, Paul Vreeswijk, David A. H. Buckley, Rob P. Fender, B. W. Stappers, D. L. A. Pieterse, R. Wijnands, Laura N. Driessen,Comments: Accepted for publication in MNRASSubjects: astro-ph.SR astro-ph.HECreated: 2026-07-24; Updated: 2026-07-27; Datestamp: 2026-07-27
We report the discovery and characterisation of MKT J032848.4-271904.6, a new radio transient identified in the LADUMA field using SARAO Science Data Processor (SDP) UHF-band images from approximately one year of MeerKAT observations. Using the Transient Pipeline (TraP) and advanced filtering techniques, we identified a number of candidate variable radio sources in the field. All but one show variability consistent with refractive interstellar scintillation, leaving MKT J032848.4-271904.6 as the sole source exhibiting intrinsic variability. In addition, MKT J032848.4-271904.6 shows intrinsic variability at 0.816 GHz, with 13 radio detections across 41 epochs and a peak flux density of 1.041+/-0.043 mJy. We associate this emission with a low-mass M-dwarf star LP 888-63, located 23 pc from the Sun and identified as a companion to the white dwarf binary system LAWD 14 / WD 0326-273. LP 888-63 displays active flaring behaviour across the electroMAGNETic spectrum, including multi-band optical data from MeerLICHT. TESS photometry reveals a periodic modulation in the blended light curve of 5.780+/-0.507 days, consistent with rotational variability of a mid-M dwarf. Archival ESO spectra reveal Halpha emission, confirming MAGNETic activity. These findings highlight the capability of MeerKAT's SDP imaging and facilities like MeerLICHT for real-time detection and characterisation of stellar transients.
[abstract 32 / 33] (score: 2) - Title: Proton-air interaction properties at $\sqrt{s} \simeq 100$ TeV from shower-depth measurements with the Pierre Auger Observatory and their connection to the Muon PuzzleAuthors: The Pierre Auger Collaboration, A. Abdul Halim, P. Abreu, M. Aglietta, M. Ahmed, I. Allekotte, K. Almeida Cheminant, R. Aloisio, J. Alvarez-Muñiz, A. Ambrosone, J. Ammerman Yebra, L. Anchordoqui, B. Andrada, L. Andrade Dourado, L. Apollonio, C. Aramo, J. C. Arteaga Velázquez, P. Assis, G. Avila, E. Avocone, A. Bakalova, Y. Balibrea, A. Baluta, F. Barbato, A. Bartz Mocellin, O. Batalla Cruz, J. P. Behler, C. Berat, M. E. Bertaina, M. Bianciotto, P. L. Biermann, V. Binet, K. Bismark, T. Bister, J. Biteau, J. Blazek, J. Blümer, M. Boháčová, D. Boncioli, C. Bonifazi, N. Borodai, J. Brack, P. G. Brichetto Orquera, S. Buitink, A. Bwembya, T. R. Caba Pineda, K. S. Caballero-Mora, S. Cabana-Freire, L. Caccianiga, J. Caraça-Valente, R. Caruso, A. Castellina, F. Catalani, G. Cataldi, L. Cazon, M. Cerda, B. Čermáková, A. Cermenati, K. Cerny, J. A. Chinellato, J. Chudoba, L. Chytka, R. W. Clay, A. C. Cobos Cerutti, R. Colalillo, R. Conceição, G. Consolati, M. Conte, F. Convenga, D. Correia dos Santos, P. J. Costa, C. E. Covault, M. Cristinziani, C. S. Cruz Sanchez, S. Dasso, K. Daumiller, B. R. Dawson, R. M. de Almeida, E. -T. de Boone, B. de Errico, J. de Jesús, S. J. de Jong, J. R. T. de Mello Neto, I. De Mitri, D. de Oliveira Franco, F. de Palma, V. de Souza, E. De Vito, A. Del Popolo, O. Deligny, N. Denner, K. Denner Syrokvas, L. Deval, A. di Matteo, C. Dobrigkeit, J. C. D'Olivo, L. M. Domingues Mendes, T. Dominguez, Y. Dominguez Ballesteros, Q. Dorosti, R. C. dos Anjos, J. Ebr, F. Ellwanger, R. Engel, M. Erdmann, A. Etchegoyen, C. Evoli, H. Falcke, G. Farrar, A. C. Fauth, T. Fehler, F. Feldbusch, A. Fernandes, M. Fernández Alonso, B. Fick, J. M. Figueira, P. Filip, A. Filipčič, B. Flaggs, A. Franco, M. Freitas, T. Fujii, A. Fuster, C. Galea, B. García, C. Gaudu, P. L. Ghia, U. Giaccari, M. Giammarco, C. Glaser, F. Gobbi, F. Gollan, G. Golup, P. F. Gómez Vitale, J. P. Gongora, N. González, D. Góra, A. Gorgi, M. Gottowik, F. Guarino, G. P. Guedes, Y. C. Guerra, L. Gülzow, S. Hahn, P. Hamal, M. R. Hampel, P. Hansen, V. M. Harvey, A. Haungs, M. Havelka, T. Hebbeker, C. Hojvat, J. R. Hörandel, P. Horvath, M. Hrabovský, T. Huege, A. Insolia, P. G. Isar, M. Ismaiel, P. Janecek, V. Jilek, K. -H. Kampert, B. Keilhauer, V. V. Kizakke Covilakam, H. O. Klages, M. Kleifges, A. Klingel, J. Köhler, F. Krieger, M. Kubatova, N. Kunka, B. L. Lago, N. Langner, N. Leal, M. A. Leigui de Oliveira, Y. Lema-Capeans, A. Letessier-Selvon, I. Lhenry-Yvon, L. Lopes, M. Mallamaci, S. Mancuso, D. Mandat, P. Mantsch, A. G. Mariazzi, C. Marinelli, I. C. Mariş, G. Marsella, D. Martello, S. Martinelli, O. Martínez Bravo, A. Martínez-Mendez, M. A. Martins, H. -J. Mathes, J. Matthews, G. Matthiae, E. Mayotte, S. Mayotte, P. O. Mazur, G. Medina-Tanco, D. Melo, A. Menshikov, C. Merx, S. Michal, M. I. Micheletti, L. Miramonti, M. Mogarkar, S. Mollerach, F. Montanet, L. Morejon, K. Mulrey, R. Mussa, W. M. Namasaka, S. Negi, L. Nellen, K. Nguyen, G. Nicora, M. Niechciol, D. Nitz, D. Nosek, A. Novikov, V. Novotny, L. Nožka, A. Nucita, L. A. Núñez, S. E. Nuza, J. Ochoa, M. Olegario, C. Oliveira, L. Östman, M. Palatka, J. Pallotta, G. Parente, T. Paulsen, M. Pech, J. Pękala, R. Pelayo, C. Pérez Bertolli, L. Perrone, S. Petrera, T. Pierog, M. Pimenta, M. Platino, P. Privitera, C. Priyadarshi, M. Prouza, K. Pytel, S. Querchfeld, J. Rautenberg, D. Ravignani, J. V. Reginatto Akim, M. Z. Rennó, A. Reuzki, J. Ridky, F. Riehn, M. Risse, V. Rizi, B. Rocha Moldes, E. Rodriguez, G. Rodriguez Fernandez, J. Rodriguez Rojo, S. Rossoni, M. Roth, E. Roulet, A. C. Rovero, A. Saftoiu, M. Saharan, F. Salamida, H. Salazar, G. Salina, P. Sampathkumar, N. San Martin, J. D. Sanabria Gomez, F. Sánchez, F. M. Sánchez Rodriguez, E. Santos, F. Sarazin, R. Sarmento, R. Sato, P. Savina, V. Scherini, H. Schieler, M. Schimp, D. Schmidt, O. Scholten, H. Schoorlemmer, P. Schovánek, F. G. Schröder, J. Schulte, T. Schulz, S. J. Sciutto, M. Scornavacche, A. Sedoski, S. Sehgal, S. U. Shivashankara, G. Sigl, K. Simkova, F. Simon, R. Šmída, S. Soares Sippert, P. Sommers, S. Stanič, J. Stasielak, P. Stassi, S. Strähnz, M. Straub, T. Suomijärvi, A. D. Supanitsky, Z. Svozilikova, Z. Szadkowski, F. Tairli, A. Tapia, C. Taricco, C. Timmermans, O. Tkachenko, P. Tobiska, C. J. Todero Peixoto, B. Tomé, A. Travaini, P. Travnicek, C. Trimarelli, M. Tueros, M. Unger, R. Uzeiroska-Geyik, L. Vaclavek, M. Vacula, I. Vaiman, J. F. Valdés Galicia, L. Valore, P. van Dillen, E. Varela, V. Vašíčková, A. Vásquez-Ramírez, D. Veberič, I. D. Vergara Quispe, S. Verpoest, V. Verzi, J. Vicha, S. Vorobiov, J. B. Vuta, A. A. Watson, A. Weindl, M. Weitz, L. Wiencke, H. Wilczyński, B. Wundheiler, B. Yue, A. Yushkov, E. Zas, D. Zavrtanik, M. Zavrtanik,Comments: Submitted to Phys. Rev. LettSubjects: hep-ex astro-ph.HECreated: 2026-07-24; Updated: 2026-07-27; Datestamp: 2026-07-27
Hybrid measurements at the Pierre Auger Observatory indicate that most high-energy hadronic interaction models underestimate the average depth of the shower maximum, $\langle X_{\max} \rangle$, at a center-of-mass energy of $\sqrt{s}=97.7 \pm 0.4^{+6.6}_{-6.2}\,\mathrm{TeV}$. In this Letter, the hadronic interaction models are shown to follow a universal relation between the predicted $\langle X_{\max} \rangle$ and the mean values of variables characterizing the energy spectra of secondary particles produced in the first interaction of proton-induced air showers. Assuming the validity of these relations in Nature, we map the values of $\langle X_{\max} \rangle$ favored by Auger data into mean values of these variables. All models favor an increase in the mean elasticity and in the fraction of hadronic energy in proton--air interactions. The latter must be amplified by a factor of $2.8$ to $4.6$ to account for the muon puzzle.
[abstract 33 / 33] (score: 2) - Title: Is S301 the Captured Companion of the Hypervelocity Star S5-HVS1?Authors: Andrea Caputo, Giovanni Maria Tomaselli,Comments: 3 pages, Claude's generated reproducibility repo at https://github.com/GimmyTomas/S301_S5-HVS1_BayesSubjects: astro-ph.GA astro-ph.HE astro-ph.SRCreated: 2026-07-24; Updated: 2026-07-27; Datestamp: 2026-07-27
Stellar binary disruptions through the Hills mechanism produce two fossils: a hypervelocity star (HVS), and a star tightly bound to the supermassive BLACK HOLE. Among known galactic HVSs, only S5-HVS1 has unambiguous galactic-centre origin. Its measured mass and velocity determine a relation between the mass and semi-major axis of its captured companion. GRAVITY has now discovered S301, whose orbit and photometrically inferred mass satisfy this relation, making it the only compelling candidate for the captured companion of S5-HVS1. We build a forward model for the Hills origin and compare it to the null hypothesis. This confirms that S301's orbit aligns much more closely with that of S5-HVS1's companion than a typical S-star. However, the catalog-level Bayes factor remains of order unity and dependent on the probabilities of survival and detection. S301 is thus a compelling candidate, but establishing its association with S5-HVS1 will require improved mass measurements, chemical comparisons and GRAVITY-calibrated selection functions.
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