Current date: 2026-05-27
Setting default datestamp limit: 0
Datestamp limit: 2026-05-27 (0 days ago)
Created/updated limit: 2026-05-20 (7 days ago)
Found keywords_cs.datFound keywords_cis.dat
Suggested sets: physics, physics:astro-ph, physics:gr-qc, physics:physics
Setting default set: physics
OAI-PMH request: http://export.arxiv.org/oai2?verb=ListRecords&from=2026-05-27&until=2026-05-27&set=physics&metadataPrefix=arXiv
Scoring abstracts
Number of records retrieved: 705
Keyword score statistics
score 12 -- 1 abstracts
score 9 -- 1 abstracts
score 7 -- 2 abstracts
score 6 -- 1 abstracts
score 5 -- 2 abstracts
score 4 -- 5 abstracts
score 3 -- 8 abstracts
score 2 -- 17 abstracts
in total -- 37 abstracts
Articles that appeared on 2026-05-27
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[abstract 1 / 37] Wow! (score: 12)
- Title: Detection of the distant QUASAR OP 313 with the first Large-Sized Telescope of CTAOAuthors: K. Abe, S. Abe, J. Abhir, A. Abhishek, V. A. Acciari, F. Acero, A. Aguasca-Cabot, I. Agudo, C. Alispach, D. Ambrosino, T. Aniello, S. Ansoldi, L. A. Antonelli, C. Aramo, A. Arbet-Engels, C. Arcaro, T. T. H. Arnesen, K. Asano, P. Aubert, A. Babić, C. Bakshi, A. Baktash, M. Balbo, A. Bamba, A. Baquero Larriva, V. Barbosa Martins, U. Barres de Almeida, J. A. Barrio, L. Barrios Jiménez, I. Batkovic, J. Baxter, J. Becerra González, W. Bednarek, E. Bernardini, J. Bernete, A. Berti, J. Besenrieder, C. Bigongiari, A. Biland, E. Bissaldi, O. Blanch, Ž. Bošnjak, G. Bonnoli, P. Bordas, G. Borkowski, A. Briscioli, E. Bronzini, G. Brunelli, J. Buces, A. Bulgarelli, I. Burelli, L. Burmistrov, A. Campoy-Ordaz, M. Cardillo, S. Caroff, A. Carosi, R. Carosi, R. Carraro, M. S. Carrasco, M. Carretero-Castrillo, F. Cassol, A. J. Castro-Tirado, D. Cerasole, G. Ceribella, A. Cerviño Cortínez, Y. Chai, K. Cheng, A. Chiavassa, M. Chikawa, G. Chon, L. Chytka, G. M. Cicciari, A. Cifuentes Santos, J. L. Contreras, J. Cortina, H. Costantini, S. Covino, M. Croisonnier, G. D'Amico, P. Da Vela, M. Dalchenko, F. Dazzi, A. De Angelis, M. de Bony de Lavergne, B. De Lotto, R. de Menezes, G. De Palma, V. de Souza, R. Del Burgo, L. Del Peral, M. Delfino, C. Delgado Mendez, J. Delgado Mengual, D. della Volpe, A. Di Piano, F. Di Pierro, R. Di Tria, L. Di Venere, C. Díaz, A. Dinesh, D. Dominis Prester, A. Donini, D. Dorner, M. Doro, L. Eisenberger, D. Elsässer, G. Emery, J. Escudero, L. Fariña, L. Feligioni, F. Ferrarotto, A. Fiasson, L. Foffano, L. Font, F. Frías García-Lago, S. Fröse, Y. Fukazawa, S. Gallozzi, R. J. García López, S. Garcia Soto, C. Gasbarra, D. Gasparrini, S. Gasparyan, M. Gaug, J. G. Giesbrecht Paiva, N. Giglietto, F. Giordano, P. Gliwny, N. Godinovic, T. Gradetzke, R. Grau, L. Greaux, D. Green, J. Green, G. Grolleron, S. Gunji, P. Günther, J. Hackfeld, D. Hadasch, A. Hahn, G. Harutyunyan, M. Hashizume, T. Hassan, K. Hayashi, L. Heckmann, M. Heller, J. Herrera Llorente, K. Hirotani, D. Hoffmann, D. Horns, J. Houles, M. Hrabovsky, D. Hrupec, D. Hui, M. Iarlori, R. Imazawa, T. Inada, Y. Inome, S. Inoue, K. Ioka, M. Iori, D. Israyelyan, T. Itokawa, A. Iuliano, J. Jahanvi, I. Jimenez Martinez, J. Jimenez Quiles, I. Jorge Rodrigo, J. Jormanainen, J. Jurysek, M. Kagaya, O. Kalashev, S. Kankkunen, V. Karas, H. Katagiri, T. Kayanoki, D. Kerszberg, M. Kherlakian, T. Kiyomot, G. W. Kluge, Y. Kobayashi, K. Kohri, A. Kong, J. Konrad, P. Kornecki, P. M. Kouch, G. Koziol, H. Kubo, J. Kushida, B. Lacave, M. Lainez, G. Lamanna, A. Lamastra, L. Lemoigne, E. Lindfors, M. Linhoff, S. Lombardi, F. Longo, R. López-Coto, M. López-Moya, A. López-Oramas, S. Loporchio, A. Lorini, J. Lozano Bahilo, F. Lucarelli, H. Luciani, L. Lulić, P. L. Luque-Escamilla, E. Lyard, P. Majumdar, M. Makariev, M. Mallamaci, D. Mandat, G. Maneva, M. Manganaro, S. Mangano, D. K. Maniadakis, G. Manicò, K. Mannheim, S. Marchesi, F. Marini, M. Mariotti, P. Marquez, G. Marsella, M. Martínez, J. Martí, G. Martínez, M. Martínez, O. Martinez, P. Maruševec, A. Mas-Aguilar, M. Massa, G. Maurin, D. Mazin, J. Méndez-Gallego, S. Menon, E. Mestre Guillen, D. Miceli, T. Miener, J. M. Miranda, R. Mirzoyan, M. Mizote, T. Mizuno, M. Molero Gonzalez, E. Molina, H. A. Mondal, T. Montaruli, A. Moralejo, D. Morcuende, A. Moreno Ramos, A. Morselli, V. Moya, A. L. Müller, H. Muraishi, S. Nagataki, T. Nakamori, C. Nanci, A. Negro, A. Neronov, V. Neustroev, D. Nieto Castaño, M. Nievas Rosillo, C. Nigro, L. Nikolic, K. Nilsson, K. Nishijima, K. Noda, D. Nosek, V. Novotny, S. Nozaki, M. Ohishi, Y. Ohtani, T. Oka, A. Okumura, R. Orito, L. Orsini, J. Otero-Santos, P. Ottanelli, S. Paiano, M. Palatiello, G. Panebianco, D. Paneque, F. R. Pantaleo, R. Paoletti, J. M. Paredes, M. Pech, M. Pecimotika, M. Peresano, M. Persic, F. Pfeifle, E. Pietropaolo, M. Pihet, G. Pirola, C. Plard, F. Podobnik, M. Polo, P. G. Prada Moroni, E. Prandini, M. Prouza, S. Rainò, R. Rando, W. Rhode, M. Ribó, J. Rico, V. Rizi, G. Rodriguez Fernandez, M. D. Rodríguez Frías, P. Romano, A. Roy, A. Ruina, E. Ruiz-Velasco, N. Sahakyan, T. Saito, S. Sakurai, D. A. Sanchez, H. Sano, E. Santos Moura, T. Šarić, Y. Sato, F. G. Saturni, V. Savchenko, F. Schiavone, B. Schleicher, K. Schmitz, F. Schmuckermaier, F. Schussler, T. Schweizer, A. Sciaccaluga, M. Seglar Arroyo, T. Siegert, G. Silvestri, A. Simongini, J. Sitarek, V. Sliusar, D. Sobczynska, I. Sofia, A. Stamerra, J. Strišković, D. Strom, M. Strzys, Y. Suda, A. Sunny, H. Tajima, M. Takahashi, J. Takata, R. Takeishi, P. H. T. Tam, S. J. Tanaka, D. Tateishi, T. Tavernier, P. Temnikov, Y. Terada, K. Terauchi, T. Terzic, M. Teshima, M. Tluczykont, F. Tokanai, T. Tomura, D. F. Torres, F. Tramonti, P. Travnicek, G. Tripodo, A. Tutone, S. Ubach, M. Vacula, J. van Scherpenberg, M. Vázquez Acosta, S. Ventura, S. Vercellone, G. Verna, I. Viale, A. Viana, A. Vigliano, C. F. Vigorito, E. Visentin, V. Vitale, V. Voitsekhovskyi, G. Voutsinas, I. Vovk, T. Vuillaume, R. Walter, C. Walther, L. Wan, F. Wersig, M. Will, J. Wójtowicz, T. Yamamoto, R. Yamazaki, Y. Yao, P. K. H. Yeung, T. Yoshida, T. Yoshikoshi, W. Zhang, I. Myserlis, R. Rao, M. Gurwell, G. Keating, A. Marscher, S. Jorstad, E. Angelakis, A. Kraus, C. Thum, J. A. Acosta-Pulido, A. Marchini, L. Stiaccini, P. Aceti, M. Banfi, S. Leonini, M. Conti, P. Rosi, L. M. Tinjaca Ramirez, J. Escudero Pedrosa, A. Sota, V. Casanova, F. J. Aceituno, V. Fallah Ramazani,Comments: 25 pages, 9 figuresSubjects: astro-ph.HECreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
In December 2023, the Large-Sized Telescope prototype (LST-1) detected for the first time VHE $γ$-ray emission from the FSRQ OP~313 becoming the furthest BLAZAR ever observed at VHE with z=0.997. We aim to characterize the $γ$-ray emission of OP 313 during this flare, comparing it with its average emission state in order to understand the processes leading to this detection. Its remarkable distance also enables studies on the Extragalactic Background Light (EBL), with the goal of evaluating the attenuation of VHE $γ$-ray photons. We characterize the $γ$-ray emission during the flare in December 2023 and the low emission state observed in January 2024 thanks to the LST-1 and MAGIC data and quasi-simultaneous \textit{FERMI}-LAT observations. This dataset also enables us to evaluate the EBL attenuation by systematically exploring the EBL intensity over the $γ$-ray spectrum. Finally, we study the multi-wavelength emission and interpret the broadband spectral energy distribution (SED) within BLAZAR radiative models including the thermal contributions from the accretion disc, dusty torus and broad line region. We also characterize the flare brightness in the high-energy (HE, $E>100$~MeV) $γ$-ray band, that was found to be a factor 50 above the average emission seen by \textit{FERMI}-LAT. The HE and VHE observations allow us to set constrains to the EBL density. Finally, thanks to the extensive multi-wavelength campaign organized, we are able to construct and model the broadband SED of OP~313 within the framework of a two-zone leptonic model where the $γ$-ray emission is produced via inverse-Compton scattering of the broad line region, accretion disk and dusty torus photon fields. However the dominant external photon field remains unknown, as several combinations are able to successfully explain the $γ$-ray emission observed.
[abstract 2 / 37] Wow! (score: 9) - Title: Multimessenger Characterization of High-Energy Neutrino Emission from the Brightest Neutrino-Active Galactic NucleiAuthors: Jose Alonso Carpio, Ali Kheirandish, Kohta Murase,Comments: 17 pages, 10 figures, 3 tables, minor revision, accepted for publication in ApJSubjects: astro-ph.HE hep-phCreated: 2026-05-25; Updated: 2026-05-27; Datestamp: 2026-05-27
The observation of high-energy neutrinos from the direction of the nearby active galaxy, NGC 1068, was a major step in identifying the origin of high-energy cosmic neutrinos. The multimessenger data imply that high-energy neutrinos originate from the hearts of active galaxies which are opaque to GeV-TeV $γ$-rays. This realization is reinforced by the excess of neutrinos in the direction of NGC 4151 and Circinus Galaxy, other nearby ACTIVE GALACTIC NUCLEi (AGNs). Understanding the vicinity of supermassive BLACK HOLEs with electroMAGNETic radiation is often challenging due to uncertainties associated with the absorption of emission in these dense environments, and neutrinos can be used as a powerful probe of the inner parts of the active galaxies. Considering the five brightest neutrino-active galaxies, NGC 1068, NGC 4151, CGCG 420-15, Circinus Galaxy, and NGC 7469, we employ the measured neutrino spectra together with the sub-GeV $γ$-ray emission measured by the {\em FERMI} satellite to break the degeneracy and narrow in on the parameter space of neutrino emission from turbulent coronae of AGNs. We also study contributions of JET-quiet AGNs, whose properties are similar to NGC 1068 and NGC 7469, to the isotropic neutrino background flux, through exploring possibilities that the neutrino luminosity function may deviate from the X-ray luminosity function. Our results will help estimate the prospects for identifying additional neutrino-active galaxies and guide future targeted analyses.
[abstract 3 / 37] Wow! (score: 7) - Title: Multi Messenger Study of GRB 221009A with VHE Gamma-ray and Neutrino Afterglow from a Gaussian Structured JetAuthors: T. Mondal, S. Razzaque, Jagdish C. Joshi, S. Majumder, D. Bose,Comments: 16 pages, 10 figuresSubjects: astro-ph.HECreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
Recent detections of very-high-energy (VHE; $\gtrsim 100~{\rm GeV}$) emission from GRB afterglows, most notably the unprecedented brightness of GRB~221009A observed by LHAASO, reveal components beyond the standard electron SYNCHROTRON model. The multi-TeV photons motivate SYNCHROTRON self-Compton and possible hadronic contributions, while the non-detection of coincident neutrinos by IceCube/KM3NeT/GRAND200k constrains the microphysical parameters, JET kinetic energy, and ambient-medium density. We model the VHE afterglow of GRB~221009A with an external forward shock from a Gaussian structured JET in a uniform-density medium. This angular structure reproduces the extreme TeV output at an off-axis angle but without demanding large energies as in a top-hat JET. We compute the corresponding $pγ$ neutrino flux in the PeV-EeV range and derive a time-integrated upper limit using the effective areas of IceCube-Gen2 and GRAND200k. This provides insight into the contribution of individual GRBs to neutrino events. The predicted neutrino flux for GRB~221009A, using parameters inferred from the multi-wavelength spectral energy distribution, lies below the sensitivities of these detectors. Even our correlation analysis, optimized for neutrino searches with the upcoming GRAND200k, indicates that the expected number of events from this GRB is of order $\sim 0.1$ under a highly optimistic microphysical parameter regime. We also compare neutrino-flux variations from on-axis and off-axis viewing geometries and find an approximately order of magnitude difference in the signal. Thus, our study concludes that a brighter burst closer than GRB~221009A would be crucial for neutrino detection by upcoming telescopes. Future GRB detections by the Cherenkov Telescope Array will provide important constraints on their geometry, radiation mechanisms, and possible associated neutrino signals.
[abstract 4 / 37] Wow! (score: 7) - Title: Implications of the nanoHertz Gravitational-Wave Background for Galactic Feedback and Massive Black Hole GrowthAuthors: Megan Taylor Tillman, Blakesley Burkhart, Chiara M. F. Mingarelli, J. Andrew Casey-Clyde, Lars Hernquist, Sownak Bose, Enikő Regős, César Hernández-Aguayo,Comments: 21 pages, 8 figures, 2 tables, accepted to ApJLSubjects: astro-ph.GA astro-ph.HECreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
We investigate how pulsar timing array (PTA) measurements of the nanoHertz gravitational-wave background (GWB) can constrain models for the growth history of supermassive BLACK HOLEs (SMBHs) and how ACTIVE GALACTIC NUCLEus (AGN) and stellar feedback models can affect GWB predictions. Feedback regulates supermassive BLACK HOLE (SMBH) growth, altering the BLACK HOLE mass function (BHMF). Using BHMFs drawn from multiple cosmological simulation suites including IllustrisTNG, MillenniumTNG, Simba, and CAMELS, and combining these with a QUASAR-based SMBH binary population framework, we predict the resulting GWB amplitude under a range of different stellar and AGN feedback prescriptions. We find that the choice of both stellar and AGN feedback models alters the high-mass end of the BHMF and changes the predicted GWB amplitude by up to a factor of 2 for the fiducial simulations and a factor 10 for extreme feedback variations in CAMELS. Models with inefficient or absent AGN feedback produce abundant SMBHs and yield GWB amplitudes consistent with PTA data, yet fail in producing realistic galaxies. Fiducial models of AGN and stellar feedback suppress SMBH growth too much and under-predict the expected signal, an effect which could possibly be mitigated by more realistic BLACK HOLE seeding and growth prescriptions. The mismatch between the GWB amplitudes predicted by cosmological simulations and that inferred by PTA measurements suggests that SMBH growth is more efficient or occurs earlier than captured by current models. This demonstrates that PTA measurements provide a powerful new probe of not only the SMBH population but also feedback physics.
[abstract 5 / 37] Yes (score: 6) - Title: GWTC-5.0: An Introduction to Version 5.0 of the Gravitational-Wave Transient CatalogAuthors: The LIGO Scientific Collaboration, the Virgo Collaboration, the KAGRA Collaboration, A. G. Abac, A. Abe, I. Abouelfettouh, F. Acernese, K. Ackley, A. Adam, S. Adhicary, D. 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, L. Albers, W. Ali, S. Al-Kershi, C. Allene, A. Allocca, S. Al-Shammari, J. A. Alvarez, S. Alvarez-Lopez, W. Amar, O. Amarasinghe, A. Amato, F. Amicucci, C. Amra, A. B. Anand, C. Anand, A. Ananyeva, S. B. Anderson, W. G. Anderson, M. Andia, M. Ando, F. Andrade-Oliveira, M. Andrés-Carcasona, J. L. Andrey, T. Andrić, J. Anglin, J. Anna, J. M. Antelis, S. Antier, T. Aoki, M. Aoumi, E. Z. Appavuravther, E. A. Appelt, 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, P. S. Aswathi, F. Attadio, F. Aubin, K. AultONeal, G. Avallone, N. Avdeev, E. A. Avila, S. Babak, C. Badger, S. Bae, S. Bagnasco, S. Baimukhametova, L. Baiotti, T. Baka, K. A. Baker, T. Baker, G. Balbi, G. Baldi, N. Baldicchi, M. Ball, G. Ballardin, M. Ballelli, 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, 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, J. C. Bayley, A. C. Baylor, P. A. Baynard, M. Bazzan, V. M. Bedakihale, F. Beirnaert, M. Bejger, A. S. Bell, C. Bellani, D. S. Bellie, D. Beltran-Martinez, E. Benedetti, W. Benoit, I. Bentara, M. Ben Yaala, S. Bera, F. Bergamin, B. K. Berger, M. Beroiz, C. P. L. Berry, I. Berry, D. Bersanetti, T. Bertheas, A. Bertolini, J. Betzwieser, D. Beveridge, N. Bevins, J. Bezerra-Sobrinho, R. Bhandare, R. Bhatt, A. Bhattacharjee, D. Bhattacharjee, S. Bhattacharyya, S. Bhaumik, V. Biancalana, F. Bianchi, I. A. Bilenko, M. Bilicki, G. Billingsley, A. Binetti, S. Bini, 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, M. Bloch, N. Bode, N. Boettner, P. Bogdan, G. Boileau, M. Boldrini, G. N. Bolingbroke, L. D. Bonavena, 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, T. D. Boybeyi, 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, D. D. Brown, M. L. Brozzetti, S. Brunett, G. Bruno, R. Bruntz, J. Bryant, Y. Bu, F. Bucci, A. Buchicchio, A. Buggiani, O. Bulashenko, T. Bulik, H. J. Bulten, A. Buonanno, K. Burtnyk, R. Buscicchio, N. Busdon, D. Buskulic, R. L. Byer, R. Cabrita, V. A. Cáceres-Barbosa, L. Cadonati, G. Cagnoli, C. Cahillane, A. Calafat, J. Calderón Bustillo, J. D. Callaghan, T. A. Callister, E. Calloni, S. R. Callos, K. Cannon, V. Cantory, H. Cao, L. A. Capistran, E. Capocasa, G. Capoccia, E. Capote, C. Capuano, G. Capurri, F. Carbognani, K. J. Cardona-Martínez, M. Carlassara, M. Carpinelli, G. Carrillo, G. Carullo, A. Casallas-Lagos, J. Casanueva Diaz, C. Casentini, 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, C. Chan, J. C. L. Chan, M. Chan, C. -Y. Chang, 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, Yiwen 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, A. Chiummo, A. Chopra, C. Chou, S. Choudhary, N. Christensen, Y. K. Chu, S. S. Y. Chua, G. Ciani, P. Ciecielag, M. Cieślar, M. Cifaldi, B. Cirok, F. Clara, J. A. Clark, T. A. Clarke, A. Claveus, M. R. Claypool, S. Clesse, F. Cleva, S. M. Clyne, E. Coccia, E. Codazzo, P. -F. Cohadon, D. E. Cohen, E. Colangeli, O. Cole, M. Colleoni, C. G. Collette, J. Collins, S. Colloms, A. Colombo, G. Compère, C. M. Compton, G. Connolly, L. Conti, T. R. Corbitt, I. Cordero-Carrión, S. Corezzi, N. J. Cornish, A. Corsi, S. Cortese, L. A. Corubolo, L. Cotnoir, R. Cottingham, J. A. Cotturone, M. W. Coughlin, P. Couvares, R. Coyne, A. Cozzumbo, J. D. E. Creighton, T. D. Creighton, S. Crook, R. Crouch, J. Csizmazia, K. Csukás, T. J. Cullen, A. Cumming, E. Cuoco, M. Cusinato, R. R. Cuzinatto, L. V. da Conceição, T. Dal Canton, S. Dall'Osso, S. Dal Pra, G. Dálya, Y. Dang, B. D'Angelo, S. Danilishin, O. Danner, S. D'Antonio, K. Danzmann, K. E. Darroch, L. P. Dartez, R. Das, S. Das, A. Dasgupta, V. Dattilo, A. Daumas, I. Dave, A. Davenport, T. F. Davies, D. Davis, M. C. Davis, P. Davis, E. J. Daw, M. Dax, J. De Bolle, E. deBruin, 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, C. de Melo, N. Demos, T. Dent, A. Depasse, N. DePergola, R. De Pietri, R. De Rosa, C. De Rossi, E. K. Derrick, M. Desai, D. DeSantis, S. Deshmukh, V. Deshmukh, R. De Simone, S. Determan, S. Dhage, A. Dhani, R. Dhatri, R. Dhurkunde, R. Diab, C. Diaz, M. C. Díaz, F. Diaz Guerra, M. Di Cesare, M. A. Dicorato, T. Dietrich, C. Di Fronzo, M. Di Giovanni, 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, S. Doravari, O. Dorosh, S. Doshi, F. Dosopoulou, M. Drago, J. C. Driggers, M. Dubois, R. S. Dumbreck, U. Dupletsa, D. D'Urso, P. Dutta Roy, H. Duval, S. Dwivedi, S. E. Dwyer, C. Eassa, M. Eberhardt, M. Ebersold, M. Ebiri, G. Eddolls, A. Effler, J. Eichholz, H. Einsle, M. Eisenmann, M. Emma, K. Endo, R. Enficiaud, V. Ernst, L. Errico, R. Espinosa, M. Esposito, R. C. Essick, H. Estellés, T. Etzel, M. Evans, T. Evstafyeva, 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. -N. Feldhusen, E. Fenyvesi, A. Feo, J. Fernandes, T. Fernandes, G. Fernández Rodríguez, D. Fernando, S. Ferraiuolo, T. A. Ferreira, M. Ferrer-Martinez, F. Fidecaro, P. Figura, I. Fiori, M. Fishbach, R. P. Fisher, S. K. Fitzgerald, V. Fiumara, R. Flaminio, B. Flanagan, S. M. Fleischer, L. S. Fleming, F. Flocco, E. Floden, H. Fong, J. A. Font, F. 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Stanford, A. Stanton, D. A. Steer, N. Steinle, J. Steinlechner, S. Steinlechner, C. Stephens, N. Stergioulas, S. P. Stevenson, M. StPierre, J. Stremiz, M. D. Strong, A. Strunk, R. Sturani, M. Suchenek, S. Sudhagar, R. Sugimoto, L. Suleiman, K. D. Sullivan, J. Sun, L. Sun, S. Sunil, J. Suresh, P. J. Sutton, K. Suzuki, M. Suzuki, A. Svizzeretto, B. L. Swinkels, A. Syx, M. J. Szczepańczyk, M. Tacca, M. Tagliazucchi, H. Tagoshi, S. C. Tait, H. Takaba, K. Takada, H. Takahashi, R. Takahashi, A. Takamori, S. Takano, H. Takeda, I. Takimoto Schmiegelow, C. Talbot, M. Tamaki, N. Tamanini, D. Tanabe, K. Tanaka, S. J. Tanaka, S. Tanioka, D. B. Tanner, W. Tanner, L. Tao, R. D. Tapia, E. N. Tapia San Martín, A. Taruya, J. D. Tasson, J. G. Tau, A. Tejera, J. G. Temple, Y. Teng, H. Themann, A. Theodoropoulos, M. P. Thirugnanasambandam, L. M. Thomas, M. Thomas, P. Thomas, J. E. Thompson, S. R. Thondapu, E. Thrane, J. Tissino, A. Tiwari, Pawan Tiwari, Praveer Tiwari, S. Tiwari, V. Tiwari, M. R. Todd, E. Tofani, M. Toffano, A. M. Toivonen, K. Toland, T. Tomaru, V. Tommasini, H. Tong, C. I. Torrie, I. Tosta e Melo, E. Tournefier, A. Trapananti, R. Travaglini, F. Travasso, G. Traylor, L. Traylor, M. Trevor, M. C. Tringali, A. Tripathee, G. Troian, A. Trovato, L. Trozzo, R. J. Trudeau, T. Tsang, S. Tsuchida, K. Tsuji, L. Tsukada, A. Tuci, M. Turconi, C. Turski, H. Ubach, A. S. Ubhi, N. Uchikata, T. Uchiyama, R. P. Udall, T. Uehara, V. Undheim, V. Upadhyaya, L. E. Uronen, T. Ushiba, M. Vacatello, H. Vahlbruch, G. Vajente, J. Valencia, M. Valentini, E. Vallejo-Pagès, S. A. Vallejo-Peña, S. Vallero, M. van Dael, E. Van den Bossche, J. F. J. van den Brand, C. Van Den Broeck, M. van der Kolk, M. van der Sluys, A. Van de Walle, J. van Dongen, K. Vandra, M. VanDyke, H. van Haevermaet, J. V. van Heijningen, P. Van Hove, J. Vanier, J. Vanosky, N. van Remortel, M. Vardaro, A. F. Vargas, V. Varma, A. Vecchio, G. Vedovato, J. Veitch, P. J. Veitch, S. Venikoudis, P. Verdier, M. Vereecken, D. Verkindt, B. Verma, S. Verma, Y. Verma, S. M. Vermeulen, F. Vetrano, A. Veutro, A. Viceré, S. Vidyant, A. D. Viets, A. Vijaykumar, A. Vilkha, N. Villanueva Espinosa, E. T. Vincent, J. -Y. Vinet, S. Viret, S. Vitale, A. Vives, L. Vizmeg, B. Vizzone, 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, R. -Z. Wan, H. Wang, L. Wang, P. Wang, W. H. Wang, Y. F. Wang, Z. Wang, R. L. Ward, 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. Wimmer, C. W. Winborn, A. Wingfield, J. Winterflood, C. C. Wipf, G. Woan, N. E. Wolfe, H. T. Wong, I. C. F. Wong, T. Wouters, J. L. Wright, M. Wright, B. Wu, C. Wu, D. S. Wu, H. Wu, J. Wu, K. 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. Yébana Carrilero, A. B. Yelikar, X. Yin, J. Yokoyama, T. Yokozawa, M. Yoshihara, S. Yuan, H. Yuzurihara, M. Zanatta, M. Zanolin, M. Zeeshan, T. Zelenova, J. -P. Zendri, M. Zeoli, M. Zerrad, M. Zevin, H. Zhang, J. Zhang, L. Zhang, N. Zhang, R. Zhang, T. Zhang, C. Zhao, J. Zhao, Yue Zhao, Yuhang Zhao, L. -M. Zheng, Y. Zheng, L. Zhizhong, H. Zhong, H. Zhou, H. O. Zhu, X. -J. Zhu, Z. -H. Zhu, Z. Zhu, D. Z. Zieba, A. B. Zimmerman, L. Zimmermann, M. E. Zucker,Comments: This article supersedes the corresponding GWTC-4 article, arXiv:2508.18080Subjects: gr-qc astro-ph.HECreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
The Gravitational-Wave Transient Catalog (GWTC) is a collection of short-duration (transient) gravitational-wave signals identified by the LIGO-Virgo-KAGRA Collaboration in gravitational-wave data produced by the eponymous detectors. The catalog provides information about the identified candidates, such as the arrival time and amplitude of the signal and properties of the signal's source as inferred from the observational data. GWTC is the release of this dataset and version 5.0 extends the catalog to include observations made during the second part of the fourth LIGO-Virgo-KAGRA observing run up until 2025 January 28. This paper marks an introduction to a collection of articles related to this version of the catalog, GWTC-5.0. This update significantly increases the number of detected merging binary systems of BLACK HOLEs and neutron stars to over 300, enabling many follow-up studies toward understanding the gravitational-wave universe. The collection of articles accompanying the catalog provides documentation of the methods used to analyze the data, summaries of the catalog of events, observational measurements drawn from the population, and detailed discussions of selected candidates.
[abstract 6 / 37] Yes (score: 5) - Title: IGR J12580+0134: A Possible Repeated Partial Tidal Disruption Event Inferred from Late-Time Radio Re-brighteninAuthors: Po Ma, Shao-Yu Fu, Linhui Wu, Wei-Hua Lei, Qiang Yuan,Comments: 17 pages, 6 figures, 2 tables, submitted to ApJSubjects: astro-ph.HECreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
Repeating partial tidal disruption events (pTDEs) provide a direct probe of stellar orbits and episodic mass loss around supermassive BLACK HOLEs, but robust identification requires multi-band and multi-epoch evidence. %consistent with a single physical origin. We investigate whether the late-time radio rebrightening of the nuclear transient IGR~J12580+0134 in NGC~4845 can be explained as a repeating pTDE, using multi-epoch Karl G.\ Jansky VLA observations together with X-ray constraints from \textit{SWIFT}/XRT and \textit{NICER}. Through a systematic analysis of the radio data, we identify two well-defined radio flares and a possible third late-time rebrightening flare. Modeling the second flare with a SYNCHROTRON afterglow framework using Markov Chain Monte Carlo fitting is consistent with a sub-RELATIVISTIC outflow with a characteristic velocity of order ${v \simeq 0.3c}$, an isotropic-equivalent kinetic energy of order ${10^{50}}$ erg, and an approximately constant-density circumnuclear medium. No significant contemporaneous brightening is detected by \textit{SWIFT}/XRT during the 2016 radio flare, while faint \textit{NICER} flares in 2023 suggest intermittent low-level accretion. We also considered several possible interpretations for the late-time radio rebrightening, and found that the repeated pTDE scenario provides a more natural overall explanation for the observed phenomenology. Given the currently sparse data coverage, continued sensitive radio and X-ray monitoring will be essential to test this interpretation and to search for future reactivations.
[abstract 7 / 37] Yes (score: 5) - Title: Supermassive Black Holes: modelling strongly and weakly MAGNETised misaligned accretion disksAuthors: Joshua Samuel Stanway, Cora Prather, Derek Ward-Thompson, Timothy J. Walton, Brett Patterson, Hyerin Cho,Comments: 13 pages, 12 figuresSubjects: astro-ph.HECreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
In this paper, we carry out a numerical study of misaligned accretion disks around spinning supermassive BLACK HOLEs. Here, we conduct a parameter survey covering a range of initial disk misalignment angles ($\mathcal{T}_\mathrm{init}=15^\circ, 45^\circ, 75^\circ$) with either the Magnetically Arrested Disk (MAD) or Standard And Normal Evolution (SANE) MAGNETic field configurations, using the general-RELATIVISTIC MAGNETohydrodynamic (GRMHD) code KHARMA. We find that models in the MAD state can align with the BLACK HOLE up to $\sim10 \, r_g$, even in extremely misaligned models ($\mathcal{T}_\mathrm{init}=75^\circ$), which has not been seen before. Models without a dynamically important MAGNETic field remain misaligned up to the BLACK HOLE, with a maximum disk tilt at $\sim10 \, r_g$, the peak's radial distance from the BLACK HOLE increases with increasing disk misalignment. However, the maximum disk tilt does not have a linear relationship with the initial disk misalignment, and appears to have a maximum value of $\sim50^\circ$. We also show misaligned disk simulations produced in KHARMA are consistent with other GRMHD codes, for a variety of problems.
[abstract 8 / 37] Yes (score: 4) - Title: Simulation Study of Binary Mergers of Galaxy Clusters I: Properties of Merger Shocks and Radio EmissionAuthors: Hyesung Kang, Dongsu Ryu, Jeongbhin Seo,Comments: 25 pages, 12 figures, submitted to ApJSubjects: astro-ph.HECreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
We investigate binary mergers of galaxy clusters, the formation of shocks, and the resulting radio relics using three-dimensional simulations. The initial setup consists of two idealized spherical subclusters with a mass ratio below three, each permeated by turbulent MAGNETic fields, and we follow their merger with a high-order accurate MAGNETohydrodynamic (MHD) code. In parallel, we track the acceleration of cosmic-ray electrons (CRe) via diffusive shock acceleration (DSA) at merger-driven shocks, together with radiative cooling and FERMI-II (turbulent) acceleration in the postshock region, employing a newly developed Eulerian Fokker-Planck solver. Synchrotron emission is computed from the simulated CRe distribution and MAGNETic fields. In this paper, we detail these numerical approaches and present the first results obtained with them. Two prominent axial shocks emerge along the merger axis; the shock ahead of the heavier subcluster systematically attains a higher Mach number, although it is more compact, than that ahead of the lighter subcluster. Turbulent MAGNETic fields, which are both inherited from the initial conditions and amplified during the merger, produce patchy, fine-scale structures in the radio surface brightness. Because of the combined effects of turbulent acceleration, spatially nonuniform MAGNETic fields, and the curved geometry of merger shocks, the volume-integrated radio spectra show deviations from the canonical power-law steepening expected for a planar shock with a uniform field. Reacceleration of preexisting fossil CRe enhances the surface brightness. Our results highlight the coupled roles of merger dynamics, MHD turbulence, and CRe physics in shaping the observed properties of radio relics in cluster outskirts.
[abstract 9 / 37] Yes (score: 4) - Title: You can't see me: Super-Eddington growth hindering X-ray detection in high-z broad-line ACTIVE GALACTIC NUCLEiAuthors: Alessandro Trinca, Alessandro Lupi, Francesco Haardt, Piero Madau,Comments: 10 pages, 11 figures, 1 appendix. Accepted for publication in Astronomy & AstrophysicsSubjects: astro-ph.GA astro-ph.HECreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
We revisit BLACK HOLE mass estimates for high-redshift broad-line ACTIVE GALACTIC NUCLEi (AGNs) discovered with JWST by jointly analysing their broad emission lines and their systematic non-detections in deep Chandra imaging. Building upon a self-shadowed, super-Eddington accretion framework in which the corona undergoes efficient radiative over-cooling, we couple funnel-dependent Comptonisation physics with slim-disc spectral models and explore the resulting parameter space through a full MCMC inference. Using a recently compiled sample of JWST high-redshift broad-line AGNs, we show that the observed X-ray weakness - manifested as extreme bolometric corrections, suppressed 2-10 keV luminosities, and non-detections in the 0.5-5 keV Chandra band - naturally arises when the corona is confined and radiatively over-cooled inside a narrow super-Eddington funnel. The combined broad line+X-ray analysis yields strongly bimodal posteriors: either very massive, very low-Eddington BLACK HOLEs (physically disfavoured), or a population of low-mass ($\sim 10^{6}$-$10^{7} M_{\odot}$) BLACK HOLEs accreting at $f_{\rm Edd} \gg 1$. The latter solution is strongly preferred for nearly all objects and returns masses consistent with, or lower than, local $M_{\rm BH}$-$M_{\star}$ relations, mitigating the extreme mass ratios implied by single-epoch virial estimators. The predicted intrinsic spectra are redder and exhibit reduced hard-X-ray output but higher bolometric luminosities, implying bolometric corrections larger than those typical of the local AGN population, yet consistent with low-redshift highly accreting counterparts. These results support a picture in which many JWST broad-line AGNs are powered by rapidly growing, super-Eddington BLACK HOLEs whose suppressed coronal emission and self-shadowed BLR geometry combine to mimic overmassive BLACK HOLEs at $z \gtrsim 6$.
[abstract 10 / 37] Yes (score: 4) - Title: NUSTAR as an Axion Helioscope: probing axion-nucleon and axion-electron couplingsAuthors: Tiziano Zanzarella, Francisco R. Candón, Maurizio Giannotti, Marco Regis, Jaime Ruz, Marco Taoso, Elisa Todarello, Julia K. Vogel,Comments: 18 pages, 7 figuresSubjects: astro-ph.CO astro-ph.HE hep-phCreated: 2026-05-25; Updated: 2026-05-27; Datestamp: 2026-05-27
We investigate solar X-ray observations as a probe of axions and axion-like particles. These particles can be produced in the interior of the Sun via the conversion of thermal photons, as well as through processes involving axion-electron and axion-nucleon interactions. The resulting axions can then reconvert into photons in the Sun's atmospheric MAGNETic field, generating a signal in the X-ray energy range. In this work, we derive new limits on axions using X-ray observations with the Nuclear Spectroscopic Telescope Array (NUSTAR) during the 2020 solar minimum. In the regime where ALP production is dominated by couplings to electrons or nucleons, we obtain bounds on the product of couplings $g_{ae}\cdot g_{aγ}\lesssim 1.1\times10^{-24}\,\rm GeV^{-1}$ and $g_{aN}^{\rm eff}\cdot g_{aγ}\lesssim 2.3\times 10^{-19}\,\rm GeV^{-1}$ at 95% CL, for axion masses $m_a\lesssim10^{-6}\,\rm eV$. These constraints strongly improve current ground-based experimental limits, establishing solar X-ray observations as a powerful and robust method for axion searches.
[abstract 11 / 37] Yes (score: 4) - Title: Energy extraction from NED-deformed rotating BLACK HOLEs via the Comisso-Asenjo RECONNECTion processAuthors: Marco Figliolia, Gaetano Lambiase, Ali Övgün, R. C. Pantig,Comments: 21 pages, 10 figuresSubjects: gr-qc astro-ph.HECreated: 2026-05-25; Updated: 2026-05-27; Datestamp: 2026-05-27
We study rotating BLACK HOLEs in general relativity coupled to nonlinear electrodynamics (NED), focusing on an axisymmetric solution with deformation parameter g. On the spherical seed, weak-field lensing via the Gauss-Bonnet method and the shadow radius yield a spin-insensitive bound by enforcing a conservative ~10% tolerance on the Sgr A* ring size, namely g/M \lesssim 1.26. In the eikonal regime we derive analytic quasinormal-mode shifts, even in g, and obtain an independent ceiling consistent with the shadow constraint. For the rotating geometry, we provide closed-form ZAMO scalars, chart horizons and ergoregion, and analyze equatorial geodesics (photon orbits and ISCO). We then formulate in the ZAMO frame the Comisso-Asenjo RECONNECTion channel, identify the negative-energy window, and integrate the extracted power over the allowed radii; from the tolerated fractional departure from the Kerr power we define a spin-dependent extraction bound g_δ(a|σ_0,ξ). Taken together, the QNM/shadow ceiling and the extraction bound appreciably narrow the admissible region for g/M in the (a/M, g/M) plane, so even within our deliberately simplified, single-layer equatorial setup, the two complementary probes already provide informative constraints on NED deformations, testable with present data and upcoming horizon-scale and ringdown campaigns.
[abstract 12 / 37] Yes (score: 4) - Title: The first near-infrared high-resolution échelle spectroscopy of the outflow in NGC 4151. A study of the clouds covering the Eye of SauronAuthors: Francesco Gabriele Saturni, Riccardo Middei, Hermine Landt, Valerio D'Elia, Fabio La Franca, Matteo Perri, Enrico Piconcelli,Comments: 12 pages, 7 figures, 3 tables, accepted for publication on Astronomy & AstrophysicsSubjects: astro-ph.GACreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
We present the first high-resolution near-infrared spectroscopy of the nucleus of the nearby, well-known Seyfert galaxy NGC 4151 (the "Eye of Sauron"). Past studies of this source have revealed that it exhibits a variable absorption feature associated with the He I $λ$10,830 AA emission line, potentially indicative of obscuration events affecting the central engine. Here, we take advantage of the IRTF/iSHELL and TNG/GIANO-B spectrographs to observe this feature with unprecedented spectral resolution ($λ/Δλ> 50,000$), being able to study in detail the structure of the absorption trough and its variations over a time span of $\sim$700 days. In order to infer a connection between the He I absorption variability and that of the X-ray ionising continuum, we also analyse the publicly available data collected by the SWIFT-XRT instrument over the same period of time, unveiling a potential driving mechanism in the changes of the outflow ionisation state due to the X-ray flux variations. We also derive outflow physical parameters - $\dot{M}_{\rm out} \lesssim 10^{-2}$ M$_\odot$ yr$^{-1}$, $r_{\rm out} \sim 3$ pc, $v_{\rm max} \sim 1000$ km s$^{-1}$ - that are in line with those of comparable ionised winds found in similar targets, where the outflow is not powerful enough to trigger a significant AGN feedback ($\dot{E}_{\rm kin}/L_{\rm bol} \sim 0.001$%). Such findings point at a scenario in which a dusty and clumpy outflow that obscures NGC 4151 up to galactic scales responds to changes in the ionising X-ray flux, similarly to what happens in QUASARs with broad absorption lines and Seyferts with multiphase outflows such as NGC 5548.
[abstract 13 / 37] (score: 3) - Title: Co-evolution of COSMIC RAY energy spectra, composition, and anisotropiesAuthors: Bing-Qiang Qiao, Qiang Yuan, Yi-Qing Guo,Comments: 22 pages, 3 figures, accepted by JCAPSubjects: astro-ph.HECreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
The origin of COSMIC RAYs remains an unresolved fundamental problem in astrophysics. The synergy of multiple observational probes, including the energy spectra, the mass composition, and anisotropy is a viable way to jointly uncover this mystery. In this work, we propose that the energy-dependent of those observables in a wide energy range, from $O(10)$ GeV to ultrahigh energies of $10^{11}$ GeV, share quite a few correlated features, indicating a strong co-evolution which could be a consequence of the underlying origin of different source populations. We decipher these structures with a four-component model, i.e., the ensemble of Galactic sources, a local source close to the solar system, and the ensemble of two extra-galactic source populations. In this scenario, the $O(10^2)$ GV hardening and $O(10)$ TV bump is due to the contribution of the local source, the knee is due to the maximum acceleration energy of protons by the Galactic source population, the second knee is due to the maximum acceleration energy of iron nuclei by Galactic sources, the dip feature between the two knees is due to the appearance of the extra-galactic component, the ankle comes from the transition from one extra-galactic component to the other, and the spectral suppression at the highest energies arises from the acceleration limit of the second extra-galactic component. The transition from Galactic to extra-galactic origin of COSMIC RAYs occurs around $O(10^8)$ GeV, which is smaller than the ankle energy.
[abstract 14 / 37] (score: 3) - Title: X-ray POLARIZATION of reflected thermal emissionAuthors: J. Podgorný, M. Dovčiak, R. Goosmann, F. Marin, L. Marra, G. Matt, A. Różańska, R. Taverna,Comments: 14 pages, 8 figures, accepted for publication in A&ASubjects: astro-ph.HECreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
We compute rest-frame reflection spectra and the corresponding energy-dependent linear POLARIZATION degree and angle for (un)polarized single-temperature blackbody spectra impinging on a partially ionized constant-density optically thick slab. We use a combination of a Monte Carlo simulation that takes into account scattering, absorption, and spectral lines, with a non-LTE radiative transfer pre-computation of the ionization structure of the slab in photo-ionization equilibrium. We discuss the impact of the reflector's ionization and of the incident spectral shape on the obtained energy dependence of POLARIZATION. For isotropic incident intensity and for rather parallel than perpendicular unidirectional illumination with respect to the slab normal direction, despite the presence of highly polarized absorption features and low-polarized spectral lines, an underlying scattering-induced increase of POLARIZATION degree with energy in mid to hard X-rays naturally arises due to multiple Compton-scattering energy shifts. Such re-processing effect is particularly apparent in 2-8 keV for steep incident X-ray spectra reflecting from highly-ionized optically thick media. Integration of the resulting local reflection tables in specific large-scale reflection geometries occurring in X-ray binary systems, including RELATIVISTIC effects, will be presented in a follow-up paper. Nonetheless, we anticipate that the obtained local energy-dependent features will imprint at large distances from the source to the observed X-ray POLARIZATION, and could contribute to the observed increase of total POLARIZATION degree with energy in 2-8 keV in some accreting systems by the IXPE mission.
[abstract 15 / 37] (score: 3) - Title: On the consistency of JET feedback modelling across different astrophysics hydrodynamical codesAuthors: N. Maragkakis, M. A. Bourne, C. Power, F. Huško, A. Ludlow, S. Shabala,Comments: 27 pages, 15 figuresSubjects: astro-ph.GACreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
Active Galactic Nuclei (AGN) feedback is essential in cosmological simulations of galaxy formation, yet its implementation has to rely on subgrid models due to limited resolution. We present a novel subgrid JET-launching method for galaxy formation simulations and implement it in three hydrodynamical codes: the smoothed particle hydrodynamics (SPH) code SWIFT, the moving-mesh code AREPO, and the Eulerian grid code PLUTO. To isolate the impact of hydrodynamical solvers on JET evolution, we compare idealised JETs and their remnants in uniform and stratified media across resolutions and JET parameters. In uniform media, all JETs drive bow shocks, inflate hot lobes, exhibit backflows, and evolve self-similarly. For the parameters explored, SWIFT lobes are shorter, wider, and hotter; AREPO lobes are longer, thinner, and cooler; while PLUTO lobes display complex flows with intermediate characteristics. In stratified media, JETs deviate from self-similar evolution, inflating longer and thinner lobes due to lower external ram pressure. After switch-off, SWIFT JETs evolve into smooth cylindrical bubbles, AREPO JETs produce long filamentary remnants, and PLUTO JETs yield intermediate-length remnants with varying degrees of mixing. Despite such differences, all JETs and remnants have a similar impact on the ambient medium. We conclude that variations in lobe properties between codes emerge even for identical subgrid prescriptions, since the coupling of JET feedback to resolvable scales and the effective resolution depend on the hydrodynamical method. In structure formation simulations, these solver differences are likely subdominant to uncertainties in subgrid modelling and calibration, while averaging over galaxy populations may lessen their impact.
[abstract 16 / 37] (score: 3) - Title: Dynamics of Binary System around a Supermassive Black Hole :Binary Scattering and Eccentric vZLK OscillationsAuthors: Kei-ichi Maeda, Hirotada Okawa,Comments: 25 pages, 23 figuresSubjects: gr-qc astro-ph.GA astro-ph.HECreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
We study the dynamics of a binary orbiting a supermassive BLACK HOLE (SMBH), focusing on both binary scattering in unbound orbits and eccentric von Zeipel-Lidov-Kozai (vZLK) oscillations in bound orbits. The motion is described in a local inertial frame in Kerr spacetime, where tidal effects are encoded in the Riemann curvature. For unbound (parabolic and hyperbolic) orbits, we identify four scattering regimes-adiabatic, tidally affected, chaotic, and disruptive-depending on the binary semi-major axis. As the binary becomes softer, tidal interactions near periapsis lead to strong eccentricity excitation, large changes in the orbital parameters, and eventually chaotic behavior or tidal disruption, with a sensitive dependence on the argument of periapsis. For eccentric bound (elliptic) orbits, the vZLK mechanism differs qualitatively from the standard one, although the $z$-component of the angular momentum in the local inertial frame remains approximately conserved. The evolution proceeds on a dynamical timescale and exhibits step-like changes driven by repeated periapsis passages, which can be interpreted as a sequence of scattering events. We refer to this behavior as scattering-type vZLK oscillations. The rotation of the SMBH also modifies the oscillation profiles, although its effect is less significant than the dependence on the initial orbital parameters. These results suggest a unified picture of periapsis-driven tidal dynamics in galactic nuclei.
[abstract 17 / 37] (score: 3) - Title: Reassessing high-energy emission correlations in GAMMA-RAY BURSTs using a large, homogeneous sample of X-ray afterglowsAuthors: A. A. Vigliano, F. Longo, Ž. Bošnjak,Comments: A&A, acceptedSubjects: astro-ph.HE astro-ph.IMCreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
Gamma-ray bursts (GRBs) show diverse X-ray afterglow light-curves, including breaks and plateaus, whose physical origins remain debated. Previous claims linked high-energy ($E \ge 100$ MeV) detection to X-ray afterglow complexity or plateau incidence, but they were often based on small or heterogeneous samples. We present a large-scale, uniform, model-independent analysis of the complete SWIFT-XRT GRB afterglow catalog, including more than 1400 events. Our automated pipeline performs flare removal and segmented power-law fitting consistently across the sample. We find that both light-curve complexity and plateau incidence are strongly governed by the XRT observation start time, $t_{XRT}$. Apparent correlations between high-energy emission and X-ray morphology arise when $t_{XRT}$ is ignored, but vanish when the sample is stratified or controlled for this variable. X-ray complexity and plateaus are therefore not directly coupled to high-energy detectability, and early X-ray morphology is not predictive of high-energy emission. These results resolve conflicting claims in the literature and show that controlling for $t_{XRT}$ is essential in large-sample GRB studies. The automated pipeline provides a reproducible basis for future analyses of GRB afterglows from SWIFT and upcoming missions such as SVOM, Einstein Probe, and THESEUS.
[abstract 18 / 37] (score: 3) - Title: Strong Constraints on Millisecond Pulsar Injection Spectra from FERMI-LAT Observations of the Galactic CenterAuthors: Jordan Koechler, Pedro De la Torre Luque, Mattia Di Mauro,Comments: 16 Pages, 5 figures, 1 table. Comments are welcome!Subjects: astro-ph.HE hep-phCreated: 2026-05-25; Updated: 2026-05-27; Datestamp: 2026-05-27
Millisecond pulsars (MSPs) are a leading explanation of the Galactic Center excess (GCE) observed in FERMI-LAT data. We constrain this scenario by jointly modeling prompt and inverse-Compton $γ$ rays from MSP-injected $e^\pm$ on the Galactic bulge, using recent FERMI-LAT GCE spectra from state-of-the-art interstellar emission models and data analysis. Current data place strong upper limits on the efficiency ratio $η_e/η_γ$ across broad $e^\pm$ injection scenarios, surpassing those from globular-cluster observations with MAGIC and competitive with projected CTAO sensitivities toward the Galactic bulge.
[abstract 19 / 37] (score: 3) - Title: The Role of Whistler and Ion Cyclotron Waves in Particle Escape from Mirror Modes in the Intracluster MediumAuthors: Petr Ugarov, Francisco Ley, Ellen Zweibel,Comments: 14 pages, 9 figuresSubjects: astro-ph.HE physics.plasm-phCreated: 2026-05-25; Updated: 2026-05-27; Datestamp: 2026-05-27
Electron and ion-cyclotron waves are well known to exist in solar system plasmas but their existence and importance in galaxy clusters is an open question. Guided by numerical simulations, (Ley et al. (2024)) argued that whistlers (electron-cyclotron) and ion-cyclotron (IC) waves are generated by trapped particles in mirror modes in the nonlinear stages of the mirror instability under ICM conditions. Building on this work, we construct a novel particle propagation simulation of the ICM plasma based on the static electroMAGNETic field configuration from the fully kinetic particle-in-cell (PIC) simulation of the nonlinear mirror instability by (Ley et al. (2024)). We study how the trapping rate of particles is related to the secondary waves driven by mirror modes. We observe that secondary whistlers and IC waves enhance trapped particle escape from mirror modes. We measure the particle-wave scattering rate by whistlers and IC waves, demonstrate that the scattering rates and wave amplitudes follow the proportionality relation expected from quasilinear theory, and show the existence of a significant correlation between scattering rates and the excitation of secondary instabilities.
[abstract 20 / 37] (score: 3) - Title: Canonical quantization of massive vector field in Schwarzschild BLACK HOLE backgroundAuthors: Chandra Prakash, Rajesh Karmakar,Comments: 24 pages, 6 figuresSubjects: gr-qcCreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
We perform a first-principles canonical quantization of a massive vector field, often referred to as the Proca field, in a Schwarzschild spacetime background. While scalar, fermionic, and electroMAGNETic fields are well studied in this context, the Proca field requires a more nuanced treatment because of the physical nature of the longitudinal POLARIZATION mode and the constrained dynamics of the field variables. By implementing the Dirac bracket formalism to treat the constraints inherent in the Proca action, we derive a consistent framework for the commutator algebra of creation and annihilation operators. Following this construction, we define the usual Boulware, Unruh, and Hartle-Hawking vacua. Using the Unruh vacuum, we derive and analyze the Hawking spectrum of the Proca field. Furthermore, we numerically evaluate the Proca condensate constructed from the two-point correlation function $\langle A_μ(x) A_ν(x') \rangle$, defined on all three vacuum states. We find that the condensate becomes significant near the boundary of the future horizon. Our results highlight the interplay among the different POLARIZATION modes and the significance of the Proca mass in quantum observables.
[abstract 21 / 37] (score: 2) - Title: Pulsar timing in the Galactic CenterAuthors: Riccardo Della Monica, Ivan de Martino,Comments: 19 pages, 8 figures, 2 tables. Matches version accepted in PRDSubjects: gr-qcCreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
We propose a novel approach which implements the RELATIVISTIC calculations of the photon travel time into a robust timing model for pulsars orbiting supermassive BLACK HOLEs. We demonstrate that timing models relying on the lowest-order (1PN) post-Newtonian approximation can produce significant discrepancies in strong-field configurations, affecting the predicted RELATIVISTIC times of arrival at an Earth-based observatory. We also show how a misestimation of the pulsar parameters can lead to the appearance of phase-dependent residual, which hints at a tremendous constraining power of the binary and intrinsic parameters for timing observations of potential pulsars at the Galactic Center.
[abstract 22 / 37] (score: 2) - Title: Examining the influence of anisotropy on the fundamental mode of nonradial oscillation in neutron stars on a complete general RELATIVISTIC schemeAuthors: José D. V. Arbañil, Gabriel O. Cavalheiro, Victor B. T. Alves, Juan M. Z. Pretel, César O. V. Flores, César H. Lenzi,Comments: 29 pages, 7 figures. To appear in JCAPSubjects: gr-qc astro-ph.HECreated: 2026-05-25; Updated: 2026-05-27; Datestamp: 2026-05-27
The anisotropic influence on the $f$-mode frequency of oscillations and dimensionless tidal deformability of neutron stars is analyzed by employing the nonradial oscillation equations for the complete general relativity frame and tidal deformability equations, which are derived and modified from their standard form to introduce the anisotropic factor. The fluid inside the compact star obeys an equation of state constructed by matching microscopic nuclear and perturbative QCD calculations through a piecewise polytropic interpolating scheme. For the anisotropic profile, we use a local anisotropy which is regular along the whole star and vanishes both at the center and on the star's surface. We show that the \(f\)-mode oscillation frequency and dimensionless tidal deformability are noticeably affected by anisotropy. Finally, we investigate the correlation between the dimensionless tidal deformability inferred from the GW$170817$ event and the anisotropy parameter.
[abstract 23 / 37] (score: 2) - Title: GW231123: Overlapping Gravitational Wave Signals?Authors: Qian Hu, Harsh Narola, Jef Heynen, Mick Wright, John Veitch, Justin Janquart, Chris Van Den Broeck,Comments: 8 pages, 3 figures. Accepted versionSubjects: gr-qc astro-ph.HECreated: 2026-05-21; Updated: 2026-05-27; Datestamp: 2026-05-27
The recently discovered gravitational wave event GW231123 was interpreted as the merger of two BLACK HOLEs with a total mass of 190-265 $M_\odot$, making it the heaviest such merger detected to date. Whilst much of the post-discovery literature has focused on its astrophysical origins, primary analyses have exhibited considerable discrepancies in the measurement of source properties between waveform models, which cannot reliably be reproduced by simulations. Such discrepancies may arise when an unaccounted overlapping signal is present in the data, or from phenomena that produce similar effects, such as gravitational lensing or overlapping noise artifacts. In this work, we analyse GW231123 using a flexible model that allows for two overlapping signals, and find that it is favoured over the isolated signal model with Bayes factors of $\sim 10^2 - 10^{4}$, depending on the waveform model. These values lie within the top few per cent of the background distribution. Similar effects are not observed in GW190521, another high-mass event. Under the overlapping signals model, discrepancies in the measurement of source properties between waveform models are largely mitigated. We also find that neglecting an additional signal in overlapping-signal data can lead to discrepancies in the estimated source properties resembling those reported in GW231123. Although the overlapping signal model provides a higher Bayesian evidence, the astrophysical prior probability of two short signals overlapping is low. However, we find that the two recovered sources show similar properties. This, taken with the higher evidence of the two signal model, suggests that gravitational lensing may provide an alternative explanation.
[abstract 24 / 37] (score: 2) - Title: 3D Dynamics of a PreMAGNETized Gas-puff Z-pinch implosionAuthors: P. Phillips, M. Escalona, P. Retamales, M. Ribeiro, F. Veloso, J. C. Valenzuela,Comments: 13 pages with 14 figuresSubjects: physics.plasm-phCreated: 2026-05-25; Updated: 2026-05-27; Datestamp: 2026-05-27
We present the first simultaneous, spatially-resolved measurement of all three velocity components (radial, azimuthal, and axial) in an annular MAGNETized argon gas-puff Z-pinch, performed using Collective Thomson Scattering along three orthogonal lines of sight from the same scattering volume at each time step. Measurements were carried out on the Llamp{ü}dke{ñ} pulse-power generator (400 kA peak, 200 ns rise time), for applied axial fields ranging from 0.04 to 0.26 T using two coil configurations: a double coil with negligible initial radial field at the probed plane ($z = 8$ mm), and a single coil that imposes a finite initial radial field. Three principal results are reported. First, the axial velocity component, which had not previously been measured experimentally in this configuration, reaches 60--70~km\,s$^{-1}$ near the axis at low applied fields ($B_{z0} < 0.1$ T) and is suppressed to within $\pm 20$~km\,s$^{-1}$ for stronger applied fields, in correlation with the reduction of the zippering angle, with direct implications for the implosion energy balance. Second, the self-generated rotation extends across the full plasma diameter, not only at the periphery, and the diametrical profile of the azimuthal velocity decreases toward the axis with an exponential-like shape consistent with the underlying current density distribution; this feature was not visible in previous edge-localized measurements. Third, rotation persists in the double-coil case ($B_{r0} \approx 0$) and is enhanced in the single-coil case (finite $B_{r0}$), supporting the interpretation that $B_r$ develops self-consistently during the implosion and drives the rotation through a $J_z \times B_r$ torque. These results constrain the role of each MAGNETic-field component and motivate direct measurement of $B_r$ and the current density distribution as the next step.
[abstract 25 / 37] (score: 2) - Title: Dymnikova Black Holes in Unimodular Gravity: Maxwell Sources and Vacuum ContributionsAuthors: G. Alencar, V. H. U. Borralho,Comments:Subjects: gr-qcCreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
In this work, we investigate the Dymnikova regular BLACK HOLE within the framework of unimodular gravity, emphasizing the role of the effective vacuum sector in the regularization of the geometry. By allowing a controlled violation of the covariant conservation of the energy--momentum tensor, the cosmological contribution emerges dynamically as a radial-dependent function, $Λ=Λ(r)$. We first reinterpret the Dymnikova spacetime as a charged configuration supported by nonlinear electrodynamics and derive the corresponding electric and MAGNETic sources. Subsequently, we demonstrate that the same geometry can be consistently generated by standard Maxwell electrodynamics in unimodular gravity. In this construction, the resulting electric field is everywhere regular and corresponds to a localized charge distribution with vanishing asymptotic charge, indicating that the spacetime does not behave as an asymptotically charged object.
[abstract 26 / 37] (score: 2) - Title: A Compression-Directional Entropic Stress Method for Shock-Regularized Compressible FlowAuthors: Bonan Xu, Chihyung Wen, Peixu Guo,Comments:Subjects: physics.flu-dynCreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
We introduce the Compression-Directional Entropic Stress (CoDeS) method inspired by information geometric regularization. CoDeS replaces scalar multidimensional entropic pressure with a tensor stress aligned with the principal directions of compression. The stress has the form $\boldsymbolΠ_Σ=σ\boldsymbol{M}$, where $σ$ is obtained from a modified-Helmholtz equation and $\boldsymbol{M}$ is constructed from the compressive eigenspace of the symmetric velocity-gradient tensor. The source is gated by volumetric and principal-strain compression, so the regularization vanishes in smooth expansion, rigid-body rotation, and ideal contacts, while recovering the compressive one-dimensional IGR mechanism at planar shocks. The same tensor stress is used in the conservative momentum flux and the stress-work energy flux. CoDeS is tested on one-, two-, and three-dimensional problems including smooth expansion, double rarefaction, the Sod shock tube, multidimensional Riemann flow, a viscous shock tube, a two-fluid triple point, a Mach-3 slot JET, and a supersonic Taylor--Green vortex. The results show that CoDeS remains inactive in expansive and contact regions, supplies localized stress at shocks, and concentrates regularization along compressive wave structures while remaining weak in shear- and vorticity-dominated regions. At matched resolutions, the three-dimensional Taylor--Green results are comparable to or more energetic than seventh-order WENO/TENO references. These results indicate that CoDeS provides a compression-selective shock regularization compatible with high-order finite-volume resolution of contacts, interfaces, shear layers, and vortical structures. All the code, case settings, and code for plotting figures of this paper are available at https://github.com/xubonan/code\_for\_CoDeS.
[abstract 27 / 37] (score: 2) - Title: Continuous coherent spin-frequency metrology in storage rings via resonant beam-driven detectionAuthors: Younggeun Kim, Themis Bowcock, Dmitry Budker, Giovanni Cantatore, Hooman Davoudiasl, Dmitry Denisov, Abhay Deshpande, Wolfram Fischer, Selcuk Haciomeroglu, Haixin Huang, David Kawall, Alexander Keshavarzi, On Kim, Ivan Koop, Valeri Lebedev, Jonathan Lee, William M. Morse, Cenap Ozben, Vincent Schoefer, Yannis K. Semertzidis, Eleftherios Skordis, Edward Stephenson, Vladimir Tishchenko, Nicholaos Tsoupas, Graziano Venanzoni, Joost Vossebeld, Peter Winter,Comments: 32 pages, 3 figures. v2 includes corrected author list/metadata and minor revisions to the manuscriptSubjects: hep-exCreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
Precision measurements in storage rings are increasingly limited by the ability to monitor collective spin dynamics coherently over long time scales. Existing polarimetry techniques rely on destructive scattering processes that preclude continuous, non-intercepting tracking of spin evolution and constrain both statistical sensitivity and systematic control. Here we introduce a non-destructive, phase-coherent polarimetry method in which the stored beam POLARIZATION is treated as a continuous dynamical observable rather than a quantity inferred from scattering events. Spin-dependent electroMAGNETic fields generated by a polarized RELATIVISTIC beam establish a symmetry-selected differential signal on pickup electrodes. This signal is transduced into a narrowband phase modulation of a high-Q resonator interrogated with a coherent probe, while dominant charge-induced backgrounds are rejected through geometric symmetry, helicity reversal, and synchronous demodulation. Controlled spin precession (spin-wheel operation) provides a stable phase reference enabling phase-coherent detection of slow spin evolution. Combined with optimized lattice symmetry and beam cooling, this approach can substantially extend the usable spin coherence time, with values approaching 10^5 s appearing realistic within existing accelerator technology. The resulting readout supports optimal slope-based estimation with T^{-3/2} statistical scaling while eliminating the efficiency penalties inherent to scattering-based polarimetry. For storage-ring EDM experiments, this combination enables sensitivity approaching the level expected within the Standard Model. More broadly, the method establishes a general phase-coherent architecture for collective spin measurements in storage rings, adapting resonant sensing concepts from axion dark-matter searches to charged-particle precision experiments.
[abstract 28 / 37] (score: 2) - Title: The Evolution of Cataclysmic Variables Under Various Magnetic Braking PrescriptionsAuthors: Wen-Shi Tang, Xiang-Dong Li, Zhe Cui, Zhu-Ling Deng, Wei-Min Gu,Comments: 15 pages, 7 figures, accepted by ApJ. The revised version only modifies the title in arxiv by adding 'Braking Prescriptions' at the endSubjects: astro-ph.HECreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
Recent studies revealed discrepancies between observations and the predictions of the standard MAGNETic braking (MB). Although alternative models have been broadly discussed in neutron star binaries, they have not been systematically tested in cataclysmic variables (CVs). In this work, we investigate the performance of four MB models in CVs: the standard MB, the Convection And Rotation Boosted (CARB) model, the $τ$-boosted model, and the saturated, boosted, and disrupted (SBD) model. We find that both the CARB and $τ$-boosted models appear too strong so that it fails to reproduce the location of the period gap in CVs, indicating that they are not appropriate for CVs. Furthermore, we present a comparison between the standard MB and the SBD models. Compared with the standard model, although the SBD model can better reproduce some observational features, it also exacerbates certain discrepancies between theory and observations. We also find that different prescriptions for the convective turnover timescale have a significant impact on the results in the non-standard MBs. Finally, we discuss the impact of the SBD model on the formation and evolution of AM CVn.
[abstract 29 / 37] (score: 2) - Title: Cosmic Ray Feedback in Galactic Disks: Star Formation, Cosmic Ray Transport, and Multiphase Outflows in \tigresspp\ SimulationsAuthors: Chang-Goo Kim, Lucia Armillotta, Eve C. Ostriker, Sanghyuk Moon, Lachlan Lancaster, Jeong-Gyu Kim, Nora B. Linzer, Ronan N. Hix,Comments: resubmitted to ApJ after minor revisionSubjects: astro-ph.GACreated: 2026-05-25; Updated: 2026-05-27; Datestamp: 2026-05-27
We present new simulations of local star-forming disks that self-consistently evolve COSMIC RAYs (CRs) and multiphase gas using TIGRESS++. To isolate the role of CRs, we conduct paired simulations under solar-neighborhood conditions: a MAGNETohydrodynamics (MHD) model following the standard TIGRESS-classic framework with FUV heating and SUPERNOVA (SN) feedback from star clusters formed via gravitational collapse; and a CRMHD model in which an additional 10% of each SN's energy is injected as CRs. These CRs are transported anisotropically along MAGNETic field lines via a two-moment solver, with the CR scattering rate set by balancing Alfven-wave growth and damping based on the self-confinement paradigm. The CRMHD model develops a characteristic two-zone vertical CR profile: uniform pressure in the diffusion-dominated, high-density midplane gas, and an exponential atmosphere shaped primarily by advection and streaming in low-density extraplanar gas. The CR pressure is comparable to the total thermal gas pressure in the midplane, but is too uniform to affect gas dynamics, leaving SFRs unchanged. In contrast, the vertical CR pressure gradient at |z| > 1 kpc accelerates warm outflowing gas, resulting in an approximately 4 times higher mass loading factor than in the MHD model. CR-gas interactions increase CR energy near the midplane through compressional work, while CR streaming heats low-density warm-hot gas. TIGRESS++ opens a path toward investigating CR transport and CR-regulated ISM and outflow dynamics at high resolution across diverse galactic environments.
[abstract 30 / 37] (score: 2) - Title: Nuclear Physics of Binary Neutron Star MergersAuthors: Armen Sedrakian,Comments: Invited review for Encyclopedia of Nuclear Physics, 43 pages, 11 figures. Comments are welcomeSubjects: astro-ph.HE astro-ph.SR nucl-thCreated: 2026-05-25; Updated: 2026-05-27; Datestamp: 2026-05-27
Binary neutron star mergers provide a unique laboratory for studying matter under conditions that cannot be reproduced in terrestrial experiments. They probe dense matter at supranuclear density, finite temperature, rapid rotation, strong gravity, and extreme neutron excess, while producing observable signals in gravitational waves, electroMAGNETic radiation, and, in principle, neutrinos. This review focuses on the nuclear physics of binary neutron star mergers. We discuss the dense-matter equation of state (EoS), the inspiral and merger dynamics, the structure and lifetime of the post-merger remnant, transport and dissipative processes, weak interactions and neutrino transport, and the production of heavy elements through $r$-process nucleosynthesis. Particular emphasis is placed on the connection between microscopic physics and multimessenger observables, including tidal deformability, post-merger gravitational-wave spectra, kilonova light curves, short GAMMA-RAY BURSTs, and afterglows. We also review how observations of events such as GW170817, together with neutron star mass and radius measurements, laboratory nuclear experiments, and theoretical many-body calculations, constrain the EoS and the composition of dense matter. The goal is to summarize the current understanding of how nuclear physics controls the dynamics and observable signatures of binary neutron star mergers, and to identify the open questions that future multimessenger observations and improved nuclear theory will address.
[abstract 31 / 37] (score: 2) - Title: Equatorial Circular Motion of Charged Test Particles in a Weakly Magnetized Taub--NUT BackgroundAuthors: B. J. Bansawang, Tasrief Surungan,Comments: 10 pages, 18 figuresSubjects: gr-qcCreated: 2026-05-25; Updated: 2026-05-27; Datestamp: 2026-05-27
We study circular motion of charged test particles on the equatorial slice of a Taub--NUT BLACK HOLE with Manko--Ruiz parameter $C$, immersed in a weak external MAGNETic field introduced via Wald's prescription. Because the Taub--NUT metric is not reflection-symmetric about the equator once $l\neq 0$, generic charged orbits lie on cones $x=\cosθ\neq 0$ rather than on the equatorial plane. We therefore analyse \emph{constrained} circular orbits obtained by imposing $x=\dot x=0$, and we exhibit in closed form the residual angular constraint that a fully self-consistent orbit would have to satisfy. Within this scope we derive the circularity and marginal-stability conditions and study how $B$ and $C$ shift the ISCO radius for prograde and retrograde branches. Increasing $B$ monotonically decreases $r_{\mathrm{ISCO}}$; the sign of the particle charge splits the two branches, with the ordering reversed between prograde and retrograde motion; and $C$ contributes only subleading corrections. The extension to self-consistent conical orbits is the natural direction for follow-up work.
[abstract 32 / 37] (score: 2) - Title: A Comparative Analysis of Clustering Algorithms for Characterizing Surface Ocean Variability in the Western MediterraneanAuthors: Victor Rodriguez-Mendez, Enrico Ser-Giacomi, Jose J. Ramasco, Cristobal Lopez, Emilio Hernandez-Garcia,Comments: 25 pages, 12 figuresSubjects: physics.ao-phCreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
Understanding regional dynamical structures in the sea is fundamental to characterize energy transfer and transport properties, with implications in physical and biogeochemical modeling and characterization. In this work, we study the potential of clustering techniques to identify regional patterns, persistent or recurrent configurations, out of daily snapshots of sea surface temperature and kinetic energy in a region of the western Mediterranean Sea. From the methodological perspective, we use different clustering techniques: K-means, Self-Organizing Maps and InfoMap to verify if the patterns found are coherent across methods. Our results show that K-means and Self-Organizing Maps consistently delineate four distinct clusters of sea surface temperature configurations, aligned with the seasons even after removing the annual cycle, which indicates the persistence of seasonal structures beyond a mean effect in the temperature field. The study of surface kinetic energy, characterized by higher spatial and temporal variability, reveals more complex circulation regimes. While K-means and Self-Organizing Maps provide a robust and convergent classification of the dominant large-scale energy patterns, InfoMap uncovers finer-scale features such as localized JETs and eddies. InfoMap, in particular, provides a complementary perspective to the partition-based methods, validating subtle yet significant hydrodynamic structures and acting as an anomaly detector for extreme events.
[abstract 33 / 37] (score: 2) - Title: Interaction-Phase Dynamics and Spectral Organization in Damped Higher-Order Nonlinear Schrödinger ModelsAuthors: C. M. Schober,Comments: 30 pages, 26 figuresSubjects: nlin.PSCreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
We investigate the dynamical mechanisms underlying the contrasting nonlinear Floquet spectral evolutions observed in viscous and nonlinear mean-flow damped higher-order nonlinear Schr"odinger systems. Motivated by the persistent organized Floquet-band structure under nonlinear mean-flow damping and the repeated Floquet band RECONNECTion observed under viscous damping, we derive a reduced five-mode carrier-sideband truncation and reformulate the dynamics in amplitude-phase variables to isolate the dominant interaction phases associated with the principal four-wave interaction products. Within this framework, viscous damping acts primarily modewise and does not directly modify the leading interaction-phase dynamics. By contrast, nonlinear mean-flow damping contributes directly to the interaction-phase evolution through interaction-dependent dissipative corrections. In the carrier-sideband regime, these corrections generate terms of the form $-κ_j \sin(ψ_j)$, introducing dissipative feedback into the dominant carrier-sideband interaction dynamics. To interpret the resulting interaction-phase evolution, we examine recurrent finite-gap NLS benchmark solutions whose modulation dynamics are independently understood. These benchmarks show that substantial interaction-phase evolution and localized restructuring may occur even within organized quasiperiodic dynamics possessing invariant Floquet spectral structure. Numerical diagnostics show that the nonlinear mean-flow damped system exhibits persistent recurrent carrier-sideband focusing dynamics together with organized Floquet evolution despite substantial interaction-phase restructuring, whereas the viscous system exhibits progressively diffuse modulation dynamics together with repeated Floquet reconfiguration and weakening persistence of the recurrent carrier-sideband interaction structure.
[abstract 34 / 37] (score: 2) - Title: ITER ECE front-end design, alignment and in-situ calibrationAuthors: Saeid Houshmandyar, W. L. Rowan, J. P. Ziegel, A. Ouroua,Comments:Subjects: physics.plasm-phCreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
The electron cyclotron emission (ECE) diagnostics suite at ITER utilizes a front-end quasi-optical (QO) system whose design is fundamentally constrained by a field-stop concept. The field-stop defines the Gaussian beam variation throughout the optical system and within the plasma, thereby setting the ECE sampling volume and spatial resolution. An in-situ hot calibration source, optimized using Gaussian beam transmission criteria, provides independent and absolute electron temperature measurements. The QO system extends beyond the front-end to include the POLARIZATION splitter unit (PSU), transmission lines, and switchyard, forming an integrated optical path to the ECE instruments. Misalignment between the front-end and PSU reduces the effective field-stop size, degrading spatial resolution and measurement fidelity. The oblique ECE view, a key feature of the ITER design, enhances sensitivity to non-thermal electron populations and complements the diagnosis of neoclassical tearing modes. Integrated QO design and plasma physics understanding are essential for reliable ITER ECE measurements.
[abstract 35 / 37] (score: 2) - Title: GWTC-5.0: Observations from the Second Part of the Fourth LIGO-Virgo-KAGRA Observing Run and Updates to the Gravitational-Wave Transient CatalogAuthors: The LIGO Scientific Collaboration, the Virgo Collaboration, the KAGRA Collaboration,Comments: main paper: 30 pages, 8 figures; total with appendices: 43 pages, 9 figures. This article draws heavily from the corresponding GWTC-4 article, arXiv:2508.18082Subjects: gr-qc astro-ph.HECreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
Version 5.0 of the Gravitational-Wave Transient Catalog (GWTC-5.0) adds new candidates detected by the LIGO, Virgo, and KAGRA observatories through the second part of the fourth observing run (O4b: 2024 April 10 15:00:00 to 2025 January 28 17:00:00 UTC) and a preceding engineering run. In these new data, we find 150 compact binary coalescence candidates that are identified by at least one of our search algorithms with a probability of astrophysical origin $p_\mathrm{astro} \geq 0.5$ and that are not vetoed during event validation. We also provide detailed source property measurements for 103 of these that have a false-alarm rate < 1yr$^{-1}$. Based on the inferred component masses, these candidates are consistent with signals from binary BLACK HOLEs without binary neutron stars or neutron star-BLACK HOLE binaries. Median inferred component masses of binary BLACK HOLEs in the catalog now range from 5.14$M_\odot$ (GW241109_115924) to 70$M_\odot$ (GW241116_151753). For the first time, we have discovered binary BLACK HOLE signals with network signal-to-noise ratio exceeding 70, GW250114_082203, enabling high-fidelity studies of the astrophysical properties of these systems and test of general relativity. Together with updated 139 candidates up to the first part of the fourth observing run, this brings the total number of transients in the cumulative GWTC to 390, which fulfills the criteria of $p_\mathrm{astro} \geq 0.5$, further expanding the size of the catalog and our view of the gravitational-wave Universe.
[abstract 36 / 37] (score: 2) - Title: GWTC-5.0: Population Properties of Merging Compact BinariesAuthors: The LIGO Scientific Collaboration, the Virgo Collaboration, the KAGRA Collaboration,Comments: Abstract truncated in Arxiv metadata. The paper appendices draw heavily from the corresponding GWTC-4 article, arXiv:2508.18083Subjects: astro-ph.HE gr-qcCreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
We present the population properties of merging compact binaries inferred using 267 mergers from the cumulative Gravitational-Wave Transient Catalog 5.0. As this data set contains no new sources with a neutron star, we primarily focus on the properties of the binary BLACK HOLE mergers. We infer the merger rate of binary BLACK HOLEs with component masses between $2.5\,\mathrm{M}_\odot $ and $200\,\mathrm{M}_\odot $ to be $27.5\text{--} 49.4 \, \mathrm{Gpc}^{-3}\,\mathrm{yr}^{-1}$ (all intervals at $90\%$ credible levels) at redshift $z = 0.2$. We find evidence for a subpopulation of binary BLACK HOLE mergers that host a rapidly spinning BLACK HOLE (dimensionless spins $χ\sim 0.7$), consistent with signatures of hierarchical mergers. We find that these occur at two mass scales, the first at primary masses $\sim 10$--$20\,\mathrm{M}_\odot $ and the second above $\sim 45\,\mathrm{M}_\odot $, and we estimate their total rate at $z=0.2$ to be $0.2\text{--} 3.11 \, {\rm Gpc}^{-3} {\rm yr}^{-1}$. We infer that, above $40\,\mathrm{M}_\odot $, the mass distribution of the less massive (secondary) BLACK HOLE declines more steeply than that of the more massive (primary) one. This is consistent with a flatter mass-ratio distribution and indicates the prevalence of unequal-mass binaries with large primary masses. We find evidence for two features in the BLACK HOLE mass spectrum: a peak around $10\,\mathrm{M}_\odot $ and a change of slope at around $35\,\mathrm{M}_\odot $. Black holes of $\sim 35\,\mathrm{M}_\odot $ pair preferentially with companions of similar mass. Additionally, we find that the effective inspiral spin distribution of binary BLACK HOLEs is asymmetric about zero, based on which we infer that at least $9 \%$ of mergers occur in channels with some preference for spin-orbit alignment. We find evidence that...
[abstract 37 / 37] (score: 2) - Title: Strong-lensing degeneracies of BLACK HOLEs embedded in self-interacting scalar field DARK MATTER halosAuthors: Mohsen Fathi, Gabriel Gómez,Comments: 19 pages, 10 figures, 6 tablesSubjects: gr-qc astro-ph.CO astro-ph.HECreated: 2026-05-26; Updated: 2026-05-27; Datestamp: 2026-05-27
In this paper, we explore the strong gravitational lensing properties of BLACK HOLEs embedded in self-interacting scalar field DARK MATTER halos, together with NFW-type configurations for comparison. The corresponding spacetime geometry is reconstructed numerically through the Einstein cluster formalism, allowing us to study how the surrounding DARK MATTER distribution affects the propagation of photons near the BLACK HOLE. We first analyze the effective function governing photon trajectories and calculate the corresponding photon sphere radius and critical impact parameter. We then investigate different strong-lensing observables, including RELATIVISTIC Einstein rings, finite-order image positions, image separations, magnifications, and time delays, with particular attention to the supermassive BLACK HOLEs M87* and Sgr A*. Our results show that the considered halo configurations produce only small deviations with respect to the Schwarzschild case, typically at the level of $\mathcal{O}(10^{-3})$ or smaller, leading to a strong observational degeneracy among the models. Nevertheless, small but systematic differences remain present, especially in the time delay between RELATIVISTIC images, which provides the clearest amplification of the halo-induced corrections for very massive BLACK HOLEs. These results suggest that, although standard strong-lensing observables remain highly robust against the considered halo environments, time-domain signatures may offer a more promising way to probe the effect of DARK MATTER surrounding BLACK HOLEs.
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