Current date: 2026-06-18
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Scoring abstracts
Number of records retrieved: 692
Keyword score statistics
score 10 -- 1 abstracts
score 9 -- 1 abstracts
score 8 -- 3 abstracts
score 7 -- 2 abstracts
score 5 -- 2 abstracts
score 4 -- 6 abstracts
score 3 -- 6 abstracts
score 2 -- 12 abstracts
in total -- 33 abstracts
Articles that appeared on 2026-06-18
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[abstract 1 / 33] Wow! (score: 10)
- Title: GRMHD and GRRT Simulations of Black Hole Accretion: Flares, Precession, and Complex SpacetimesAuthors: Hong-Xuan Jiang,Comments: PhD ThesisSubjects: astro-ph.HE gr-qcCreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
This dissertation studies the electroMAGNETic signatures of accreting supermassive BLACK HOLEs using general RELATIVISTIC MAGNETohydrodynamic simulations and covariant radiative-transfer calculations. It develops a unified numerical framework for modeling black-hole accretion, JET launching, flaring activity, and multi-band variability in Kerr, non-Kerr, and binary black-hole spacetimes. For isolated Kerr BLACK HOLEs, I investigate how MAGNETic-field geometry affects accretion dynamics and transient emission. Multi-loop MAGNETic configurations naturally produce RECONNECTion events and flux-rope structures that can power near-infrared flares from Sagittarius A*, while the evolving optical depth of expanding plasma explains delayed millimeter emission. I also show that in tilted MAGNETically arrested disks, MAGNETic torques can drive retrograde disk and JET precession. The dissertation then applies the same framework to more complex spacetimes. Simulations of accretion onto regular loop-quantum BLACK HOLEs show that quantum-gravity corrections can modify photon-ring size, POLARIZATION structure, and JET power, leading to observational constraints from Event Horizon Telescope data. Finally, simulations of supermassive binary BLACK HOLEs in time-dependent spacetimes reveal how gravitational self-lensing, shock activity, and spin-orbit coupling shape multi-wavelength light curves and JET precession. Together, these results connect RELATIVISTIC plasma dynamics with current and future observations of black-hole systems.
[abstract 2 / 33] Wow! (score: 9) - Title: ElectroMAGNETic Signatures of Supermassive Binary Black Holes: Synchrotron, Self-Lensing Flares, and Jet PrecessionAuthors: Hong-Xuan Jiang, Xinyu Li, Jing-Ze Xia, Yosuke Mizuno, Ziri Younsi, Christian M. Fromm,Comments: 22 pages, 16 figures, accepted by ApJSubjects: astro-ph.HECreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
The recent evidence for a nanohertz gravitational wave background from Pulsar Timing Arrays highlights the urgent need to identify electroMAGNETic counterparts to supermassive binary BLACK HOLEs. Here, we perform global 3D general RELATIVISTIC MAGNETohydrodynamic (GRMHD) simulations of a secondary BLACK HOLE (mass ratio $q=0.1$) interacting with a Magnetically Arrested Disk around a primary BLACK HOLE using a time-dependent superposed Kerr-Schild metric and post-processed general RELATIVISTIC radiation transfer calculations based on thermal electron distribution function (eDF). We explore three orbital configurations: a vertical impact orbit, a coplanar embedded orbit, and a high-spin, eccentric, inclined scenario. Despite clear orbital periodicity and recurrent shock formation, the thermal SYNCHROTRON light curves frequently lack expected shock-induced flares. In vertical impacts, shock brightenings are typically sub-dominant to the stochastic MAD variability of the primary BLACK HOLE, unless viewed at specific alignment phases. Conversely, coplanar orbits produce distinctive, rapid flares driven by gravitational self-lensing. We identify a frequency-dependent emission hierarchy: the primary BLACK HOLE dominates sub-millimeter flux, while the secondary dominates near-infrared emission due to higher electron temperatures in thermal eDF. Finally, spin-orbit coupling drives Lense-Thirring precession, yielding twisted, wobbling JETs that following the tilt and precession of the primary BH. Crucially, we show that intrinsic MAD turbulence can easily mask shock-induced radio flares, making self-lensing flares a more reliable electroMAGNETic counterpart candidate for supermassive binary BLACK HOLEs.
[abstract 3 / 33] Wow! (score: 8) - Title: A self-consistent explanation of the MeV line in GRB 221009A unveils a dense circum-stellar mediumAuthors: O. S. Salafia, A. Celotti, E. Sobacchi, L. Nava, G. Oganesyan, G. Ghirlanda, S. Boula, M. E. Ravasio, G. Ghisellini,Comments: 20 pages, 9 figures. Final version accepted for publication on A&ASubjects: astro-ph.HECreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
GRB~221009A has been the brightest GAMMA-RAY BURST (GRB) observed to date, and its afterglow has been characterized with unprecedented detail at TeV energies by LHAASO. Quite puzzlingly, it is also the most energetic GRB known. Among the riddles posed by this mysterious source, however, the sheer energetics are hardly the most intriguing: an unprecedented emission line at around 10 MeV has been uncovered by a detailed spectral analysis of FERMI/GBM data immediately following the brightest peak in the GRB prompt emission and the peak of the TeV afterglow. The temporal evolution of the line properties can be explained as high-latitude emission from a geometrically thin, RELATIVISTICally expanding shell where annihilation of a large number of electron-positron pairs took place. We show that this interpretation yields stringent constraints on the properties of such shell, that point to a process that happens at radii typical of external shocks. We then demonstrate that the shell could have been the blastwave associated with the GRB precursor, with the line arising after pair loading of such blastwave as it was illuminated by the bright and hard radiation of the GRB. The scenario, which also explains the abrupt initial rise of the LHAASO afterglow, requires the progenitor of the GRB to have been surrounded by a circum-stellar medium (CSM) extending out to a few 10^15 cm, with a density 10^8-10^9 cm-3 reminiscent of those found in Type IIn SUPERNOVAe. The consequences of such a CSM on the dynamics and emission of the external shock are yet to be fully explored. If future, more detailed work will confirm the compatibility of the GRB 221009A afterglow with our scenario, this will provide a precious clue to the nature of the progenitor of this peculiar GRB, which could also be present in other bursts that feature a long quiescence followed by a bright emission episode with a hard spectrum.
[abstract 4 / 33] Wow! (score: 8) - Title: A VLBA-resolved Jet Associated with Super-Eddington Accretion in a Radio-loud Quasar at $z=3.4$Authors: Sakiko Obuchi, Ingyin Zaw, Kazuhiro Hada, Kohei Ichikawa, Joseph D. Gelfand,Comments: 11 pages, 5 figures, accepted for publication in ApJLSubjects: astro-ph.GA astro-ph.HECreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
We report the detailed JET properties of eROSITA Final Equatorial Depth Survey (eFEDS) J084222.9+001000 (hereafter ID830), a radio-loud super-Eddington QUASAR at $z=3.4351$, revealed by Very Long Baseline Array (VLBA) observations at 1.6 GHz, 4.9 GHz, and 8.2 GHz. Thanks to the high spatial resolution of the VLBA, we successfully resolve a parsec-scale core-JET structure of ID830, and find a well-collimated JET extending over $\approx 745$ pc, making it the most distant and one of the very few currently known radio-loud QUASARs with a resolved JET associated with super-Eddington accretion. The physical scale and evolutionary track of ID830 differs markedly from the low-$z$ analogues, such as nearby radio-luminous high-Eddington narrow-line Seyfert 1 galaxies, suggesting that this source represents a distinct high-$z$ population compared to previously known samples, with important implications for AGN feedback in early galaxy evolution. We also find that the JET has a RELATIVISTIC speed of $v \gtrsim 0.19c$ and a modest viewing angle of $ϕ\lesssim 79^\circ$ to the line of sight, although its emission is not significantly Doppler-boosted ($δ\sim 1$). This provides the first evidence that such a RELATIVISTIC and collimated JET can be produced over several hundred parsecs in the super-Eddington phase, lasting for at least $10^{3\text{-}4}$ yr. Our results call for further theoretical and numerical studies to understand the physical processes required to sustain such large-scale collimation in super-Eddington accretion, which remains a missing piece.
[abstract 5 / 33] Wow! (score: 8) - Title: 2D MAGNETohydrodynamic JET simulations: properties of recollimation shocksAuthors: Stella Boula, Fabrizio Tavecchio, Gianluigi Bodo, Nektarios Vlahakis, Paolo Coppi,Comments: 18 pages, 21 figures, 2 tables, submitted in A&ASubjects: astro-ph.HECreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
Recollimation shocks are a frequent outcome in overpressured RELATIVISTIC JETs and are crucial for interpreting stationary features in Active Galactic Nuclei. The precise influence of MAGNETic fields on JET stability, energy dissipation, and variability remains debated, particularly as different field configurations can significantly alter shock properties and the onset of fluid instabilities. We perform a study of 2D axisymmetric RMHD JETs to quantify how the ambient density contrast ($ν$), pressure ratio ($P$), MAGNETization ($σ$), and MAGNETic pitch parameter ($α$) govern the formation and strength of the first recollimation shock. We also assess how these parameters create the local geometric conditions favorable for the centrifugal instability (CFI), utilizing linear theory as a diagnostic. We find that the JET's global geometry is affected by the MAGNETic pressure. The recollimation distance decreases monotonically with increasing MAGNETization $σ$, as increased MAGNETic forces immediately limit JET expansion. Remarkably, in the MAGNETically dominated regime, the ratio of the MAGNETized recollimation distance ($z_{\rm MHD}$) to its purely hydrodynamic counterpart ($z_{\rm HD}$) converges onto a power-law scaling, $z_{MHD}/z_{HD} \propto (B_0^2/P_{ext})^{-1/3}$, where $B_0$ the initial MAGNETic field and $P_{ext}$ the external pressure. Jets with high density contrast relative to the ambient medium or high internal pressure further enhance field compression. Furthermore, synthetic SYNCHROTRON maps show that a dominant toroidal field yields highly boosted, localized emission knots, whereas a strong poloidal field creates a diffuse profile and shifts the recollimation zone downstream. Regions susceptible to CFI are determined primarily by the local $σ_{\text{tor}}/Γ^2$ profile and streamline curvature created during recollimation.
[abstract 6 / 33] Wow! (score: 7) - Title: Predicting Multiwavelength Emission Associated with X-Ray Flares and Extended Emission of Gamma-Ray BurstsAuthors: Riki Matsui, Shigeo S. Kimura, Kohta Murase, Bing Theodore Zhang,Comments: 16 pages, 7 Figures, 3 tables. Updated title and minor revisionsSubjects: astro-ph.HECreated: 2026-06-12; Updated: 2026-06-18; Datestamp: 2026-06-18
Gamma-ray bursts (GRBs) are one of the most extreme transients in the universe, but their explosion and emission mechanism remains unclear. To investigate the nature of GRB JETs, here we focus on X-ray flares (XFs) and extended emissions (EEs), which are X-ray emissions that occur 100 to 1000 seconds after the main burst. They can be observed by recently developed multi-wavelength facilities. In this paper, we calculate emissions across multi-wavelengths associated with XFs and EEs under the hypothesis that XFs and EEs are optically-thin SYNCHROTRON emissions from nonthermal electrons in RELATIVISTIC JETs. Considering ranges of the dissipation radius $r_{\rm diss}$ and the Lorentz factor $Γ$ of the JET, we determine the parameter space in which a detectable emission can be produced at each wavelength. We found that simultaneous ultraviolet and very-high-energy gamma-ray emission associated with XFs or EEs can be detected by SWIFT/UVOT, SVOM/VT, and CTAO approximately every three years. The detection and non-detection rates for each detector are key to determining the uncertain yet essential values necessary for understanding the physics of GRB JETs.
[abstract 7 / 33] Wow! (score: 7) - Title: Emergence of cyclic flux eruptions in kinetic simulations of MAGNETized spherical accretion onto a Schwarzschild BLACK HOLEAuthors: Enzo Figueiredo, John Mehlhaff, Adrien Soudais, Benoît Cerutti,Comments: 12 pages, 9 figures, accepted in A&ASubjects: astro-ph.HECreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
The dynamics of BLACK HOLE MAGNETospheres critically depend on the BLACK HOLE spin and on the structure of the accretion flow. In the limit of a Schwarzschild BLACK HOLE immersed in a zero-net angular momentum flow, accretion is spherical. However, in the presence of a large-scale vertical MAGNETic field, the classical Bondi accretion model is significantly altered. The frozen-in field is stretched radially as the plasma is pulled inward by gravity. This continues until the restoring force from the MAGNETic tension suddenly expels the material and resets the field, allowing a new cycle to begin. Although this scenario has been well depicted in previous studies, it remains incomplete as the issues of dissipation and particle acceleration are not yet fully resolved. In this work, we aim to revisit these issues with a first-principles kinetic plasma model. We perform two-dimensional global general RELATIVISTIC particle-in-cell simulations of MAGNETized spherical accretion onto a Schwarzschild BLACK HOLE, for both pair and electron-ion plasmas. The simulations are evolved over long timescales to capture multiple flux eruption events and establish a quasi-steady state. For each accretion cycle, we find that the system goes through three main stages: (i) an ideal advection phase where MAGNETic flux through the horizon increases quasi-linearly with time; (ii) a RECONNECTion-regulated phase where the net increase of the flux is slowed down by intermittent RECONNECTion events near the horizon; and (iii) a flaring phase when a major, large-scale RECONNECTion event expels the flux, leading to efficient particle acceleration. The emergence of large-amplitude quasi-periodic flux eruptions and concomitant particle acceleration is reminiscent of Sgr A* flaring activity. This phenomenon could also be applicable to quiescent BLACK HOLEs, especially isolated BLACK HOLEs accreting the interstellar medium.
[abstract 8 / 33] Yes (score: 5) - Title: Open Data from LIGO, Virgo, and KAGRA through the Second Part of the Fourth Observing RunAuthors: 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, F. Dosopoulou, M. Drago, J. C. Driggers, M. Dubois, R. S. Dumbreck, U. Dupletsa, D. D'Urso, P. Dutta Roy, H. Duval, P. -A. Duverne, 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. Fontinele-Nunes, C. Foo, B. Fornal, P. W. F. Forsyth, A. Fragkos, N. Franchini, A. Franco-Ordovas, F. Frappez, F. Frasconi, J. P. Freed, Z. Frei, A. Freise, O. Freitas, R. Frey, W. Frischhertz, P. Fritschel, V. V. Frolov, M. Fuentes-Garcia, R. Fujii, T. Fujimori, Y. Fujiwara, P. Fulda, M. Fyffe, J. R. Gair, S. Galaudage, V. Galdi, M. Galimberti, 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, F. Gautier, V. Gayathri, T. Gayer, G. Gemme, A. Gennai, V. Gennari, J. George, R. George, O. Gerberding, L. Gergely, A. Ghinassi, Archisman Ghosh, Sayantan Ghosh, Shaon Ghosh, Shrobana Ghosh, Suprovo Ghosh, Tathagata Ghosh, J. A. Giaime, K. D. Giardina, D. R. Gibson, C. Gier, F. Gittins, J. Glanzer, F. Glotin, E. Glowacki, J. Godfrey, R. V. Godley, O. Godwin, A. S. Goettel, E. Goetz, J. Golomb, S. Gomez Lopez, G. González, P. Goodarzi, S. R. Goode, A. Goodwin-Jones, M. Gosselin, S. M. Goss-Grubbs, C. Gostiaux, R. Gouaty, D. W. Gould, D. Goupilliere, K. Govorkova, A. Grado, V. Graham, A. E. Granados, M. Granata, V. Granata, S. Gras, P. Grassia, C. Gray, R. Gray, G. Greco, A. C. Green, L. Green, S. R. Green, A. M. Gretarsson, E. M. Gretarsson, D. Griffith, C. Grimaud, H. Grote, S. Grunewald, A. G. Guerrero, G. M. Guidi, T. Guidry, H. K. Gulati, F. Gulminelli, H. Guo, W. Guo, Y. Guo, A. Gupta, I. Gupta, N. C. Gupta, S. K. Gupta, V. Gupta, N. Gupte, N. Guttman, F. Guzman, M. Haberland, S. Haino, E. D. Hall, E. Z. Hamilton, G. Hammond, W. -B. Han, 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, J. Harms, G. M. Harry, I. W. Harry, M. T. Hartman, B. Haskell, C. -J. Haster, K. Haughian, H. Hayakawa, K. Hayama, J. Hedberg, A. Heffernan, D. Hegde, M. C. Heintze, J. Heinzel, H. Heitmann, F. Hellman, A. F. 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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 version has an updated author list, updated references and some text has been modified to improve clarity. This article draws heavily from the corresponding O4a article, arXiv:2508.18079Subjects: gr-qc astro-ph.HECreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
LIGO, Virgo, KAGRA, and GEO 600 form a network of gravitational-wave observatories. Data and analysis results from this network are made publicly available through the Gravitational Wave Open Science Center (GWOSC). This paper describes open data from this network, including the addition of data from the second part of the fourth observing run (O4b) and selected periods from the preceding engineering run (ER16), which were collected from times spanning April 6th, 2024 to January 28th, 2025. The public data set includes calibrated strain time series for each instrument, data from additional channels used for noise subtraction and detector characterization, and new analysis data products in the online GWOSC release associated with version 5.0 of the Gravitational-Wave Transient Catalog.
[abstract 9 / 33] Yes (score: 5) - Title: Short-Duration Gamma-ray Burst and Afterglow Rates in the Rubin and Roman EraAuthors: Tzvetelina Dimitrova, Nathaniel Butler,Comments: ApJ submittedSubjects: astro-ph.HECreated: 2026-06-16; Updated: 2026-06-18; Datestamp: 2026-06-18
Short-duration GAMMA-RAY BURST (sGRB) afterglows that follow BNS-gravitational wave (GW) events are essential for understanding the tension between the observed sGRB rate and BNS merger rate, heightened by the recent conclusion of aLIGO O4 with no new confirmed BNS detections. Using a probabilistic sGRB world model derived from a source BNS merger population, we simulate afterglow emission with AfterglowPy to investigate detection prospects of afterglows in the new era of optical surveys, and probe their multi-messenger implications. The predicted sGRB/BNS association is strongly dependent on sGRB beaming, which may be constrained by orphan afterglows (OA) - that arise from events with no prompt $γ$-ray detection. We conclude that the Vera C. Rubin Observatory's Large Synoptic Survey Telescope (LSST) may detect an afterglow sample sufficient in constraining sGRB JETting, with an estimated $0.9^{+0.5}_{-0.3}$ on-axis afterglow and $1.3^{+0.9}_{-0.5}$ OA detections per year; while the deep sensitivity of the Roman Space Telescope appears promising for probing the faint end of afterglow events in targeted follow-up strategies. The detection of afterglows in upcoming LIGO runs is possible but challenging, as we predict less than one LSST or Roman discoverable event per year within the projected aLIGO O5 BNS range across all considered JET models and observing scenarios. We update previous sGRB-BNS rate predictions, finding that continued non-detection of a BNS in O5 would require revisiting key assumptions underlying sGRB-BNS models.
[abstract 10 / 33] Yes (score: 4) - Title: A recoiling supermassive BLACK HOLE in a powerful QUASARAuthors: Marco Chiaberge, Takahiro Morishita, Matteo Boschini, Stefano Bianchi, Alessandro Capetti, Gianluca Castignani, Davide Gerosa, Masahiro Konishi, Shuhei Koyama, Kosuke Kushibiki, Erini Lambrides, Eileen T. Meyer, Kentaro Motohara, Massimo Stiavelli, Hidenori Takahashi, Grant R. Tremblay, Colin Norman,Comments: 36 pages, 10 figures, revised version after referees' comments. Fig. 8 Corrected (was erroneously a duplicate of Fig. 2)Subjects: astro-ph.GA gr-qcCreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
Supermassive BLACK HOLEs (SMBH) are thought to grow through accretion of matter and mergers. Models of SMBH mergers have long suffered the final parsec problem, where SMBH binaries may stall before energy loss from gravitational waves (GW) becomes significant, leaving the pair unmerged. Direct evidence of coalesced SMBH remains elusive. Theory predicts that GW recoiling BLACK HOLEs can occur following a BLACK HOLE merger. Here we present new and conclusive spectroscopic evidence that both the accretion disk and the broad line region in the spatially offset QUASAR 3C 186 are blue-shifted by the same velocity relative to the host galaxy, with a line of sight velocity of (-1310 +- 21) km/s. This is best explained by the GW recoil super-kick scenario. This confirmation of the ejection process implies that the final parsec problem is resolved in nature, providing evidence that even the most massive BLACK HOLEs can merge.
[abstract 11 / 33] Yes (score: 4) - Title: FPIC: a new Particle-In-Cell code for stationary and axisymmetric black-hole spacetimesAuthors: Claudio Meringolo, Luciano Rezzolla,Comments: 15 pages, 11 figuresSubjects: astro-ph.HE gr-qc physics.plasm-phCreated: 2026-06-16; Updated: 2026-06-18; Datestamp: 2026-06-18
In this paper we present a newly developed GRPIC code framework called FPIC, providing a detailed description of the Maxwell-equations solver, of the particle ``pushers'', and of the other algorithms that are needed in this approach. We describe in detail the code, which is written in Fortran and exploits parallel architectures using MPI directives both for the fields and particles. FPIC adopts spherical Kerr-Schild coordinates, which encode the overall spherical topology of the problem while remaining regular at the event horizon. The Maxwell equations are evolved using a finite-difference time-domain solver with a leapfrog scheme, while multiple particle ``pushers'' are implemented for the evolution of the particles. In addition to well-known algorithms, we introduce a novel hybrid method that dynamically switches between the most appropriate scheme based on the violation of the Hamiltonian energy. We first present results for neutral particles orbiting around BLACK HOLEs, both in the Schwarzschild and Kerr metrics, monitoring the evolution of the Hamiltonian error across different integration schemes. We apply our hybrid approach, showing that it is capable of achieving improved energy conservation at reduced computational cost. We apply FPIC to investigate the Wald solution, first in electrovacuum and subsequently in plasma-filled configurations. In the latter case, particles with negative energy at infinity are present inside the ergosphere, indicating that the Penrose process is active. Finally, we present the split-monopole solution in a plasma-filled environment and successfully reproduce the Blandford-Znajek luminosity, finding very good agreement with analytical predictions.
[abstract 12 / 33] Yes (score: 4) - Title: Orbital evolution of asymmetric binaries within accreting environmentsAuthors: Albert Radulea, Marcelo E. Rubio, Konstantinos Kritos, Andrea Maselli,Comments: 14 pages, 7 figuresSubjects: gr-qc astro-ph.HECreated: 2026-06-16; Updated: 2026-06-18; Datestamp: 2026-06-18
Extreme mass-ratio inspirals embedded in accretion disks provide a natural arena for studying the interplay between RELATIVISTIC orbital dynamics and environmental effects. In this work, we develop a framework to investigate the secular evolution of compact objects repeatedly crossing an accretion disk around a supermassive BLACK HOLE. The orbital motion is modeled through Kerr geodesics, while disk interactions are encoded through effective prescriptions for mass accretion and dynamical friction. We find that disk-induced dissipation generically drives a two-stage evolution characterized by rapid alignment of the orbital plane with the disk, followed by slower eccentricity damping. By systematically comparing the dynamics with a purely Keplerian treatment, we show that cumulative RELATIVISTIC effects produce deviations even at large orbital separations, where the Keplerian approximation would naively be expected to remain accurate. These discrepancies grow through repeated disk crossings and become increasingly pronounced in more RELATIVISTIC orbital configurations. We further investigate the impact of the accretion-disk model by comparing the Sirko-Goodman and Novikov-Thorne prescriptions. Relativistic disk structures predict systematically lower densities and larger scale heights, leading to weaker orbital dissipation and slower secular evolution. By contrast, the spin of the central BLACK HOLE has only a minor effect on the overall circularization efficiency. Our results demonstrate the importance of consistently modeling both RELATIVISTIC orbital dynamics and disk structure when studying compact objects embedded in AGN disks, and provide a framework for exploring their long-term evolution, as well as a possible connection to quasi-periodic eruptions.
[abstract 13 / 33] Yes (score: 4) - Title: Late-time JWST/NIRCam Observations of the Extremely Long-duration GRB 250702B/EP 250702a and Its Host GalaxyAuthors: Huei Sears, Jean J. Somalwar, Ryan Chornock, Tanmoy Laskar, Andrew Levan, Raffaella Margutti, Brendan O'Connor, Nayana A. J., Tomas Ahumada, Kate D. Alexander, Igor Andreoni, Akash Anumarlapudi, Jonathan Carney, James Freeburn, Lluís Galbany, Benjamin P. Gompertz, Or Graur, Saarah Hall, Xander J. Hall, Erica Hammerstein, Saurabh W. Jha, Mansi M. Kasliwal, Dheeraj Pasham, Itai Sfaradi, Yuhan Yao,Comments: 18 pages, 10 figuresSubjects: astro-ph.HE astro-ph.SRCreated: 2026-06-16; Updated: 2026-06-18; Datestamp: 2026-06-18
We present JWST/NIRCam observations of the extremely long-duration GAMMA-RAY BURST (GRB) 250702B taken at ~ 95 days post-GRB (observer frame). The observations of the host galaxy reveal a single galaxy with a prominent dust lane observed nearly edge-on. Prospector modeling of the host galaxy photometry finds a high stellar mass (log(M_*/M_Sun) = 11.0 +0.2/-0.3) and large dust column (A_V = 2.8 +/- 0.3 mag), in agreement with previous results. If GRB 250702B is a collapsar-driven GRB, the host galaxy is the brightest (in rest-frame r and rest-frame H) and most massive compared to GRB hosts at similar redshifts. The transient localization is near the dust lane, and while we find no evidence for transient emission in F277W, F356W, and F444W, forced photometry in F150W and F200W reveals possible ~ 3 sigma detections of the transient at m_{F150W} ~ 27.9 AB mag and m_{F200W} ~ 27.4 AB mag. If these are secure detections, they are indicative of a late-time light curve flattening. This behavior is consistent with that of JETted tidal disruption events (TDEs); however, it is also consistent with a SUPERNOVA plus GRB afterglow model. Alternatively, if these are upper limits, they are consistent with, but do not further constrain, the extrapolated power-law decline of the afterglow. The ambiguity of the possible detection of the transient in F150W and F200W highlights the need for late-time template observations with JWST/NIRCam.
[abstract 14 / 33] Yes (score: 4) - Title: A comparative study of solar flux emergence and eruptivity in simulations of horizontal versus toroidal MAGNETic fieldsAuthors: Vaggelis Karantanis, Juxhin Zhuleku, Vasilis Archontis, Kostas Moraitis,Comments:Subjects: astro-ph.SRCreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
Context: Magnetic flux emergence is a fundamental driver of eruptive activity in the solar atmosphere. While many numerical studies employed idealized horizontal flux tubes, toroidal tubes provide a more realistic geometry for finite emerging loops with anchored footpoints. Aims: We compare the evolution and eruptive capability of horizontal and toroidal flux tubes under identical initial parameters. Methods: We performed 3D resistive MAGNETohydrodynamic (MHD) simulations of the emerging MAGNETic flux structures to evaluate their respective dynamics Results: Although the toroidal tube emerges later than in the horizontal case, it produces a higher frequency of eruption-driven JETs (four versus two) because the supply of coronal axial flux is sustained. In contrast, the horizontal tube injects MAGNETic flux and energy more impulsively, driving stronger but less persistent activity and then rapidly stagnating when its atmospheric axial-flux reservoir is depleted. Free MAGNETic energy builds up after emergence and is released in discrete drops associated with eruptions. The toroidal case exhibits a quasi-cyclic buildup and release pattern, whereas the horizontal case relaxes to a lower-activity state after its early eruptions. The temporal evolution of relative MAGNETic helicity mirrors the free-energy evolution. Helicity increases with the stressing and twisting of the coronal field during emergence, peaks near eruptive episodes, and decreases as eruptions remove twisted flux, with the toroidal tube maintaining a more persistent helicity budget that supports recurrent events. Conclusions: Initial flux-tube geometry strongly controls the coronal flux budget and the storage and release of free energy and helicity, and therefore, the frequency and longevity of eruptive phenomena in emergence-driven active regions.
[abstract 15 / 33] Yes (score: 4) - Title: Distinct Near-Horizon Trend of Synchrotron Polarization in Kerr SpacetimeAuthors: Yehui Hou, Jiewei Huang, Bin Chen,Comments: 11 pages, 1 figureSubjects: gr-qcCreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
We show that the near-horizon expansion of the linear POLARIZATION vector for SYNCHROTRON emission in a Kerr background admits a distinct analytic form. For emission from a stationary, axisymmetric, degenerate electroMAGNETic field, the leading-order POLARIZATION pattern depends only on the Kerr spin and the source polar angle, while the next-to-leading-order correction further encodes the geometric and rotational structure of the electroMAGNETic field. Our result extends the equatorial analysis of [Hou et al. (2024)] and the off-equatorial leading-order result of [Chael et al. (2026)]. Near-horizon POLARIZATION thus offers a potential probe of the fundamental properties of rotating BLACK HOLEs and of gravito-electroMAGNETic interactions.
[abstract 16 / 33] (score: 3) - Title: Evidence for a $\sim 43$ GeV $γ$-ray line signal in a stacking analysis of the Virgo, Fornax, and Ophiucus Galaxy clustersAuthors: Yi-Zhong Fan, Zhao-Qiang Shen, Yun-Feng Liang, Xiang Li, Kai-Kai Duan, Zi-Qing Xia, Xiao-Yuan Huang, Lei Feng, Qiang Yuan,Comments: 8+14 pages, 4+16 figures, 0+5 tables; accepted for publication in PRLSubjects: astro-ph.HE astro-ph.CO hep-phCreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
As the largest gravitationally bound objects in the Universe, galaxy clusters have provided the first piece of evidence for the presence of DARK MATTER and may be suitable targets for indirect DARK MATTER searches. Among various signals, the GeV-TeV $γ$-ray line has been taken as the smoking-gun signal of the DARK MATTER annihilation/decay since no known astrophysical/physical process(es) could generate such a peculiar spectrum. With 15.5 years of FERMI-LAT P8R3 publicly available data, we search for the $γ$-ray line emission in the directions of a group of 13 massive galaxy clusters at redshifts $z \leq 0.028$ with an unbinned likelihood analysis. A $γ$-ray line signal at $\sim 43.2$ GeV has a net TS value of $\approx 30$ if we only take into account the data in the directions of Virgo, Fornax and Ophiuchus clusters, three massive clusters with the highest J-factors expected to generate the DARK MATTER annihilation signal. The signal still presents when the data of other 10 nearby massive clusters have also been included, though the TS value decreases to $\approx 21$ likely because of their lower signal-to-noise ratios. The absence of this signal in the inner Galaxy disfavors both the instrumental effect and the canonical DARK MATTER annihilation interpretation, and a more sophisticated DARK MATTER model or very peculiar astrophysical scenario might be needed. This $γ$-ray line signal, if intrinsic, could be unambiguously verified by the Very Large Area $γ$-ray Space Telescope in its first two years of performance.
[abstract 17 / 33] (score: 3) - Title: The X-ray emission of the long-period transient and accreting cataclysmic variable ASKAP J174508.9-505149Authors: M. Imbrogno, M. Veresvarska, Y. L. Wang, N. Rea, F. Coti Zelati, K. Rose, J. Pritchard, D. de Martino, S. Scaringi, Z. Wang, D. L. Kaplan,Comments: Accepted for publication in A&A Letters on 27/05/2026. 7 pages (4 main text+ 3 appendices)Subjects: astro-ph.HECreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
Long-period transients (LPTs) challenge our knowledge of the mechanism producing radio periodic pulsations in compact objects. Some LPTs have been associated with systems hosting a white dwarf and a low-mass star in a detached binary. Recently, a new LPT (ASKAP\,J174508.9-505149) has been classified as an accreting cataclysmic variable (CV). In the present letter, we report on the detailed study of the X-ray variability of ASKAP\,J174508.9-505149 as observed by \emph{XMM-Newton} and \emph{Einstein Probe} between September 2025 and May 2026. Simultaneous optical and radio observations are also presented. We studied the timing variability of the source, and estimated an X-ray periodicity of $P=4868(22)$\,s, consistent with radio and optical periods. We also observe the same periodicity in the hardness ratio extracted from the \emph{XMM-Newton} observation, peaking at the minimum of the modulation. A long-term modulation is also present in the X-rays and in the B-band photometry, but it is poorly constrained by the current dataset. Spectral X-ray analysis shows the presence of a black-body component ($\sim$0.1\,keV), a collisionally ionised plasma ($\sim$15\,keV), and an absorption feature at 0.77 keV (possibly due to Oxygen-VII). This is the third LPT detected in the X-ray band, the second with a detected X-ray periodicity and variable X-ray emission, and the first conclusively recognised as an accreting MAGNETic CV.
[abstract 18 / 33] (score: 3) - Title: Ultra-High-Resolution Astronomy with the Solar Gravitational LensAuthors: Slava G. Turyshev,Comments: 40 pages, 13 figures, 11 tablesSubjects: astro-ph.IMCreated: 2026-06-16; Updated: 2026-06-18; Datestamp: 2026-06-18
The solar gravitational lens (SGL) is a target-specific observatory: the Sun supplies the wave-optical element, while spacecraft provide occultation, annular photometry, sampling, metrology, and inverse reconstruction. We develop an observability framework for non-exoplanet SGL astronomy. Viability is set by image-plane scale, raster pitch, finite-source gain, source-to-background ratio, temporal coherence, PSF knowledge, calibration, metrology, and focal-line access. We separate the vector Poisson measurement operator from the scalar convolution used for benchmarks. Four analytic scenes are propagated and reconstructed: a solar analog and MAGNETic white dwarf at 10 pc, an M87*-scale millimeter ring/JET source, and a bright 0.1 AU protoplanetary subfield at 140 pc. Under stated kernel-mismatch, background, calibration-floor, support-mask, sampling, regularization, and imposed information-floor assumptions, the scalar reconstructions give SSIM values of 0.993, 0.918, 0.973, and 0.923. These metrics quantify scalar inverse conditioning, not delivered flight performance; FRC50, support-leakage, and information-floor sensitivity diagnostics expose the dependence on assumptions. Many self-luminous compact targets are not photon-starved relative to a reflected-light exo-Earth reference, shifting the dominant requirements to ring extraction, coronal subtraction, detector dynamic range, PSF knowledge, cadence, spectroscopy, metrology, scan overhead, and access. The strongest bounded cases are white-dwarf surface and MAGNETic mapping, nearby stellar surfaces, compact AGN/black-hole structure with long-wavelength instrumentation, velocity-resolved broad-line-region mapping, and planet-forming subfields. The priority enabling program is SGL transfer-function characterization: measuring solar-multipole, plasma, extended-Sun, and instrumental response needed for scientifically interpretable imaging.
[abstract 19 / 33] (score: 3) - Title: Extension of a multi-region free-surface MHD solver beyond the inductionless approximationAuthors: Min Ki Jung, Brian Wynne, Francisco Saenz, Yufan Xu, Jabir Al-Salami, Yong-Su Na, Egemen Kolemen,Comments:Subjects: physics.comp-ph physics.plasm-phCreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
Free-surface liquid metal flows are a leading candidate for the plasma-facing components of future fusion reactors. Existing transient, three-dimensional, free-surface MHD solvers rely on the inductionless approximation in which the induced MAGNETic field is neglected. This paper extends the open-source solver FreeMHD [B. Wynne et al., Phys. Plasmas 32, 013907 (2025)] beyond the inductionless approximation to resolve the induced MAGNETic field self-consistently using a vector-potential formulation that enforces $\nabla\cdot\boldsymbol{B}=0$ by construction while preserving the original multi-region, two-phase framework. The solver is verified against analytical Shercliff and Hunt duct-flow solutions across a range of Hartmann numbers and validated against free-surface height measurements from the LMX-U experiment. To the best of our knowledge, FreeMHD2 is the first open-source, experimentally validated free-surface liquid metal solver to resolve the evolution of the induced MAGNETic field without invoking the inductionless approximation. By removing this approximation rather than relaxing it, the formulation provides the basis for future modeling of the finite MAGNETic Reynolds number conditions expected in large-scale, transient fusion events.
[abstract 20 / 33] (score: 3) - Title: Searching for a superdisk in RADIO GALAXy J0116-473Authors: Ankur Sinha, Riya Rathore, Narendra Nath Patra, Abhirup Datta,Comments: 13 pages, 5 figuresSubjects: astro-ph.GACreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
Superdisks have emerged as an active area of research in recent years, and J0116-473 represents a promising target for studying this extended structure. Our primary objective was to search for HI absorption associated with the suspected superdisk. However, no such absorption feature was detected, suggesting a low, or absence of neutral hydrogen content in the superdisk. In addition, we examined a compact point source located near the galaxy's core and the presumed plane of the superdisk, enabling us to search for HI absorption against this background continuum. We also present a detailed multi-band morphological analysis of the galaxy using Giant Metrewave Radio Telescope (GMRT) observations in Bands 3, 4, and 5. A spectral analysis of both the galaxy and the nearby point source was carried out using data from these three frequency bands. A systematic steepening of the spectral index is observed from the core toward the lobes, as expected for aging SYNCHROTRON-emitting plasma. We also found that the northern inner lobe exhibits a significantly steeper spectrum than its southern counterpart, possibly reflecting environmental effects associated with the proposed superdisk. Since superdisks are expected to contain hot, ionized gas, we additionally examined archival X-ray observations from the XMM-Newton telescope. Although diffuse X-ray emission associated with the radio lobes is visible, no significant emission is detected from the region corresponding to the suspected superdisk.
[abstract 21 / 33] (score: 3) - Title: Fine-scale downflows above flare ribbons captured by Solar Orbiter/EUIAuthors: Zheng Sun, Alexander G. M. Pietrow, Malcolm K. Druett, Hui Tian, Julián D. Alvarado-Gómez, Song Tan, Alexander Warmuth, Jiasheng Wang, Yuhang Gao, Zhenyong Hou, Alexandros Stork,Comments: Accepted by A&A. There is one attached video (one could contact zhsun@aip.de to get the video)Subjects: astro-ph.SRCreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
In solar flares, flare ribbons map chromospheric footpoints where flare energy deposition occurs. These locations are associated with field aligned energy transport from the corona that results from energy liberated during MAGNETic RECONNECTion. Recent chromospheric observations in the H$α$ and H$β$ bands have revealed fine-scale downflow structures above flare ribbons, referred to as riblets. In this study, we identify similar downflow structures in the extreme-ultraviolet (EUV) wavelength using high-resolution observations from Solar Orbiter/EUI. These fine-scale downflows appear as downward-propagating, bright, and thread-like structures. They exhibit typical velocities of $\sim100~\mathrm{km\ s^{-1}}$, lifetimes of $\sim15$~s, and lengths of $\sim1.6$~Mm. Based on their morphological and dynamical properties, we interpret these observed downflows as the EUV counterparts of the riblets that have previously been reported from chromospheric observations. This study presents EUV imaging of $\sim 10^6$~K downflows above flare ribbons. We interpret these downflows as a result of (1) the energisation and subsequent compression of pre-existing chromospheric fibrils due to particle beams or (2) adiabatic or shock-driven compression induced by the downward-propagating plasma from the corona. These fine-scale EUV riblets provide a new diagnostic tool for probing the dynamics of MAGNETic RECONNECTion as well as energy transport and deposition during solar flares.
[abstract 22 / 33] (score: 2) - Title: Non-conservative Mass Transfer as a Formation Channel for Gaia Black Hole SystemAuthors: Aleksandra Olejak, Jakub Klencki, Alejandro Vigna-Gomez, Selma E. de Mink, Lieke van Son, Jakub Cehula, Jakob Stegmann, Taeho Ryu, David D. Hendriks,Comments: 17 pages, version accepted for publication in ApJSubjects: astro-ph.HE astro-ph.SRCreated: 2026-06-16; Updated: 2026-06-18; Datestamp: 2026-06-18
The detected Gaia systems hosting compact objects challenge standard models of binary star evolution. In particular, if the observed BLACK HOLE (BH) systems evolved in isolation, they are expected to have undergone a mass transfer phase. Given their highly unequal masses, such mass transfer is dynamically unstable within standard models, leading to a stellar merger or a short-period binary. In contrast, the observed systems have much wider orbits than predicted, making their formation within conventional evolutionary frameworks difficult to reconcile. Using detailed binary evolution calculations, we test whether non-conservative mass transfer, in which most of the mass is lost from the system carrying the specific angular momentum of the donor's center of mass, can explain the properties of two Gaia BH systems. This mass-loss geometry differs from standard isotropic re-emission from the accretor's vicinity. We find that our mass-loss geometry model reproduces the orbital periods of the two Gaia BH systems remarkably well over a wide range of initial conditions, offering a plausible formation pathway. We speculate this may point to enhanced eruptive mass loss, potentially driven by high-opacity subsurface layers in the donor prior to Roche-lobe overflow, consistent with preferentially bipolar outflows observed in luminous blue variables. Alternatively, it may indicate the need for more sophisticated mass-transfer prescriptions that account for highly unequal Roche-lobe sizes, sub-synchronous rotation, and possible self-accretion. Similar mechanisms may operate in other post-mass-transfer systems facing analogous evolutionary challenges, including Gaia neutron-star and white-dwarf binaries, stripped-envelope Wolf-Rayet stars, and low-mass X-ray binaries.
[abstract 23 / 33] (score: 2) - Title: Probing Hairy Kerr Black Holes through Quasi-Periodic Oscillations I: A study based on the kinematic modelsAuthors: Anirban Dasgupta, Supragyan Priyadarshinee, Indrani Banerjee, Subhash Mahapatra,Comments: 44 pages, 23 figures, 7 table; Accepted for publication in the Physics of the Dark UniverseSubjects: gr-qcCreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
Black holes endowed with nontrivial scalar or matter fields, known as hairy BLACK HOLEs, possess additional parameters beyond mass, charge, and spin, leading to richer phenomenology. Constraining their parameter space is therefore essential, particularly in view of current electroMAGNETic and gravitational-wave observations. In this work, we study rotating hairy BLACK HOLE solutions inspired by the gravitational decoupling method, which satisfy the Einstein field equations with a conserved energy-momentum tensor obeying the strong energy conditions. We explore in detail the horizon structure of such BLACK HOLEs and report for the first time certain unique features not observed in Kerr BLACK HOLEs. We examine how the hair parameters influence the fundamental frequencies governing particle motion in the hairy Kerr spacetime and compare these effects with the Kerr case. Since theoretical models of high-frequency quasi-periodic oscillations (HFQPOs) are directly linked to these fundamental frequencies, this provides a powerful observational probe of hairy BLACK HOLEs. By confronting several kinematic HFQPO models with observations from six BLACK HOLE sources, we report that for most sources, the HFQPO data at the current level of precision cannot distinguish between the Kerr and hairy Kerr scenarios. However, based on agreement with previous spin estimates, our analysis provides a systematic framework to assess the relative suitability of different HFQPO models for each source. Notably, even with current observational precision, we find that both the Relativistic Precession Model and the Tidal Disruption Model appear unsuitable for the sources GRO J1655-40 and GRS 1915+105. The broader implications of these findings are discussed.
[abstract 24 / 33] (score: 2) - Title: Quark and gluon production in the presence of the time-varying chiral MAGNETic currentAuthors: Kirill Tuchin,Comments: 14 pages, 8 figures, v2: typos fixed, appendix addedSubjects: hep-ph nucl-thCreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
The chiral MAGNETic effect consists in the induction of the electric current along the direction of the MAGNETic field. The corresponding transport coefficient $b_0$, known as the chiral MAGNETic conductivity, is proportional to the chiral imbalance in the medium. In many systems, such as QUARK-gluon plasma, $b_0$ is time-dependent. This paper studies the effect of the time variation of $b_0$ on the particle spectra and energy loss produced through the chiral Cherenkov and associated processes in Abelian and non-Abelian systems. The rates of all processes are derived in the ultra-RELATIVISTIC approximation. The results are applied to the RELATIVISTIC heavy-ion collisions utilizing a specific model describing the relaxation of the initial $P$-odd domain within the QUARK-gluon plasma. The corresponding energy loss is computed. The results suggest strong POLARIZATION of JETs in QUARK-gluon plasma.
[abstract 25 / 33] (score: 2) - Title: Shadow dependent phenomenology framework for rotating BLACK HOLE metricAuthors: Nikko John Leo S. Lobos, Emmanuel T. Rodulfo,Comments: 8 pagesSubjects: gr-qcCreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
We establish a formal thermodynamic-optical duality that bridges the semiclassical quantum evaporation of BLACK HOLEs with their classical macroscopic geometry. The physical viability of this framework is anchored by a stable multivariate coordinate transformation and a non-vanishing Jacobian determinant, which allows for a diffeomorphic inversion mapping that decouples intrinsic physical quantities such as bare mass from the unobservable spacetime interior. By re-parameterizing BLACK HOLE properties entirely in terms of the analytical shadow radius ($R_{sh}$), we derive explicit, observable-based expressions for the weak deflection angle, Hawking temperature, and integrated semiclassical luminosity. We demonstrate the framework's predictive utility by applying it to standard Kerr, Kerr-MOG (Scalar-Tensor-Vector Gravity), and rotating Horndeski spacetimes. Our results provide a definitive mathematical solution to parameter degeneracy, revealing that distinct fundamental fields (vector vs. scalar) leave unique observational fingerprints on far-field astrometry and horizon-scale quantum thermodynamics. By confronting these models with Event Horizon Telescope (EHT) M87* data, we show that this formalism successfully breaks mass-parameter degeneracies, offering a robust and computationally efficient operational tool for testing the Kerr hypothesis and probing modified gravity theories with next-generation very-long-baseline interferometry (VLBI).
[abstract 26 / 33] (score: 2) - Title: MeV Gamma-Ray Lines from Radioactive Nuclei in Magnetar Giant FlaresAuthors: Wu-Zimo Qiumu, Meng-Hua Chen, Qiu-Hong Chen, Fei Xie, Hou-Jun Lü, Xiang-Gao Wang, En-Wei Liang,Comments: 12 pages, 6 figures, 2 tables. Accepted for publication in SCIENCE CHINA Physics, Mechanics & AstronomySubjects: astro-ph.HECreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
The rapid neutron-capture process (r-process) is widely regarded as the dominant mechanism responsible for the synthesis of heavy elements in the universe, yet its astrophysical sites remain an open question. Recent studies suggest that the high-entropy, rapidly expanding baryonic material ejected by MAGNETar giant flares may provide favorable conditions for r-process nucleosynthesis, while the late-time gamma-ray emission observed from the MAGNETar SGR 1806-20 offers direct observational support for this scenario. In this work, we perform nuclear reaction network simulations to investigate the nucleosynthesis yields of MAGNETar giant flares and to characterize the associated nuclear gamma-ray line emission arising from the radioactive decay of heavy nuclei. The nuclei synthesized in MAGNETar giant flares are found to be mainly distributed near the first and second r-process abundance peaks. Owing to this nuclide composition, the gamma-ray opacity is found to be strongly energy-dependent with the opacity in the keV band exceeding that in the MeV band by approximately three orders of magnitude. The nuclear gamma-ray emission is dominated by MeV photons at early times and gradually extends toward the sub-MeV and keV bands as time progresses, thereby offering a diagnostic of heavy element enrichment in the ejecta. The gamma-ray spectrum exhibits a peak near 1 MeV with major contributions from $^{88}$Kr and $^{92}$Sr, whose radioactive decays produce several bright gamma-ray lines with fluxes exceeding $\sim10^{-8}$ erg cm$^{-2}$ s$^{-1}$, making them the most promising lines for detection by MeV gamma-ray detectors. Because MAGNETar giant flares occur in the Galaxy at a rate roughly three orders of magnitude higher than neutron star mergers and their gamma-ray lines are accessible to current MeV instruments, they offer new and valuable science opportunities for MeV gamma-ray astronomy.
[abstract 27 / 33] (score: 2) - Title: A Log-Uniform Initial Magnetic Field Distribution Explains Pulsar and Magnetar Populations through Magnetic Inclination AlignmentAuthors: Takumi Shimasue, Kenta Hotokezaka, Paz Beniamini,Comments: 12 pages, 12 figuresSubjects: astro-ph.HECreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
The origin of the gap in the observed MAGNETic field distribution between pulsars and MAGNETars raises a challenge to understanding these populations within a unified framework. We analytically show that the gap can be naturally explained by the alignment of the MAGNETic inclination angle between the MAGNETic and spin axes. Based on coupled evolution of spin-down and MAGNETic inclination angle in the plasma-filled MAGNETosphere, the alignment timescale follows $τ_α\propto B^{-2}$. Thus, strongly MAGNETized neutron stars including high-$B$ pulsars and MAGNETars align more rapidly than pulsars with $10^{12}\,\mathrm{G}$, reducing their beaming fraction and thereby suppressing their observed numbers. However, MAGNETars are primarily identified through X-ray activity and are therefore relatively less affected by beaming. Taking into account both beaming fraction and luminosity corrections, we reconstruct the initial MAGNETic field distribution from the observed distribution. We show that pulsars and MAGNETars do not dictate intrinsically distinct initial distributions, but can instead be understood within a single continuous initial MAGNETic field distribution, such as a log-uniform distribution.
[abstract 28 / 33] (score: 2) - Title: \texttt{TransFit-MAG}: Self-Consistent Modeling of Magnetar-Powered Transients from Shock Breakout to Spin-Down HeatingAuthors: Jing-Yao Li, Liang-Duan Liu, Yun-Wei Yu, Guang-Lei Wu, Yu-Hao Zhang,Comments: 11 pages, 4 figuresSubjects: astro-ph.HECreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
Magnetar engines are widely invoked to power luminous optical transients, but their early emission depends on the coupled evolution of engine injection, shock heating, adiabatic cooling, and radiative diffusion. We present \texttt{TransFit-MAG}, a time-dependent radiative-diffusion framework for MAGNETar-powered transients. The model couples the \texttt{TransFit} diffusion solver to the dynamics of a MAGNETar-inflated pulsar wind nebula (PWN) and its forward shock propagating through homologously expanding ejecta, calculating the internal radiation-energy distribution, photospheric evolution, shock-heating location, and emergent luminosity self-consistently. For different parameter values, the model naturally produces well-separated double peaks, partially merged peaks, or single broad peaks. These results suggest that early bumps and broad single peaks in engine-powered transients may be understood within a unified engine--shock--diffusion framework, in which the observed diversity reflects the coupled evolution of central-engine power, shock propagation, and radiative transport through expanding ejecta. As an illustrative application, we fit the multiband optical light curves of the double-peaked SLSN-I LSQ14bdq.
[abstract 29 / 33] (score: 2) - Title: Multi-objective Bayesian optimization of rigid and flexible nozzles for energy-efficient pulsed JET propulsionAuthors: Paras Singh, Yukesh Karki, Victor Hernandez, Daehyun Choi, Saad Bhamla, Chandan Bose,Comments:Subjects: physics.flu-dynCreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
The biomechanics of pulsed-JET propulsion in aquatic animals, including squids and jellyfish, provide valuable insights into energy-efficient locomotion. In these organisms, flexible funnel deformation enables rapid acceleration and maneuverability while minimizing energy use. Drawing inspiration from these biological systems, this study investigates performance trade-offs between rigid and flexible nozzle geometries in pulsed-JET propulsion systems. A multi-objective Bayesian optimization framework integrated with three-dimensional fluid-structure interaction (FSI) simulations identifies nozzle designs that maximize hydrodynamic impulse and minimize JET energy input. The optimization reveals fundamentally distinct performance characteristics for rigid and flexible nozzles. Rigid nozzles achieve the highest impulse amplification, up to 5 times that of a baseline cylindrical nozzle, but at substantially increased energy expenditure. In contrast, flexible nozzles yield lower peak impulse enhancement of about 2.5 times while achieving significantly greater propulsion efficiency. The maximum normalized impulse-to-energy ratio for flexible nozzles is about 1.8 times higher than that of rigid configurations, indicating more effective conversion of input energy into useful propulsive output. Analysis of the flow physics shows that optimized rigid nozzles enhance performance through geometry-induced internal entrainment, secondary vortex formation, and contraction-driven JET acceleration. This results in stronger vortex circulation and downstream convection. Flexible nozzles use traveling expansion-contraction deformation waves that promote additional entrainment during expansion and accelerate the internally entrained fluid during contraction to improve pressure recovery, reduce pressure-energy expenditure, and mitigate negative pressure impulse contributions.
[abstract 30 / 33] (score: 2) - Title: Bivariate incomplete-Bessel kernels for the first nonlinear Vlasov-Maxwell responseAuthors: Roberto Ricci,Comments: Under consideration for publication in J. Plasma PhysSubjects: physics.plasm-phCreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
The weakly nonlinear response of a homogeneous MAGNETised plasma is usually written as a double cyclotron-harmonic expansion. This representation is explicit, but the repeated use of the Jacobi-Anger expansion produces long sums of Bessel functions and nested resonance denominators. In the linear problem we recently obtained an alternative formulation by keeping the Larmor phase unexpanded and by evaluating the characteristic integral in terms of the newly introduced incomplete-Bessel function $G_μ(z,ψ)$. In this article we apply the same idea directly to the first nonlinear Vlasov-Maxwell equation. The nonlinear source contains the linear response of an inner mode. When this linear response is written in incomplete-Bessel form, the outer characteristic integral produces a bivariate orbit-resolvent $G_{μ,ν}^{(r)}(z,ψ;w,χ)$. This function emerges therefore as the natural orbit integral generated by the first nonlinear characteristic problem. We derive the nonlinear distribution function in terms of these bivariate functions, collect the identities needed for the current projection, recover an extension of the classical double-harmonic Liu-Tripathi formula by expansion, and indicate how the nonlinear susceptibility tensor is obtained from bivariate angular contractions.
[abstract 31 / 33] (score: 2) - Title: The first detection of dense gas in a massive main-sequence galaxy at cosmic noonAuthors: Jianhang Chen, Natascha M. Förster Schreiber, Rodrigo Herrera Camus, Lilian L. Lee, Minju M. Lee, Claudia Pulsoni, Daizhong Liu, Sebastián Arriagada-Neira, Capucine Barfety, Ric Davies, Frank Eisenhauer, Juan Manuel Espejo Salcedo, Reinhard Genzel, Jean-Baptiste Jolly, Dieter Lutz, Giovanni Mazzolari, Stavros Pastras, Alvio Renzini, Linda Tacconi, Giulia Tozzi, Hannah Übler,Comments: Submitted to A&A, 7 pages, 4 figures, comments are welcomeSubjects: astro-ph.GACreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
Dense gas is the direct fuel for STAR FORMATION, but measuring it has long been difficult at z>2, especially in typical star-forming main-sequence galaxies. In this work, we report the first detection of HNC (J = 5--4) and CN (N = 4--3) emission in a massive main-sequence galaxy, BX610, at z=2.21. The velocity integrated emission of HNC(5--4)+CN(4--3) is concentrated in the galactic centre, coincident with the region of ongoing intense STAR FORMATION. Based on line decomposition, we measure a line flux ratio HNC(5--4)/CN(4--3) of $1.05\pm0.23$, similar to that of starburst galaxies at comparable redshifts but lower than that of QUASAR/AGN host galaxies. The comparatively fainter HNC(5--4) disfavours the presence of a strongly buried AGN in BX610, consistent with optical line diagnostics. The radiative transfer analysis favours the presence of dense gas with a density of $(2-4)\times10^{6}\,\text{cm}^{-3}$ and a kinetic temperature of 50-80 K. The derived abundance ratio between N(HNC) and N(CN) favours dense gas clouds near photodissociation regions, as commonly seen in typical starburst environments. The inferred dense-gas line luminosity closely follows the scaling relation between far-IR and dense-gas line luminosities established for local luminous infrared galaxies (LIRGs). Our observations support the view that STAR FORMATION in cosmic noon galaxies is primarily controlled by the availability of dense gas, which could be enhanced in central galactic regions with efficient cold gas inflows as observed in BX610 along the inner spiral arms and a possible stellar bar.
[abstract 32 / 33] (score: 2) - Title: Direct Tests of Black Hole Accretion Rate Prescriptions: I. Bondi Accretion at Different ScalesAuthors: James Agostino, Ming-Yi Lin, Natasha Jones, Anne M. Medling, Loreto Barcos-Muñoz, Daniel Anglés-Alcázar, Claudio Ricci, George C. Privon, Vivian U, Paul Torrey, Philip F. Hopkins, Claire Max,Comments: 21 pages, 4 figuresSubjects: astro-ph.GACreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
We present spatially resolved parsec-scale measurements of nuclear conditions (gas density and kinetic temperature) relevant for BLACK HOLE accretion rate predictions in the Seyfert 2 galaxy, NGC 1068. We inject these parameters into the prescription for a Bondi-like accretion model, then compare the resulting accretion rate prediction to the empirical accretion rate derived from hard X-ray observations. Cosmological simulations have spatial resolution ranging from $\sim$10 pc to $\sim$kpc scales, and so for reasonable comparison we test these accretion rate predictions in pixel-sized radial steps out to 500 pc. Compared to warm H$_2$ gas, CO gas is the dominant mass carrier close to the SMBH. We find that the Bondi accretion rate ($\dot{\mathrm{M}}_{\mathrm{Bondi}}$) of cold molecular gas alone (measured using CO) overestimates the true accretion rate by up to 14 dex in a small aperture (r$\lesssim$5 pc) around the BLACK HOLE, and by at least 8 dex inside large apertures (r$\lesssim$500 pc). These results are the first in a series of direct tests of accretion rate prescriptions, and they suggest that using a Bondi accretion formalism to model supermassive BLACK HOLE accretion in Seyfert 2 galaxies may lead to overestimated accretion rates in simulations.
[abstract 33 / 33] (score: 2) - Title: Constraints on Cosmic Strings from the Curl-Mode CMB Lensing Power Spectrum measured by ACT DR6Authors: A. I. Lonappan, K. Ramesh, T. Namikawa, F. J. Qu, B. Keating,Comments: 8 pages, 3 figures, 2 tablesSubjects: astro-ph.CO gr-qc hep-phCreated: 2026-06-17; Updated: 2026-06-18; Datestamp: 2026-06-18
A network of cosmic strings is one of the few well-motivated cosmological sources of vector and tensor metric perturbations on the largest observable scales. Such perturbations imprint a characteristic curl component in the deflection angle of cosmic microwave background (CMB) photons that, unlike the scalar lensing potential, vanishes for adiabatic density fluctuations at linear order. We exploit the curl-mode lensing reconstruction released as part of the Atacama Cosmology Telescope (ACT) Data Release~6 (DR6), based on five seasons of temperature and POLARIZATION data covering $9400~\mathrm{deg}^2$ of sky, to set new constraints on the dimensionless string tension $Gμ$ and the inter-commutation (RECONNECTion) probability $P$. Modelling the string-induced curl power spectrum within the velocity-dependent one-scale framework, we obtain a $2σ$ upper bound on the combination $GμP^{-1}\le 3.5\times 10^{-5}$ in the small-$P$ regime, and $Gμ\le 5.0\times 10^{-5}$ at $2σ$ assuming the canonical Nambu-Goto value $P=1$. Combining the ACT DR6 curl bandpowers with the Planck 2013 curl-mode reconstruction, which extends down to $L_{\rm min}=2$, tightens these bounds to $GμP^{-1}\le 3.2\times 10^{-5}$ and $Gμ\le 4.3\times 10^{-5}$ ($2σ$). These represent the tightest constraints on cosmic strings derived from the curl-mode CMB lensing power spectrum to date. Using the ACT data alone, compared to the ACT 2008-season analysis, the ACT DR6 constraint on $GμP^{-1}$ is nearly an order of magnitude tighter.
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