Current date: 2026-06-25
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Number of records retrieved: 719
Keyword score statistics
score 21 -- 1 abstracts
score 10 -- 2 abstracts
score 9 -- 1 abstracts
score 7 -- 1 abstracts
score 6 -- 3 abstracts
score 5 -- 8 abstracts
score 4 -- 5 abstracts
score 3 -- 14 abstracts
score 2 -- 27 abstracts
in total -- 62 abstracts
Articles that appeared on 2026-06-25
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[abstract 1 / 62] Wow! (score: 21)
- Title: Broadband multiwavelength properties of the archetypal BLAZAR 3C 279 during the 2017 Event Horizon Telescope campaignAuthors: G. Principe, J. C. Algaba, E. Aviano, W. Y. Cheong, K. Hada, D. Haggard, A. Hahn, S. G. Jorstad, E. V. Kravchenko, Y. Kovalev, S. S. Lee, M. Lisakov, S. Markoff, A. P. Marscher, M. Sasada, P. Voitsik, Kazunori Akiyama, Ezequiel Albentosa-Ruiz, Antxon Alberdi, Walter Alef, Richard Anantua, Eleni Antonopoulou, Keiichi Asada, Rebecca Azulay, Anne-Kathrin Baczko, David Ball, Bidisha Bandyopadhyay, John Barrett, Michi Baubock, Bradford A. Benson, Dan Bintley, Lindy Blackburn, Raymond Blundell, Katherine L. Bouman, Geoffrey C. Bower, Michael Bremer, Roger Brissenden, Silke Britzen, Avery E. Broderick, Dominique Broguiere, Thomas Bronzwaer, Sandra Bustamante, Douglas F. Carlos, John E. Carlstrom, Andrew Chael, Chi-kwan Chan, Dominic O. Chang, Koushik Chatterjee, Ming-Tang Chen, Yongjun Chen, Xiaopeng Cheng, Paul Chichura, Ilje Cho, Nicholas S. Conroy, John E. Conway, Thomas M. Crawford, Geoffrey B. Crew, Alejandro Cruz-Osorio, Yuzhu Cui, Brandon Curd, Rohan Dahale, Jordy Davelaar, Joost de Kleuver, Mariafelicia De Laurentis, Roger Deane, Jason Dexter, Vedant Dhruv, Indu K. Dihingia, Sheperd S. Doeleman, Sergio A. Dzib, Razieh Emami, Heino Falcke, Joseph Farah, Vincent L. Fish, Edward Fomalont, H. Alyson Ford, Marianna Foschi, Raquel Fraga-Encinas, William T. Freeman, Per Friberg, Christian M. Fromm, Antonio Fuentes, Peter Galison, Charles F. Gammie, Roberto Garcia, Olivier Gentaz, Boris Georgiev, Ciriaco Goddi, Roman Gold, Arturo I. Gomez-Ruiz, Jose L. Gomez, Minfeng Gu, Mark Gurwell, Ronald Hesper, Dirk Heumann, Luis C. Ho, Paul Ho, Mareki Honma, Chih-Wei L. Huang, Lei Huang, David H. Hughes, Shiro Ikeda, C. M. Violette Impellizzeri, Makoto Inoue, Sara Issaoun, David J. James, Buell T. Jannuzi, Michael Janssen, Britton Jeter, Wu Jiang, Alejandra Jimenez-Rosales, Michael D. Johnson, Adam C. Jones, Abhishek V. Joshi, Taehyun Jung, Tomohisa Kawashima, Garrett K. Keating, Mark Kettenis, Dong-Jin Kim, Jae-Young Kim, Jongsoo Kim, Junhan Kim, Motoki Kino, Jakob Knollmüller, Jun Yi Koay, Prashant Kocherlakota, Yutaro Kofuji, Patrick M. Koch, Shoko Koyama, Carsten Kramer, Joana A. Kramer, Michael Kramer, Thomas P. Krichbaum, Cheng-Yu Kuo, Noemi La Bella, Deokhyeong Lee, Aviad Levis, Shaoliang Li, Zhiyuan Li, Rocco Lico, Greg Lindahl, Michael Lindqvist, Jun Liu, Kuo Liu, Elisabetta Liuzzo, Wen-Ping Lo, Andrei P. Lobanov, Laurent Loinard, Colin J. Lonsdale, Amy E. Lowitz, Ru-Sen Lu, Nicholas R. MacDonald, Jirong Mao, Nicola Marchili, Daniel P. Marrone, Alan P. Marscher, Ivan Marti-Vidal, Satoki Matsushita, Lynn D. Matthews, Lia Medeiros, Karl M. Menten, Hugo Messias, Izumi Mizuno, Yosuke Mizuno, Joshua Montgomery, Kotaro Moriyama, Monika Moscibrodzka, Wanga Mulaudzi, Cornelia Müller, Hendrik Müller, Alejandro Mus, Gibwa Musoke, Ioannis Myserlis, Hiroshi Nagai, Neil M. Nagar, Dhanya G. Nair, Masanori Nakamura, Gopal Narayanan, Iniyan Natarajan, Antonios Nathanail, Santiago Navarro Fuentes, Joey Neilsen, Chunchong Ni, Andy Nilipour, Michael A. Nowak, Hiroki Okino, Hector Ra. l Olivares Sanchez, Feryal Ozel, Daniel C. M. Palumbo, Georgios Filippos Paraschos, Jongho Park, Harriet Parsons, Nimesh Patel, Ue-Li Pen, Dominic W. Pesce, Vincent Pietu, Alexander Plavin, Aleksandar PopStefanija, Oliver Porth, Ben Prather, Dimitrios Psaltis, Hung-Yi Pu, Alexandra Rahlin, Venkatessh Ramakrishnan, Ramprasad Rao, Mark G. Rawlings, Angelo Ricarte, Luca Ricci, Bart Ripperda, Jan Roder, Freek Roelofs, Cristina Romero-Ca. izales, Eduardo Ros, Arash Roshanineshat, Helge Rottmann, Alan L. Roy, Ignacio Ruiz, Chet Ruszczyk, Kazi L. J. Rygl, Leon D. S. Salas, Salvador Sanchez, David Sanchez-Argüelles, Miguel Sanchez-Portal, Ali SaraerToosi, Kaushik Satapathy, Saurabh, Tuomas Savolainen, Karl-Friedrich Schuster, Zhiqiang Shen, Sasikumar Silpa, Randall Smith, Bong Won Sohn, Jason SooHoo, Kamal Souccar, Joshua S. Stanway, He Sun, Alexandra J. Tetarenko, Paul Tiede, Remo P. J. Tilanus, Michael Titus, Kenji Toma, Pablo Torne, Teresa Toscano, Efthalia Traianou, Sascha Trippe, Matthew Turk, Ilse van Bemmel, Bram van den Berg, Huib Jan van Langevelde, Daniel R. van Rossum, Sebastiano D. von Fellenberg, Jesse Vos, Jan Wagner, Zhiren Wang, Derek Ward-Thompson, John Wardle, Jasmin E. Washington, Jonathan Weintroub, Maciek Wielgus, Kaj Wiik, Michael F. Wondrak, George N. Wong, Jompoj Wongphexhauxsorn, Qingwen Wu, Paul Yamaguchi, Aristomenis Yfantis, Doosoo Yoon, Andre Young, Ziri Younsi, Wei Yu, Feng Yuan, Ye-Fei Yuan, Ai-Ling Zeng, J. Anton Zensus, Shuo Zhang, Guang-Yao Zhao, J. Abhir, A. Abhishek, V. A. Acciari, A. Aguasca-Cabot, I. Agudo, I. Albanese, T. Aniello, S. Ansoldi, L. A. Antonelli, A. Arbet Engels, C. Arcaro, T. T. H. Arnesen, A. Babic, C. Bakshi, U. Barres de Almeida, J. A. Barrio, L. Barrios-Jimenez, I. Batkovic, J. Becerra Gonz. lez, W. Bednarek, E. Bernardini, J. Bernete, A. Berti, J. Besenrieder, C. Bigongiari, A. Biland, O. Blanch, G. Bonnoli, Ž. Bošnjak, E. Bronzini, I. Burelli, A. Campoy-Ordaz, A. Carosi, R. Carosi, M. Carretero-Castrillo, A. J. Castro-Tirado, D. Cerasole, G. Ceribella, A. Cervi. o, Y. Chai, G. Chon, J. L. Contreras, J. Cortina, S. Covino, P. Da Vela, F. Dazzi, A. De Angelis, B. De Lotto, M. Delfino, J. Delgado, C. Delgado Mendez, F. Di Pierro, R. Di Tria, L. Di Venere, A. Dinesh, D. Dominis Prester, A. Donini, D. Dorner, M. Doro, L. Eisenberger, D. Elsaesser, L. Foffano, L. Font, F. Fr. as Garcia-Lago, S. Fr. se, Y. Fukazawa, S. Gasparyan, M. Gaug, J. G. Giesbrecht Paiva, N. Giglietto, F. Giordano, P. Gliwny, T. Gradetzke, R. Grau, J. G. Green, P. Günther, D. Hadasch, G. Harutyunyan, J. Herrera Llorente, D. Hrupec, D. Israyelyan, J. Jahanvi, I. Jimenez Martinez, J. Jimenez Quiles, S. Kankkunen, T. Kayanoki, J. Konrad, P. M. Kouch, H. Kubo, J. Kushida, M. L. inez, A. Lamastra, E. Lindfors, S. Lombardi, F. Longo, R. Lopez-Coto, M. Lopez-Moya, A. Lopez-Oramas, S. Loporchio, L. LuliLc, P. Majumdar, M. Makariev, M. Mallamaci, G. Maneva, M. Manganaro, S. Mangano, K. Mannheim, S. Marchesi, M. Mariotti, M. Martinez, P. Maruševec, D. Mazin, S. Menchiari, J. M. ndez Gallego, S. Menon, D. Miceli, J. M. Miranda, R. Mirzoyan, M. Molero Gonzalez, E. Molina, H. A. Mondal, A. Moralejo, C. Nanci, A. Negro, V. Neustroev, C. Nigro, L. Nikolic, K. Noda, S. Nozaki, A. Okumura, J. Otero-Santos, S. Paiano, D. Paneque, R. Paoletti, J. M. Paredes, M. Peresano, M. Persic, M. Pihet, G. Pirola, F. Podobnik, P. G. Prada Moroni, E. Prandini, M. Rib., J. Rico, A. Roy, N. Sahakyan, F. G. Saturni, F. Schiavone, K. Schmitz, A. Sciaccaluga, G. Silvestri, A. Simongini, J. Sitarek, V. Sliusar, D. Sobczynska, A. Stamerra, J. Striškovic, D. Strom, Y. Suda, M. Takahashi, R. Takeishi, J. Tartera Barber., P. Temnikov, T. Terzic, M. Teshima, A. Tutone, S. Ubach, S. Ventura, G. Verna, I. Viale, A. Vigliano, C. F. Vigorito, E. Visentin, V. Vitale, M. Vorbrugg, I. Vovk, R. Walter, C. Walther, F. Wersig, P. K. H. Yeung, A. Acharyya, F. Aharonian, H. Ashkar, M. Backes, M. Barnard, Y. Becherini, M. B. ttcher, J. Bolmont, B. Bruno, T. Bylund, S. Casanova, M. Chernyakova, J. O. Chibueze, O. Chibueze, B. Cornejo, J. Damascene Mbarubucyeye, I. D. Davids, J. de Assis Scarpin, M. de Naurois, A. Dmytriiev, K. Egberts, S. Fegan, K. Feijen, M. D. Filipovic, G. Fontaine, S. Gabici, J. F. Glicenstein, P. Goswami, L. Heckmann, B. He., M. Holler, D. Horns, E. Kasai, K. Katarzynski, D. Kerszberg, B. Kh. lifi, K. Kosack, R. G. Lang, S. Lazarevic, P. Liniewicz, A. Luashvili, D. Malyshev, D. Malyshev, M. G. F. Mayer, M. Meyer, A. Mikhno, E. Moulin, H. Ndiyavala, J. Niemiec, P. Pichard, T. Preis, G. Pühlhofer, A. Quirrenbach, A. Reimer, O. Reimer, I. Reis, B. Rudak, K. Sabri, V. Sahakian, A. Santangelo, M. Sasaki, I. Shebalkova, W. Si Said, L. Stawarz, R. Steenkamp, T. Tanaka, G. L. Taylor, R. Terrier, Y. Tian, M. Tluczykont, C. Venter, J. Vink, V. Voitsekhovskyi, S. J. Wagner, A. Wierzcholska, M. Zacharias, A. A. Zdziarski,Comments: 29 pages, 13 figures, accepted by Astronomy & Astrophysics on June 18, 2026Subjects: astro-ph.HE astro-ph.GACreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
The archetypal BLAZAR 3C 279 hosts a prominent RELATIVISTIC JET and exhibits strong broadband variability across the electroMAGNETic spectrum. In April 2017, the Event Horizon Telescope (EHT) observed 3C 279, alongside one of the most extensive quasi-simultaneous multiwavelength (MWL) campaigns ever conducted. With the aim of investigating the physical processes governing 3C 279, we analyzed individual observations and multiband light curves, and constructed a new quasi-simultaneous MWL spectrum. We also performed phenomenological modeling using the turbulent extreme multi-zone (TEMZ) model to constrain the fundamental physical properties of the source. The EHT observations reveal a clear flux increase in the innermost core between April 5 and 11, 2017. Over a broader timescale, radio measurements at longer wavelengths show concurrent enhancements in core flux and POLARIZATION around mid-April, coinciding with the ejection of a superluminal knot. Record UV-optical flares with strong POLARIZATION variability occurred in late March, followed by gamma-ray activity that declined before the end of the EHT observing period. During this interval, the source remained in a low X-ray state and showed no detectable VHE emission. The TEMZ modeling suggests that the broadband spectrum and variability of 3C 279 can be explained within a JET scenario in which turbulent plasma cells are compressed by a stationary conical shock. However, alternative interpretations, such as MAGNETic RECONNECTion or a moving shock-in-JET event, remain plausible. This coordinated MWL campaign advances our understanding of the origin of JET and gamma-ray emission in 3C 279, while also providing a comprehensive publicly available dataset that will serve as a valuable reference for future studies.
[abstract 2 / 62] Wow! (score: 10) - Title: Extreme PeV accelerator associated with GRS 1915+105Authors: Zhen Cao, F. Aharonian, Y. X. Bai, Y. W. Bao, D. Bastieri, X. J. Bi, Y. J. Bi, W. Bian, J. Blunier, A. V. Bukevich, C. M. Cai, Y. Y. Cai, W. Y. Cao, Zhe Cao, J. Chang, J. F. Chang, E. S. Chen, G. H. Chen, H. K. Chen, L. F. Chen, Liang Chen, Long Chen, M. J. Chen, M. L. Chen, Q. H. Chen, S. Chen, S. H. Chen, S. Z. Chen, T. L. Chen, X. B. Chen, X. J. Chen, X. P. Chen, Y. Chen, N. Cheng, Q. Y. Cheng, Y. D. Cheng, M. Y. Cui, S. W. Cui, X. H. Cui, Y. D. Cui, B. Z. Dai, H. L. Dai, Z. G. Dai, Danzengluobu, Y. X. Diao, A. J. Dong, X. Q. Dong, K. K. Duan, J. H. Fan, Y. Z. Fan, J. Fang, J. H. Fang, K. Fang, C. F. Feng, H. Feng, L. Feng, S. H. Feng, X. T. Feng, Y. Feng, Y. L. Feng, S. Gabici, B. Gao, Q. Gao, W. Gao, W. K. Gao, M. M. Ge, T. T. Ge, L. S. Geng, G. Giacinti, G. H. Gong, Q. B. Gou, M. H. Gu, F. L. Guo, J. Guo, K. J. Guo, X. L. Guo, Y. Q. Guo, Y. Y. Guo, R. P. Han, O. A. Hannuksela, M. Hasan, H. H. He, H. N. He, J. Y. He, X. Y. He, Y. He, S. Hernández-Cadena, B. W. Hou, C. Hou, X. Hou, H. B. Hu, S. C. Hu, C. Huang, D. H. Huang, J. J. Huang, X. L. Huang, X. T. Huang, X. Y. Huang, Y. Huang, Y. Y. Huang, A. Inventar, X. L. Ji, H. Y. Jia, K. Jia, H. B. Jiang, K. Jiang, X. W. Jiang, Z. J. Jiang, M. Jin, S. Kaci, M. M. Kang, I. Karpikov, D. Khangulyan, D. Kuleshov, K. Kurinov, Cheng Li, Cong Li, D. Li, F. Li, H. B. Li, H. C. Li, Jian Li, Jie Li, K. Li, L. Li, R. L. Li, S. D. Li, T. Y. Li, W. L. Li, X. R. Li, Xin Li, Y. Li, Zhe Li, Zhuo Li, E. W. Liang, Y. F. Liang, S. J. Lin, B. Liu, C. Liu, D. Liu, D. B. Liu, H. Liu, J. Liu, J. L. Liu, J. R. Liu, M. Y. Liu, R. Y. Liu, S. M. Liu, W. Liu, X. Liu, Y. Liu, Y. Liu, Y. N. Liu, Y. Q. Lou, Q. Luo, Y. Luo, H. K. Lv, B. Q. Ma, L. L. Ma, X. H. Ma, I. O. Maliy, J. R. Mao, Z. Min, W. Mitthumsiri, Y. Mizuno, G. B. Mou, A. Neronov, K. C. Y. Ng, M. Y. Ni, L. Nie, L. J. Ou, Z. W. Ou, P. Pattarakijwanich, Z. Y. Pei, D. Y. Peng, J. C. Qi, M. Y. Qi, J. J. Qin, D. Qu, A. Raza, C. Y. Ren, D. Ruffolo, A. Sáiz, D. Savchenko, D. Semikoz, L. Shao, O. Shchegolev, Y. Z. Shen, X. D. Sheng, Z. D. Shi, F. W. Shu, H. C. Song, Yu. V. Stenkin, V. Stepanov, Y. Su, D. X. Sun, H. Sun, J. X. Sun, Q. N. Sun, X. N. Sun, Z. B. Sun, N. H. Tabasam, J. Takata, P. H. T. Tam, H. B. Tan, Q. W. Tang, R. Tang, Z. B. Tang, W. W. Tian, C. N. Tong, L. H. Wan, C. Wang, D. H. Wang, G. W. Wang, H. G. Wang, J. C. Wang, K. Wang, Kai Wang, Kai Wang, L. P. Wang, L. Y. Wang, L. Y. Wang, R. Wang, W. Wang, X. G. Wang, X. J. Wang, X. Y. Wang, Y. Wang, Y. D. Wang, Z. H. Wang, Z. X. Wang, Zheng Wang, D. M. Wei, J. J. Wei, Y. J. Wei, T. Wen, S. S. Weng, C. Y. Wu, H. R. Wu, Q. W. Wu, S. Wu, X. F. Wu, Y. S. Wu, S. Q. Xi, J. Xia, J. J. Xia, G. M. Xiang, D. X. Xiao, G. Xiao, Y. F. Xiao, Y. L. Xin, H. D. Xing, Y. Xing, D. R. Xiong, B. N. Xu, C. Y. Xu, D. L. Xu, R. F. Xu, R. X. Xu, S. S. Xu, W. L. Xu, L. Xue, D. H. Yan, T. Yan, C. W. Yang, C. Y. Yang, F. F. Yang, L. L. Yang, M. J. Yang, R. Z. Yang, W. X. Yang, Z. H. Yang, Z. G. Yao, X. A. Ye, L. Q. Yin, N. Yin, X. H. You, Z. Y. You, Q. Yuan, H. Yue, H. D. Zeng, T. X. Zeng, W. Zeng, X. T. Zeng, M. Zha, B. B. Zhang, B. T. Zhang, C. Zhang, H. Zhang, H. M. Zhang, H. Y. Zhang, J. L. Zhang, J. Y. Zhang, Li Zhang, P. F. Zhang, R. Zhang, S. R. Zhang, S. S. Zhang, S. Y. Zhang, W. Zhang, W. Y. Zhang, X. Zhang, X. P. Zhang, Yi Zhang, Yong Zhang, Z. P. Zhang, J. Zhao, L. Zhao, L. Z. Zhao, S. P. Zhao, X. H. Zhao, Z. H. Zhao, F. Zheng, T. C. Zheng, B. Zhou, H. Zhou, J. N. Zhou, M. Zhou, P. Zhou, R. Zhou, X. X. Zhou, X. X. Zhou, B. Y. Zhu, C. G. Zhu, F. R. Zhu, H. Zhu, K. J. Zhu, Y. C. Zou, X. Zuo,Comments: 25 pages, 21 figures, 10 tablesSubjects: astro-ph.HE hep-exCreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
MicroQUASARs, binary systems featuring RELATIVISTIC JETs, have emerged as sources for particle acceleration beyond PeV energies. We present a study of the broadband $γ$-ray emission from one of the most prominent Galactic microQUASARs GRS 1915+105 based on data accumulated by LHAASO and FERMI-LAT over 4 and 17 years, respectively. A joint analysis of LHAASO-WCDA and LHAASO-KM2A data reveals extended $γ$-ray emission whose centroid appears significantly shifted, by ~ 0.13°, from the binary system and its JETs. The spectral energy distribution is well described by a curved spectrum with progressive steepening that can be described by a log-parabola function with no evidence for a sharp cutoff, consistent with parent particles reaching multi-PeV energies and an extreme acceleration efficiency approaching the limit set by the available potential drop across the source. Several features, most notably the shift of the emission and single-power-law spectrum down to GeV band, favor radiation by COSMIC RAYs accelerated in the source interacting with the dense ambient medium. Our spectral modeling implies that at least a few percent of the JET mechanical power is transferred to protons, whose maximum energy reaches beyond 5 PeV. These results strengthen the case for microQUASARs as exceptionally efficient accelerators in our Galaxy.
[abstract 3 / 62] Wow! (score: 10) - Title: Unique Science Opportunities for Space VLBI Systems with the SKA TelescopesAuthors: Y. Y. Kovalev, G. Bruni, T. An, H. E. Bignall, P. G. Edwards, C. Garcia-Miro, M. Giroletti, L. I. Gurvits, M. Kadler, J. -Y. Kim, E. V. Kravchenko, I. Liodakis, Y. Q. Liu, A. V. Plavin, A. V. Popkov, A. B. Pushkarev, T. Savolainen, Z. -Q. Shen, A. Tamar, E. Traianou,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Kovalev01Subjects: astro-ph.HECreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
To date, two dedicated Space Very Long Baseline Interferometry (SVLBI) missions, the VLBI Space Observatory Programme (VSOP) and RadioAstron, have provided groundbreaking insights into the Universe at angular resolutions as fine as ~10 microarcseconds. The phased SKA-Mid, with its exceptional sensitivity and broad frequency coverage, will form a unique ground-based anchor for future SVLBI missions, driving major advances into previously unexplored regions of the angular resolution-sensitivity parameter space. The discovery of extreme brightness temperatures in BLAZARs by RadioAstron demands detailed investigation with next-generation SVLBI. Such studies are crucial for understanding particle (re-)acceleration mechanisms, with direct implications for the search for high-energy neutrino sources. Combining centimeter-wavelength SVLBI with millimeter ground-based VLBI at comparable resolutions will enable detailed studies of plasma stratification and instabilities in Active Galactic Nuclei (AGN) JETs, as well as the processes of JET formation, acceleration, collimation, and MAGNETic field evolution, for example through Faraday rotation mapping. The unprecedented sensitivity of the SKA-Mid will allow observations of ACTIVE GALACTIC NUCLEi to very high redshifts, tracing their evolution and overcoming opacity caused by the (1+z) shift of intrinsic emission frequencies. Future centimeter SVLBI experiments will also probe scattering in the interstellar medium through pulsar, maser, and AGN observations. Finally, the combination of multiple tied-array beams from the SKA telescopes and the extremely long SVLBI baselines will enable ultra-precise astrometry using the next-generation MultiView technique, allowing measurements of extragalactic parallaxes of pulsars and megamasers, proper motions of supermassive BLACK HOLEs, and even the astrometric detection of exoplanets.
[abstract 4 / 62] Wow! (score: 9) - Title: Compact RADIO GALAXies: the case of FR0sAuthors: R. D. Baldi, A. Capetti, G. Giovannini, S. Amarantidis, M. Brienza, G. Bruni, J. Chilufya, A. Costa, M. Gitti, D. V. Lal, G. Migliori, J. Moldon, M. Orienti, F. Panessa, I. Prandoni, M. Puig-Subirà, R. M. Samir, S. Shabala, F. Shankar, C. Spingola, F. Tavecchio, F. Ubertosi, B. Vaidya,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Baldi01Subjects: astro-ph.GA astro-ph.HECreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Fanaroff-Riley type 0 (FR0) RADIO GALAXies, a newly-identified and abundant population of low-power radio-loud ACTIVE GALACTIC NUCLEi, present a significant challenge to our understanding of RADIO GALAXy evolution. Unlike their more extended FRI and FRII counterparts, FR0s are characterized by compact (from pc to a few kpc) radio morphologies with weak or absent large-scale JETs, despite having optical host galaxy properties and central BLACK HOLE masses similar to classical, more powerful RADIO GALAXies. Their compactness and prevalence suggest they may represent an early stage of RADIO GALAXy evolution or indicate a fundamentally different accretion and ejection mechanism. The Square Kilometre Array (SKA), with its continuum survey and VLBI capabilities, offers a transformative opportunity to study FR0 RADIO GALAXies at unprecedented angular resolution and sensitivity. Milliarcsecond (mas) angular resolution VLBI observations will probe their parsec-scale structure, providing critical insights into the nature of their JETs, accretion-ejection physics, and the interplay between nuclear activity and the surrounding environment. Continuum and POLARIZATION surveys will enable a systematic study of their population properties, distribution, and radio spectra across a wide range of redshifts in relation to other populations of RADIO GALAXies.
[abstract 5 / 62] Wow! (score: 7) - Title: Hadronic Processes, Plasma Evolution and Neutrino Emission in Magnetic Towers of Neutron-Star Merger RemnantsAuthors: Rostom Mbarek, Jiaxi Wu, Elias R. Most,Comments: ApJLSubjects: astro-ph.HECreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Binary neutron star mergers can form short-lived MAGNETar-like remnants whose MAGNETically dominated polar towers reach $B\sim10^{15}$--$10^{16}\,\mathrm{G}$, but the microphysical composition of these outflows remains poorly understood. Combining tower geometries from GRMHD simulations with an analytic treatment of QED and hadronic processes, we argue that MAGNETic RECONNECTion is the most viable particle acceleration channel in this strongly radiative regime, where the current sheets thin to collisionless scales. Purely leptonic pair loading -- including resonant inverse Compton scattering of soft photons -- is bottlenecked by rapid pitch-angle damping and the tendency of one-photon MAGNETic conversion to populate low Landau levels. Once protons reach mildly RELATIVISTIC energies ($γ_p\gtrsim1.3$), however, inelastic proton-proton ($pp$) collisions inject large-pitch-angle pions that drive $π^0\to2γ\to e^\pm$ cascades with multiplicity $\mathcal{M}_{\rm cas}\simeq4$ at $B=10^{15}\,\mathrm{G}$, supplying the perpendicular momentum the leptonic channel cannot maintain. This hadronic route dominates pair loading and channels most of the dissipated MAGNETic energy into the $e^\pm$ population that could power the nonthermal emission emerging at larger radii. Charged-pion decay, modulated by $π^\pm$ SYNCHROTRON cooling, further seeds a nonthermal neutrino tail up to $\sim 300\,(σ_p/5)\,\mathrm{MeV}$, spectrally distinct from the thermal cooling burst and detectable from sources within $\sim 100\,\mathrm{kpc}$
[abstract 6 / 62] Yes (score: 6) - Title: Constraining the Physical Properties of Quadruply Lensed Quasars using Optical-to-X-Ray DataAuthors: Kriti Kamal Gupta, Dominique Sluse, Maarten Baes, Daniel Gilman, Anna Nierenberg, Tommaso Treu, Timo Anguita, Ryan Keeley, Pritom Mozumdar,Comments: 16 pages, 6 figures, 6 tables. Accepted for publication in A&ASubjects: astro-ph.GA astro-ph.HECreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
Gravitational lensing of luminous ACTIVE GALACTIC NUCLEi (AGN; or QUASARs) can be used as a natural telescope to zoom in on their inner structures. With more and more lensed AGN being discovered, it is extremely important to have a homogeneous study focused on constraining their key physical properties, especially the bolometric luminosity. The primary limitation for such a study is the availability of observations for a representative sample of lensed AGN in at least the optical, ultraviolet (UV), and X-ray bands, where most of the AGN emission is concentrated. In this paper, we present one of the largest multiwavelength studies of lensed AGN with the aim of accurately measuring some of the fundamental quantities, such as their bolometric luminosities, BLACK HOLE masses, and Eddington ratios. We compiled photometric and spectroscopic data in optical/UV and X-rays, for 27 quadruply lensed AGN ($0.6 < z < 3.1$) and calculated their bolometric luminosities by fitting their broadband spectral energy distributions (SEDs) with phenomenological models. We also performed spectral emission line fitting to estimate their BLACK HOLE masses using the virial method. Additionally, we compared different prescriptions to calculate the bolometric luminosities of AGN from limited data, and our results show that the luminosity-dependent 2-10 keV X-ray bolometric corrections provide unbiased and reliable predictions of the bolometric luminosity, with a maximum scatter of $\sim 0.5$ dex. The predictions from optical bolometric corrections are generally overestimated but show a lower scatter once microlensing effects are taken into account. Thanks to the compiled optical/UV and X-ray data for our lensed AGN sample, we also present the well-known UV-X-ray luminosity relation for AGN as a novel way to determine uncertainty in the magnifications of lensed AGN induced by micro- and/or millilensing.
[abstract 7 / 62] Yes (score: 6) - Title: Accreting Compact Object Binaries with the SKAAuthors: Aru Beri, Francesco Carotenuto, Rob P. Fender, James C. A. Miller-Jones, Sara Motta, Valeriu Tudose, Jakob van den Eijnden,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Beri01. Advancing Astrophysics with the SKA II (AASKAII) outlines the transformative scientific advances that will be enabled by the SKA telescopesSubjects: astro-ph.HECreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Accreting binary systems provide a time-resolved view of the accretion and ejection processes that are seen in all classes of compact objects, from stellar-mass to supermassive. They allow us to study the launching of RELATIVISTIC JETs on human timescales, probing how the JETs are coupled to the underlying accretion flow, and providing unique insights that can be extended to supermassive BLACK HOLEs via the well-established mass scale invariance. Comparative studies of JETs from different classes of compact objects allow us to determine the impact of mass, spin, MAGNETic fields, and stellar surfaces on the launching of JETs. The JETs from BLACK HOLE X-ray binaries provide probes of the Galactic BLACK HOLE population, and an important source of feedback to the surrounding interstellar medium. While existing radio facilities (including the SKA precursors) have made great progress in this field in recent years, the SKA will enhance such studies via its high point source and surface brightness sensitivity, high angular resolution, and broad frequency coverage. This will enable the extension of our existing BLACK HOLE studies to the fainter accreting neutron star and white dwarf population, the detection of previously-undiscovered systems in a low-luminosity quiescent state, and the extension of our studies to nearby galaxies, revealing rare, high-accretion rate systems that probe a key phase of BLACK HOLE growth.
[abstract 8 / 62] Yes (score: 6) - Title: Observation of A Solar Like Magnetic Reconnection Event in an AGN Corona with XRISMAuthors: Gal Vardi, Ehud Behar, Liyi Gu, Jelle Kaastra, Matteo Guainazzi, Missagh Mehdipour, Keigo Fukumura, Jon Miller, Ari Laor, Erin Kara, Megan E. Eckart, Misaki Mizumoto, Christos Panagiotou, Chen Li, Ogawa Shoji, Matilde Signorini,Comments: Submitted to APJLSubjects: astro-ph.HE astro-ph.SRCreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
The X-ray source in AGN is commonly referred to as the corona by analogy to stellar coronae. The similarities between the two suggest that the heating mechanism of AGN coronae is MAGNETic RECONNECTion -- as in cool stars -- but this has not yet been directly observed. This work presents the first observational evidence for a MAGNETic RECONNECTion flare in an AGN corona. We report on a flare in NGC 3783, which was observed with XRISM/Xtend and XMM-Newton/EPIC-PN exhibiting distinct temporal evolution in soft ($<2.0\,$keV) and hard ($>2.0\,$keV) X-rays. An Ultra-Fast Outflow (UFO) was detected during the event. The flare features the Neupert effect -- a temporal signature widely observed in the Sun, which shows that the flare is powered by MAGNETic RECONNECTion, with the UFO playing a role analogous to a solar Coronal Mass Ejection (CME). We derive an upper limit of $30 \, R_g$ on the height of the MAGNETic loop from which the flare originates. Using the UFO's measured properties to characterize the MAGNETic field, we obtain $B > 1.3 \times 10^4\,$G for the field annihilated during the flare from total energy considerations, and $B \approx 500\,$G for the momentary MAGNETic field during RECONNECTion from a dynamical consideration.
[abstract 9 / 62] Yes (score: 5) - Title: Multi-messenger and Multi-band Studies of Massive Black Holes: the Synergies Between LISA and SKAOAuthors: Pedro R. Capelo, Alberto Mangiagli, Lorenz Zwick, Lucio Mayer, Marta Volonteri,Comments: Published in Advancing Astrophysics with the SKAII (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Capelo01Subjects: astro-ph.HE astro-ph.CO astro-ph.GACreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
Depending on its mass, the same gas-embedded massive BLACK HOLE (BH) binary can emit gravitational waves (GWs) in one or more bands (nHz and mHz) concurrently, along with electroMAGNETic (EM) waves over the entire spectrum. The Square Kilometre Array Observatory (SKAO), thanks to its unparalleled sensitivity, will be pivotal in achieving coincident GW-EM (mHz-radio) and GW-GW (nHz-mHz) detections. We review the state-of-the-art predictions - achieved by means of numerical simulations and mock catalogues - of the numbers of detectable coincident GW-EM signals when employing the Laser Interferometer Space Antenna (LISA) and SKA-Mid. By exploiting the same underlying BH binary populations, to allow for a fairer comparison, we then assess the importance of a variety of EM models for the radio flares and JETs, finding that the number of radio counterparts of LISA sources is relatively insensitive to the JET/flare model employed and to whether SKA-Mid AA* or AA4 is assumed. Additionally, we describe how SKAO - as part of a pulsar timing array (PTA) - and LISA will provide the opportunity to detect the first low-frequency, multi-band (nHz-mHz) GW detection of the same object. Supermassive BH binaries embedded in gas discs are subjected to hydrodynamical torques, causing perturbations that produce additional small-amplitude, higher-frequency GWs. The main carrier GWs may thus be identifiable as a deterministic signal by SKAO-era PTAs, while the higher-frequency harmonics would shine in LISA as stochastic signals. Correlating these multi-band GWs would provide unprecedented constraints on the environment of the most massive BHs.
[abstract 10 / 62] Yes (score: 5) - Title: The kinetic-energy bottleneck in Fast Radio Burst modelsAuthors: Paz Beniamini, Pawan Kumar,Comments: 16 pages, 3 figures, submittedSubjects: astro-ph.HECreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
Most Fast Radio Burst (FRB) models invoke a two-step process in which energy released by the central engine is converted into particle kinetic energy and only subsequently radiated as coherent GHz emission. We derive model-independent constraints on FRB emission mechanisms and use them to infer the density, size, and particle Lorentz factor of the emitting region. We assess the implications for the three main classes of FRB models. (i) Inner-MAGNETospheric models violate brightness-temperature and kinetic-luminosity constraints unless particles are continuously re-accelerated in situ. Magnetar-strength MAGNETic fields can supply the required parallel electric field out to $R\lesssim10^{10} \mathrm{cm}$ with additional, model-dependent constraints. The monster-shock scenario provides such continuous acceleration, but requires particle densities exceeding the Goldreich-Julian value by $\gtrsim 10^{12}$, shifting the maser peak to $\gtrsim10^3$ GHz for typical FRB luminosities. (ii) Light-cylinder-scale forced-RECONNECTion provides continuous particle acceleration but the radio energy emitted from the compressed RECONNECTion layer is typically only $\lesssim10^{-6}$ of the injected energy. (iii) External-shock maser models satisfy kinetic-luminosity and brightness-temperature constraints. However, we show that the upstream wind is unavoidably optically thick to induced Compton scattering, independent of the model's principal parameters. Proposed escape routes - emission above the maser peak or upstream MAGNETization $σ_{\rm w}\gtrsim30$ - lead to tiny efficiencies, while the former also conflicts with narrow FRB spectra. We conclude that MAGNETospheric models operating near the neutron-star surface and incorporating continuous particle acceleration remain the most promising FRB emission scenario, subject to successful wave escape from the MAGNETosphere (discussed in the Introduction).
[abstract 11 / 62] Yes (score: 5) - Title: Bridging Theory and Observation in the SKA Era: A Cosmological Polarized Radiative Transfer Framework for Point-to-Point Polarized Sky ComparisonsAuthors: Jennifer Y. H. Chan, Alvina Y. L. On, Paul C. W. Lai, Kinwah Wu,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Chan01Subjects: astro-ph.CO astro-ph.GACreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
Realizing the full scientific potential of the SKA requires not only revolutionary instrumentation but also accurate modeling of light propagation in an evolving, expanding Universe, in order to translate intensity and POLARIZATION data into physical insight about MAGNETic fields and cosmic plasma. When all-sky cosmological polarized radiative transfer (CPRT) calculations meets SKA observations, theory and data interlock to deliver a predictive, and testable picture of the evolving MAGNETo-ionic Universe. This synergy transforms POLARIZATION observations -- assembled into empirical maps of diffuse emission and rotation-measure (RM) grids of discrete sources -- from descriptive data products into powerful astrophysical probes, advancing our understanding of cosmic MAGNETism across space and time. The CPRT formalism -- derived from fundamental conservation laws and incorporating RELATIVISTIC, cosmological, and full radiative-transfer effects -- provides a robust platform and a common framework for observers, theorists, and simulation experts to pursue shared scientific goals. Observers gain synthetic templates to interpret RM grids and POLARIZATION maps; theorists can directly confront models of MAGNETogenesis and MAGNETic-field evolution with data; and simulation experts obtain a post-processing tool to transform cosmological MAGNETo-hydrodynamic (MHD) outputs into observable skies. Furthermore, CPRT serves as a powerful testbed when traditional RM-based methods reach their limitations -- for example, in interpreting complex Faraday spectra, disentangling multiple intervening MAGNETized media, or achieving a coherent picture when diverse observational diagnostics -- such as dispersion measure, SYNCHROTRON emission and spectral index, and dust POLARIZATION -- are combined.
[abstract 12 / 62] Yes (score: 5) - Title: 3D particle-in-cell simulations of pulsar wind-disk interaction: application to the transitional millisecond pulsar PSR J1023+0038Authors: Valentina Richard-Romei, Benoît Cerutti, Alessandro Papitto, Riccardo La Placa,Comments: 11 pages, 11 figures, submitted to A&ASubjects: astro-ph.HECreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
Transitional millisecond pulsars constitute a peculiar subclass of neutron stars in which the pulsar alternates between accretion-powered and rotation-powered states, depending on the variations in the mass accretion flow coming from a low-mass companion star. A third intermediate state, referred to as ``sub-luminous disk state'', has been identified. During this state, observations indicate the presence of a disk surrounding the pulsar, and the system exhibits intriguing features, such as broad optical and X-ray pulsations characterized by a high luminosity. To date, no ab initio model of a pulsar wind interacting with an accretion disk has been developed to address these observables. We perform three-dimensional particle-in-cell simulations of a pulsar MAGNETosphere surrounded by a perfectly conducting torus to model the interaction between the pulsar wind and the disk. We find that the presence of the disk induces a significant reconfiguration of the MAGNETosphere compared to the rotation-powered state, leading to enhanced plasma density at the inner disk boundary, increased MAGNETic field strength, and more efficient plasma isotropization and particle acceleration. As a result, the SYNCHROTRON radiation is substantially enhanced, and characterized by a strong continuous component and either one or two-peaked light curves, depending on the pulsar's MAGNETic obliquity. The POLARIZATION degree is reduced compared to isolated systems, and its energy dependence is explored. The rotation of the POLARIZATION angle can also be altered, depending on the observer's viewing angle. The model successfully reproduces some of the main features of the optical and X-ray pulsed emission originating from PSR J1023+0038, thereby corroborating the scenario in which these pulsations originate from SYNCHROTRON radiation generated as the pulsar wind interacts with the inner edge of the disk.
[abstract 13 / 62] Yes (score: 5) - Title: Probing Physical Conditions in Classical and Symbiotic Novae with the Square Kilometre Array ObservatoryAuthors: Rocco Lico, Marcello Giroletti, Arnau Aguasca-Cabot, Joris Kersten, Benito Marcote, Ulisse Munari, Miriam M. Nyamai, Timothy J. O'Brien, Zsolt Paragi, Iris de Ruiter, Kirill Sokolovsky, David R. A. Williams,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Lico01. Advancing Astrophysics with the SKAII (AASKAII) outlines the transformative scientific advances that will be enabled by the SKA telescopesSubjects: astro-ph.HE astro-ph.SRCreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Cataclysmic variables and symbiotic stars are interacting binary systems in which a hot white dwarf (WD) orbits a companion main-sequence or red giant star, respectively. Accumulation of hydrogen-rich material on the WD surface may trigger re-ignition of thermonuclear reactions that, under degenerate conditions, lead to an explosive ejection of the accreted layer mixed with WD material. These explosions, known as classical novae, provide opportunities to study key astrophysical processes such as binary evolution, accretion, ionisation of circumstellar material, mass ejection, JET formation, and thermonuclear burning. Radio emission in these systems arises from both thermal and non-thermal processes, which manifest differently in classical and symbiotic novae. $γ$-ray emission has also been detected in several cases, and recent progress, driven by coordinated radio and multiwavelength observations, has greatly advanced our understanding of both types of novae. Multi-frequency, multi-epoch, and multi-scale interferometric observations are powerful probes of the evolving physical conditions following thermonuclear explosions, revealing information from both ionised and RELATIVISTIC particle populations. The SKAO, particularly its SKA-Mid component, will enable regular monitoring of Galactic novae, multiple times per year for classical novae and every few years for symbiotic systems. It will explore a wide range of conditions, including companion types, WD masses, accretion regimes, and surrounding environments. The VLBI capabilities of the SKAO will target compact shocked regions, while its exceptional sensitivity will also allow characterisation of emission during quiescent phases of the binaries.
[abstract 14 / 62] Yes (score: 5) - Title: A MAGNETically-supported disk-corona model for Changing-Look AGN transitionsAuthors: Marios Kouzis, Agata Różańska, Debora Lančová, Bożena Czerny, Dominik Gronkiewicz,Comments: 10 pages, 6 figures, 1 table, Submitted to ApJLSubjects: astro-ph.HECreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Changing-Look Active Galactic Nuclei (CLAGN) undergo dramatic spectral and luminosity transitions on timescales of months to a few years -- orders of magnitude shorter than the viscous timescale of a standard $α$-disk at the radii where the optical/UV continuum is generated, for typical supermassive BLACK HOLE masses. We show that a MAGNETically supported disk-corona model reproduces \emph{both} the observed Eddington ratio at which changing event occurs and the observed transition duration. Using the \texttt{diskvert} code, which solves the steady vertical structure under simultaneous gas, radiation and MAGNETic pressure support with a self-consistent warm corona, we (i) construct thermal-viscous S-curves, and (ii) calculate the integrated thermal timescale together with the front propagation timescale. We compute a large grid of models of different BLACK HOLE masses, Eddington ratios, MAGNETic viscosities, and disk radii, showing that MAGNETized disks push the S-curve knee down to an Eddington ratio of $ \approx 0.01-0.03$, and introduce a new stable branch of high luminosity solutions, while the limit-cycle timescale enters the months-to-years range for $M_\mathrm{BH} = 10^{7}-10^{9}\,\mathrm{M_\odot}$. Confronted with a sample of five CLAGN (Mkn 590, NGC 1566, IRAS 23226$-$3843, Mkn 1018, NGC 2617), the model jointly reproduces the empirical Eddington rates and the observed event durations only when the inner disk is strongly MAGNETized. The case of Mkn 590 is especially constraining: the recent tightly-determined transition Eddington ratio is matched by a highly MAGNETized disk-corona flow at small radii.
[abstract 15 / 62] Yes (score: 5) - Title: The SKA View of Cool-core Clusters: Evolution of Radio Mini-halos and AGN FeedbackAuthors: Myriam Gitti, Paolo Tozzi, Francesco Ubertosi, Annalisa Bonafede, Gianfranco Brunetti, Rossella Cassano, Stefano Ettori, Luigina Feretti, Marie-Lou Gendron-Marsolais, Simona Giacintucci, Julie Hlavacek-Larrondo, Alessandro Ignesti, Giulia Macario, Mamta Pandey-Pommier, Tiziana Venturi,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Gitti01. Advancing Astrophysics with the SKA II (AASKAII) outlines the transformative scientific advances that will be enabled by the SKA telescopesSubjects: astro-ph.COCreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
In about 70 per cent of relaxed, cool-core galaxy clusters, the brightest cluster galaxy (BCG) is radio loud, showing non-thermal radio JETs and lobes ejected by the central ACTIVE GALACTIC NUCLEus (AGN). In recent years such RELATIVISTIC plasma has been shown to interact with the surrounding thermal intra-cluster medium (ICM) as revealed by striking images where radio lobe fill the cavities in the X-ray-emitting gas. This "radio-mode feedback" phenomenon is widespread and crucial for understanding the physics of cluster cores and the properties of the central BCG. Mechanically-powerful AGN are expected to drive turbulence in the central ICM which may also contribute to the origin of non-thermal emission on cluster-scales. Diffuse non-thermal emission has been observed in many cool-core clusters in the form of a radio mini-halo surrounding the radio-loud BCG on scales comparable to the cooling radius. Large samples of mini-halos are essential to clarify their origin and their link with the thermal and dynamical properties of clusters, especially in view of future high-resolution X-ray studies with NewAthena X-IFU. All-sky surveys with the SKA-Mid telescope at arcsecond resolution would have the potential to detect up to about 3500 mini-halos at redshift z<1 (compared to the few tens currently known). Deep Tier surveys with the SKA-Mid at sub-arcsecond resolution would further enable a complete census of radio-loud BCGs down to 1.4 GHz powers of 10^23 W/Hz up to z~2. This will provide a comprehensive view of AGN feedback and its role in shaping large scale structures.
[abstract 16 / 62] Yes (score: 5) - Title: The Cosmic Ray Life Cycle in Galaxy ClustersAuthors: Francesco de Gasperin, Marcus Brüggen, Henrik Edler, Reinout J. van Weeren, Tiziana Venturi, Gianfranco Brunetti,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/deGasperin01Subjects: astro-ph.COCreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Within the cosmic web, gravitational energy, linked to the formation and growth of the Universe's largest structures and the activity of ACTIVE GALACTIC NUCLEi (AGN), is converted to heat through processes such as turbulence and shock waves. These processes have a fundamental impact on the evolution of galaxy clusters. For example, they lead to the amplification of MAGNETic fields and the production of COSMIC RAY (CR) electrons that emit continuum radio waves via SYNCHROTRON emission. This produces sources on scales of the entire hosting clusters. These large radio sources in galaxy clusters are often classified based on their morphological appearance as radio halos, cluster radio shocks (radio relics), and other types. To understand the CR acceleration processes in galaxy clusters (and beyond), and to gain a comprehensive view of these sources, including their long-term interactions, SKA telescope should conduct both deep observations of a carefully selected sample of nearby clusters as well as shallower wide-area surveys. Thanks to their capabilities - in particular the sensitivity to polarised and low-frequency emission - SKA-Mid (Bands 1 and 2) and SKA-Low are ideally suited to probing MAGNETic field structures in galaxy clusters, as well as the large reservoir of low-energy CRs that may be accelerated by yet-unexplored microphysical mechanisms. The high sensitivity to low-frequency emission will also be fundamental to detect the long term actions and interactions of these phenomena over gigayear timescales.
[abstract 17 / 62] Yes (score: 4) - Title: Dark Matter Heating of Compact Stars Beyond Capture: A Relativistic Framework for Energy Deposition by Particle BeamsAuthors: Jaime Hoefken Zink, Shihwen Hor, Maura E. Ramirez-Quezada,Comments: 26 pages, 4 figures, version for JHEP (accepted)Subjects: hep-ph astro-ph.HECreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Compact astrophysical objects, such as neutron stars and white dwarfs, can act as detectors of energetic particle fluxes originating from astrophysical accelerators. While most existing capture and heating calculations assume isotropic very low energetic incident fluxes from the halo DARK MATTER, many realistic sources produce highly directional beams or JETs, for which gravitational focusing, trajectory multiplicity, and local energy deposition must be treated consistently. In this work, we develop a general RELATIVISTIC formalism to compute the local density, capture probability, and energy deposition of particles arriving as directed beams onto compact objects. The framework is based on the mapping of an asymptotic particle flux to local densities through geodesic congruences, allowing for gravitational focusing, multi-stream regions, and optical depth effects to be incorporated in a unified way. The formalism applies to arbitrary particle species and interaction models, and separates capture from through-going energy deposition in a frame-consistent manner. As an explicit application, we consider RELATIVISTIC particle beams generated in astrophysical JETs and evaluate their interaction with two compact objects samples: a white dwarf and a neutron star. In particular, we illustrate the framework using boosted DARK MATTER produced in a list of 324 BLAZARs as a representative case study, computing the resulting fluxes and the associated heating in the selected stars. Additional regimes such as the interaction roof and geometric limit are discussed, highlighting the conditions under which compact objects can efficiently convert incident beam energy into observable heating.
[abstract 18 / 62] Yes (score: 4) - Title: Compact Objects Revealed by SKA and SKA-VLBIAuthors: Z. H. Lin, Y. J. Li, C. J. Hao, J. J. Li, Y. W. Dong, D. J. Liu, Y. Xu,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026(arXiv:2606.20366). Report-no:AASKAII/Lin01Subjects: astro-ph.HECreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Compact objects represent a crucial interdisciplinary frontier between astronomy and fundamental physics.The SKA/SKA-VLBI, with exceptional sensitivity (at $μ$Jy levels) and ultrahigh positional precision (at $μ$as levels), will enable direct, precise measurements of orbital dynamics in compact objects including BLACK HOLEs and neutron stars. This facility is expected to achieve at least three breakthroughs: (1) Developing effective methodologies for detecting and identifying BLACK HOLE-neutron star binaries to construct observational catalogues, thus advancing investigations into the equation of state of ultra-dense nuclear matter and strong-field RELATIVISTIC effects; (2) Determining critical parameters such as orbital elements and component masses in compact binaries, yielding insights into stellar structures and evolutionary mechanisms under extreme conditions; (3) Identifying intermediate-mass BLACK HOLEs and measuring their masses to deepen understanding of BLACK HOLE formation and evolution.
[abstract 19 / 62] Yes (score: 4) - Title: Study of Polarized Emission in Radio Halos and Filaments in the SKA Telescopes EraAuthors: Valentina Vacca, Federica Govoni, Matteo Murgia, Paolo Marchegiani, Hui Li, Myriam Gitti, Francesca Loi, Luigina Feretti, Ettore Carretti, Elia Battistelli, Andrea Cabriolu, Torsten A. Ensslin, Chiara Ferrari, Gabriele Giovannini, Richard A. Perley,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026(arXiv:2606.20366). Report-no:AASKAII/Vacca01. Advancing Astrophysics with the SKAII (AASKAII) outlines the transformative scientific advances that will been enabled by the SKA telescopesSubjects: astro-ph.COCreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Synchrotron diffuse emission in merging galaxy clusters and along filaments connecting them demonstrates the presence of RELATIVISTIC particles and MAGNETic fields in these environments. The study of the polarized signal associated with this emission represents a powerful tool to constrain the properties of intracluster MAGNETic fields and the physics of acceleration and transport of RELATIVISTIC particles. Despite technological progress, detecting this polarized signal is still very challenging. In order to shed light on the capabilities of the SKA telescopes to study this emission, we use the data of cosmological MAGNETo-hydro-dynamic simulations to predict the expected polarized surface brightness of diffuse SYNCHROTRON sources from the center of galaxy clusters to filaments of the cosmic web at 1.4 GHz. We explore the possibility to detect these sources with a POLARIZATION survey with SKA-Mid with AA4 telescopes and compare the results with those from pointed observations corresponding to longer exposure times. These simulations provide precious information to understand the potential of the SKA telescopes for studying the origin and evolution of cosmological MAGNETic fields. We discuss how these observations can be used in order to characterize the MAGNETic field and the distribution and energy content of the radio emitting plasma and to shed light on the link between non-thermal and thermal properties and the dynamical state of the system.
[abstract 20 / 62] Yes (score: 4) - Title: AGN Jets from Formation to DissipationAuthors: A. -K. Baczko, Eleni Vardoulaki, Etienne Bonnassieux, Manel Perucho, Marisa Brienza, Marcus Brüggen, Emmanuel K. Bempong-Manful, Robert Beswick, Florian Eppel, Damien Gratadour, Jonas Heßdörfer, Kiara Hervella-Seoane, Matthias Kadler, Jae-Young Kim, Aretaios Lalakos, Leah K. Morabito, Dhanya G. Nair, Felix Pötzl, Jack Radcliffe, Luca Ricci, Eduardo Ros, Jan Röder, Florian Rösch, Ainara Saiz-Pérez, Hrishikesh Shetgaonkar, Cyril Tasse, Francesco Ubertosi, Jun Yang, J. Anton Zensus,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Baczko01Subjects: astro-ph.GACreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Active Galactic Nuclei (AGN) are among the most energetic phenomena in the Universe, capable of launching powerful RELATIVISTIC JETs that extend from sub-parsec to megaparsec scales. These JETs play a crucial role in regulating STAR FORMATION, redistributing energy and matter, and shaping the evolution of galaxies and their environments. Despite decades of study, a comprehensive understanding of how AGN JETs form, propagate, and dissipate remains elusive. The aim of this chapter is to highlight how the future capabilities of the the Square Kilometre Array (SKA), as a standalone array as well as in combination with Very Long Baseline Interferometry (VLBI) arrays and multi-wavelength facilities, will transform our capabilities to study the co-evolution of AGN JETs and their host galaxies from JET formation to dissipation scales.
[abstract 21 / 62] Yes (score: 4) - Title: Jets and Outflows in Young Stellar Objects with the SKAOAuthors: Giovanni Sabatini, Gemma Busquet, Carlos Carrasco-González, Adriana Rodríguez-Kamenetzky, Codella Claudio, Linda Podio, Antonio Martínez-Henares, Josep Miquel Girart, Marta De Simone, Luca Cacciapuoti, Guillem Anglada, Lukasz Tychoniec, Lisa Giani, Manoj Puravankara, Francesca Bacciotti, Rafael Bachiller, Eleonora Bianchi, Guillermo Blázquez-Calero, Tyler L. Bourke, Stefano Bovino, Paola Caselli, Francesco Cavallaro, Cecilia Ceccarelli, Elena Diaz-Marquez, Stefano Facchini, Antonio Garufi, Greta Guidi, Tomoya Hirota, John D. Ilee, Adriano Ingallinera, Izaskun Jiménez-Serra, Valerio Lattanzi, Chin-Fei Lee, Manuela Lippi, Alessandro Lupi, Liton Majumdar, Mayank Narang, Mayra Osorio, Marco Padovani, Jaime Pineda, Isaac Radley, Basmah Riaz, Luis Felipe Rodríguez, Alvaro Sánchez-Monge, Alberto Sanna, Silvia Spezzano, Leonardo Testi, Claudia Toci, Alessio Traficante, Himanshu Tyagi, Grazia Maria Umana,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Sabatini01. Advancing Astrophysics with the SKA II (AASKAII) outlines the transformative scientific advances that will be enabled by the SKA telescopesSubjects: astro-ph.GA astro-ph.SRCreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Jets and outflows are ubiquitous phenomena associated with the formation of young stellar objects (YSOs). They play a crucial role in removing angular momentum from the accreting system and in regulating star-formation efficiency. Theoretical studies and observations with ALMA and VLA have shown that JETs and winds may have a crucial role in promoting dust growth in the envelope-disc system and in shaping the physical and chemical properties of the surrounding environment. Despite these significant advances, many fundamental questions remain unanswered regarding the acceleration, collimation, and chemical impact of JETs and outflows from YSOs. The SKA-project will overcome the limitations of current mm/cm-facilities by enabling high-angular resolution and high-sensitivity cm-observations, crucial for probing JETs/outflows near YSOs. Radio recombination lines, combined with proper motions, offer a unique opportunity to study the 3D-kinematics of JETs. Non-thermal linearly polarised SYNCHROTRON emission will allow measuring MAGNETic field strength and morphology at unprecedented scales of a few au. Observations of dust emission in outflow cavities will allow studying how dust grows and is eventually transported from the disc to the envelope and back. Finally, the SKA-project will allow exploring the dust composition and chemical enrichment in shocks, where sputtering/shattering of grains cause the release of their mantles and refractory cores in the gas-phase. Complementary to ALMA's detection of simple and complex organic molecules, the SKAO will probe, for the first time, long carbon chains/rings, several Cl-, Al-, Mg-, and other metal-bearing species (missed by current sub-mm facilities).
[abstract 22 / 62] (score: 3) - Title: FastQSL 2: A Comprehensive Toolkit for Magnetic Connectivity AnalysisAuthors: Jun Chen, Thomas Wiegelmann, Li Feng, Chaowei Jiang, Rui Liu,Comments: 18 pages, 6 figuresSubjects: astro-ph.SRCreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
We present a new version of FastQSL for locating quasi-separatrix layers (QSLs) -- regions characterized by strong MAGNETic connectivity gradients, preferential current buildup, and subsequent MAGNETic RECONNECTion. This version now supports spherical coordinates, utilizing a second spherical coordinate system for tracing MAGNETic field lines around the polar regions. This approach completely resolves the singularity problem at the two poles. Furthermore, our code accommodates arbitrary mesh shapes for output, can provide both MAGNETic field and electric current density on the mesh, and can save the traced MAGNETic field lines. We suggest using $Q_\mathrm{local}$ calculated through a localized mapping to locate (quasi-)separators. By quickly and accurately outputting the footpoint coordinates of MAGNETic field lines, FastQSL can be used to derive the two key parameters used for modeling solar wind speed and slip-squashing factors for the case of zero boundary flow. Compared with the first version, FastQSL 2 achieves significant improvements in terms of application scope.
[abstract 23 / 62] (score: 3) - Title: Black Hole Occupation Fraction: Dependence on Black Hole Mass Threshold, Environment, Resolution and RedshiftAuthors: Emanuele Contini, J. K. Jang, Jinsu Rhee, Changjo Seo, Sukyoung K. Yi,Comments: 16 pages, 7 figures. Submitted to ApJ, comments welcome!Subjects: astro-ph.GACreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
We take advantage of the state-of-the-art semi-analytic model \texttt{FEGA25} \citep{contini2025}, run on merger trees extracted from three DARK MATTER-only cosmological simulations, to study the relation between the BLACK HOLE (BH) occupation fraction, $f_{\rm BH,occ}$, and galaxy stellar mass as a function of BH mass threshold, galaxy type, simulated volume, numerical resolution, sampled galaxy population, and redshift. \texttt{FEGA25} includes an improved treatment of ACTIVE GALACTIC NUCLEus feedback and does not impose a pre-existing BH seed population: BHs grow naturally through QUASAR and radio modes. Starting from the prerequisite that \texttt{FEGA25} reproduces the observed BH mass function from at least $z=2$ to the present day, our analysis leads to several results. We find that $f_{\rm BH,occ}$ increases with stellar mass, but that its normalization and shape depend strongly on the adopted BH mass threshold and on the relative contribution of central and satellite galaxies. The relative behavior of central and satellite galaxies depends on the simulation box and BH mass threshold, while the global relation should be interpreted as a population-weighted quantity. We also find significant box-to-box variations, reflecting the combined impact of numerical resolution, simulated volume, and sampled galaxy population. The redshift evolution is not universal: YS50 and the \texttt{NewCluster} zoom-in simulation show a trend qualitatively similar to that reported by \citet{tremmel2024}, whereas larger-volume boxes show the opposite behavior. Finally, comparison with other studies shows that the inferred occupation fraction is highly sensitive to BH mass threshold, simulated volume, numerical resolution, and sampled galaxy population.
[abstract 24 / 62] (score: 3) - Title: Beyond the Tayler instability: A new global instability of toroidal MAGNETic fields in starsAuthors: Mikhail E. Gusakov, Laura Becerra, Elena M. Kantor, Andreas Reisenegger, Juan Alejandro Valdivia,Comments: 44 pages, 12 figures, 3 tables, accepted in Phys. Rev. DSubjects: astro-ph.SR astro-ph.HE physics.flu-dyn physics.plasm-phCreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
Stellar toroidal MAGNETic fields are known to be unstable to the Tayler instability. Here we demonstrate the existence of a complementary current-driven instability of essentially arbitrary toroidal-field configurations in stably stratified nonrotating stars with the following properties: (i) in ideal MAGNETo-hydrodynamics, it grows on the Alfvén timescale $τ_{\rm A}$; (ii) under certain conditions, it may reveal itself by driving shellular differential rotation about an arbitrary axis perpendicular to the MAGNETic-field symmetry axis; (iii) it is large-scale in the angular directions $θ$ and $φ$, and develops at radial wave-numbers $k \lesssim \mathcal{N}τ_{\rm A}/R$, where $\mathcal{N}$ is the Brunt-Väisälä frequency and $R$ is the stellar radius. Thus, unlike the Tayler instability, the proposed instability is intrinsically global. Consequently, it may be less susceptible to dissipative suppression than the Tayler instability and can prevail over it in some regimes. This instability may have broad implications for MAGNETic field generation in stars and could modify scenarios of MAGNETic field amplification within the Tayler-Spruit dynamo, contributing to models of efficient angular-momentum transport and chemical mixing in stellar interiors.
[abstract 25 / 62] (score: 3) - Title: X-rays Mark the Spot: The Effects of Reduced Metallicity on X-ray AGN Obscuration at High RedshiftAuthors: Yash A. Gursahani, Christopher S. Reynolds,Comments: 27 pages, 16 figures, 3 tables. Accepted for publication in ApJSubjects: astro-ph.HECreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
The James Webb Space Telescope has pushed the frontier of high-redshift galaxy and ACTIVE GALACTIC NUCLEus (AGN) observations firmly past $z=10$. Corresponding to the first 500 Myr after the Big Bang, this coincides with the epoch of supermassive BLACK HOLE seeding and their early growth, much of which is likely to occur in highly obscured environments. In this work, we investigate the expected X-ray properties of these obscured AGNs focusing on the impact of the significantly lower iron abundance predicted at such early times. We use Monte Carlo methods to model the radiative transfer of X-rays from a central AGN through a surrounding torus of cold gas, characterizing the emergent X-ray spectrum as a function of the metallicity, opening angle of the torus, and column density. Motivated by expectations of high-$z$ systems, we focus on Compton-thick obscurers with columns $N_H=10^{24}-10^{25}\,{\rm cm}^{-2}$. We find that decreased metallicity can significantly increase the fraction of X-ray photons that escape the torus, improving the prospects of detecting these very high-$z$ AGNs. The covering fraction of the obscurer (i.e. torus opening angle) plays a complex role, with repeated scatterings across the interior of the torus (isotropizing the emission) competing with escape through the opening, producing geometric beaming. Additionally, we explore non-solar abundance ratios that mimic the delay-time distribution of Type Ia SUPERNOVAe. We use our models to address the detectability of highly obscured $z=10$ AGNs in next-generation, high-angular resolution X-ray surveys.
[abstract 26 / 62] (score: 3) - Title: An SKA-Low RM Grid for constraining the origin of cosmic MAGNETismAuthors: Shane P. O'Sullivan, Franco Vazza, Ettore Carretti, Valentina Vacca, Francesca Loi,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/OSullivan01Subjects: astro-ph.CO astro-ph.GACreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
Understanding the origin and evolution of cosmic MAGNETic fields is a key science goal for the SKAO. Recent advances in metre-wavelength (m-$λ$) Faraday rotation measure (RM) grids are enabling precision probes of cosmic MAGNETism, with implications extending to early-Universe physics, AGN feedback, and the MAGNETized circumgalactic medium. Here we model the m-$λ$ polarized source counts to predict an RM Grid density with SKA-Low of $N(>P) \sim 5 ({P}/{100{\rm μJy}})^{-0.75}\,\, {\rm deg}^{-2} $, where $P$ is the polarized intensity detection threshold. This represents at least an order of magnitude improvement over the current state-of-the-art. For a representative wide-area SKA-Low AA4 survey covering 10,000 deg$^2$ in $\sim$3,200 hours, we predict more than 50,000 RMs. Coupled with an expected RM precision of $\sim$0.05 rad/m$^2$, SKA-Low promises to produce the leading RM Grid survey for constraining the origin of cosmic MAGNETism in the SKA era. These predictions can be partially tested during the Science Verification phase using the AA* Sky Model data. For example, at a nominal detection threshold of 240~$μ$Jy/beam (8 times the noise in Stokes $Q$ and $U$), we expect $\sim$2.6 RMs/deg$^2$ (5x the current best m-$λ$ RM Grid density). Combining both wide-area and all-sky data, SKA-Low could detect up to 100,000 m-$λ$ RMs across its observable sky. Finally, we demonstrate new constraints on the origin of cosmic MAGNETism by comparing cosmological MHD simulations with the LOFAR m-$λ$ RMs, and highlight the transformative advances an SKA-Low RM Grid will enable for precision studies of cosmic MAGNETism.
[abstract 27 / 62] (score: 3) - Title: A toroidally spectral field solver in the X-point Gyrokinetic Code for accurate simulation of reduced MAGNETo-hydrodynamic modesAuthors: Robert Hager, C. S. Chang, Thomas Gade, Eric Held, Seung-Hoe Ku, Alexey Mishchenko, Aaron Scheinberg, Benjamin Sturdevant,Comments:Subjects: physics.plasm-phCreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
A new field solver has been implemented in the global electroMAGNETic total-$f$ gyrokinetic particle-in-cell code XGC to extend the code's capability to large-scale reduced MHD-type instabilities in tokamak plasma. While XGC's regular field solver is accurate at typical microturbulence scales of the order of the ion Larmor radius in tokamaks with arbitrary aspect ratio, a more accurate field solver is required for large-scale (i.e., low toroidal mode number) MHD-type modes such as internal kink, tearing and peeling modes. The higher accuracy of the new field solver is achieved by dropping the (large aspect ratio) assumption that the poloidal MAGNETic field is much smaller than the toroidal MAGNETic field, while its numerical complexity is controlled by using a spectral discretization in the toroidal direction. To cover the entire spectrum from large-scale MHD-type modes to small-scale microturbulence, the regular and the new field solver can be run alongside each other. This work details the derivation of the new field solver, analyzes the differences between the XGC's regular and new field solvers, and verifies the new field solver against analytic predictions and the gyrokinetic code ORB5 and the MHD code NIMROD.
[abstract 28 / 62] (score: 3) - Title: Constraints on Line-of-Sight Acceleration from O1-O4Authors: Labani Roy, Alexander H. Nitz,Comments: 13 pages including references, 14 figures, data release at URL - https://github.com/labani-01/LOS-acceleration_LIGO-peSubjects: astro-ph.HE gr-qcCreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
A compact binary will experience a center-of-mass (CoM) acceleration in the vicinity of a massive third object. The line-of-sight (LOS) component of this acceleration is imprinted on gravitational waves produced by the compact binary as a time-varying Doppler shift. The observation of a non-zero LOS acceleration may indicate the binary is in a dense environment, such as an ACTIVE GALACTIC NUCLEus (AGN) disk or nuclear star cluster, etc. We measure the LOS acceleration of all compact binaries observed through the first part of the fourth observing run (O1-O4a) of Advanced LIGO and Virgo in addition to select binaries from later observing runs. We introduce a new method to model the LOS acceleration by directly applying the time-varying Doppler shift in the time domain to the signal produced in the binary's frame; this method can be applied to any waveform model including those with higher order modes, eccentricity, and precession. We find the LOS acceleration for all known binaries to date is consistent with zero. We find that the effects of eccentricity and LOS acceleration are partially degenerate as observed in binaries such as GW200105. Current ground-based observatories are sensitive enough to only constrain scenarios that produce high accelerations, e.g $\sim 10^{-2~}(10^{-5})~\textrm{c}/s$ for BBH (BNS) sources, however, next-generation observatories may be able to constrain the accelerations expected in some dense environments.
[abstract 29 / 62] (score: 3) - Title: Solar Radio Burst Fine StructuresAuthors: Eduard Kontar, Daniel Clarkson, Hamish Reid, Yingjie Luo, Nicolina Chrysaphi, Alexey Kuznetsov, Galina Motorina, Carine Briand,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Kontar01Subjects: astro-ph.SRCreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Solar radio bursts exhibit intricate variability in time, space, and frequency, often displaying a rich variety of fine frequency-time structures such as spikes, drift pairs, striae in Type III bursts, and herringbone patterns in Type II bursts, etc. Historically, limited spatial, spectral, and temporal resolution has hindered detailed investigation of these narrow-band, rapidly evolving features, restricting progress in identifying their physical origins and underlying processes at these scales. Advances in high-time-frequency-resolution solar imaging now offer transformative opportunities. Recent sub-second imaging spectroscopy has revealed that many fine structures challenge existing theoretical models, pointing to the need for new frameworks and a reassessment of current interpretations. The Square Kilometre Array (SKA), with its full-Stokes imaging spectroscopy at sub-second cadences, will provide unprecedented data essential for resolving these long-standing questions. These capabilities promise to significantly deepen our understanding of electron acceleration and transport, MAGNETic RECONNECTion, and coronal plasma turbulence, thereby advancing our knowledge of solar energetic processes and improving assessments of their space-weather impacts.
[abstract 30 / 62] (score: 3) - Title: Probing High-redshift Intracluster Medium Using SKAAuthors: Ramananda Santra, Ruta Kale,Comments: Published in Advancing Astrophysics with the SKAII(AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Santra01. Advancing Astrophysics with the SKA II (AASKAII) outlines the transformative scientific advances that will be enabled by the SKA telescopesSubjects: astro-ph.CO astro-ph.GACreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Galaxy clusters host vast reservoirs of MAGNETised plasma in their intracluster medium (ICM), where turbulence and shocks generated during structure formation sometimes give rise to diffuse SYNCHROTRON emission in the form of radio halos and relics. However, the origin and amplification of the MAGNETic field in the ICM remains among the least understood problems, particularly at high redshift, where direct detections are scarce. Recent observations of clusters at z $\gtrsim 0.6$ have revealed radio powers of the diffuse sources comparable to those of nearby systems, implying that efficient MAGNETic amplification suppressed inverse Compton losses. Such rapid growth of the MAGNETic fields after a few Gyrs of the Big Bang challenges standard dynamo timescales, and it raises fundamental questions about the mechanisms that strengthened cluster MAGNETic fields. In this chapter, we highlight the massive merging system El Gordo (ACT-CL J0102$-$4915, z$\sim$0.87) as a unique testbed for investigating theoretical models under extreme conditions. Proposing as a SKA science verification target, El Gordo will allow detailed studies of the ICM MAGNETic field structure, strength through broadband continuum and polarisation measurements with SKA-Low and SKA-Mid, across staged deployments starting from AA0.5 to AA4, reaching a physical resolution of $\sim$ 20-30 kpc at our redshift of interest. We further outline how upcoming SKA surveys will build statistical samples of high-redshift clusters, enabling tests of different models of MAGNETic fields and COSMIC RAYs in the formation of large-scale structure.
[abstract 31 / 62] (score: 3) - Title: Multi-Band Optical Variability of Blazar 1ES 2344+514 on Diverse Time-ScalesAuthors: Aykut Özdönmez,Comments: 18 pages, 6 figures, 4 tables. Published in "Journal of Advanced Research in Natural and Applied Sciences" supported by Canakkale Onsekiz Mart UniversitySubjects: astro-ph.HECreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
This study presents the results of multi-band observations from 2022 to 2024 and Zwicky Transient Facility (ZTF) observations from 2018 to 2023, examining the flux variability of the BLAZAR 1ES 2344+514 on diverse time-scales in the optical bands. The BLAZAR has mild short-term variability (STV) and long-term variability (LTV), with small amplitudes of $\sim0.7$ mag and 0.4 mag for the host subtracted- and included-light curves, respectively. The power-enhanced F-test and the nested Analysis of Variance (ANOVA) statistical tests of the six intra-day light curves show that the BLAZAR has no minute-scale variability. The multiband color behavior analysis revealed a moderate redder-when-brighter (RWB) trend on intra-day time scales, while the LTV shows no detectable color behavior. We found a strong correlation between the ZTF optical light curves without any time lag, but no detectable correlations for the optical band emissions. From our periodicity searches using WWZ and LS methods, three significant quasi-periodic oscillation (QPO) signals in the ZTF light curves are found at about 1.02, 1.3, and 2.85 years. The observational results indicate that the BLAZAR 1ES 2344+514 has a complex variability while emphasizing the need for future observations to unravel its underlying mechanisms.
[abstract 32 / 62] (score: 3) - Title: Exploring the physics of ram pressure stripping with radio continuum observations in the SKA eraAuthors: Alessandro Ignesti, Ian D. Roberts, Henrik W. Edler, Myriam Gitti, Reinout J. van Weeren, Paolo Serra, Pavel Jachym,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no: AASKAII/Ignesti01 . Advancing Astrophysics with the SKA II (AASKAII) outlines the transformative scientific advances that will been abled by the SKA telescopesSubjects: astro-ph.GACreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Satellite galaxies in clusters are significantly more likely to be red and passive than similar mass galaxies in the field. This fact is known as the environmental quenching of galaxy STAR FORMATION, which is believed to be driven by ram pressure stripping (RPS). The large velocity differences between the infalling galaxies and the intracluster medium (ICM) result in a strong ram pressure on their interstellar medium (ISM), which can strip it from the stellar disk. The stripped ISM can be studied at various wavelengths, including the radio band, thanks to the SYNCHROTRON emission produced by the MAGNETic fields and RELATIVISTIC electrons embedded in them. This emission is typically steep-spectrum and thus best observed at low frequencies. Thus, continuum studies of the RPS effect are currently mostly carried out with LOFAR, limiting them to the northern hemisphere. SKA-Low will permit us to extend them to the southern sky, where they will synergize with the southern observatories and the upcoming ELT. Lastly, the sub-arcsecond resolution provided by SKA-Mid will facilitate the exploration of the POLARIZATION and filamentary structure of RPS radio tails and allow us to detect them up to $z\simeq0.5$, advancing our understanding of the impact of RPS on satellite galaxies in clusters and groups.
[abstract 33 / 62] (score: 3) - Title: Study for curvature radiation and MAGNETic pair creation process on polar-cap region of MAGNETic white dwarfAuthors: Bingyan Wang, Jumpei Takata,Comments: 18 pages, 8 figures, submitted to ApJSubjects: astro-ph.HECreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Rapidly rotating, strongly MAGNETized white dwarfs (WDs) have been proposed as potential sites of rotation-powered activity analogous to that of a neutron star pulsar. In this study, we investigate particle acceleration, radiation processes, pair creation and resulting SYNCHROTRON radiation in the polar cap acceleration region. Within the framework of the space-charge-limited flow model, we examine how these processes depend on the spin period and surface MAGNETic field using both one-dimensional numerical calculations and analytical estimates. To explore the impact of the MAGNETic field geometry on the accelerating process, we consider both a pure dipole field and a combination of dipole and quadrupole fields. The inclusion of a quadrupole component reduces the curvature radius of the MAGNETic field lines, and significantly enhances the accelerating field, leading to more efficient radiation and pair creation processes. Using this framework, we evaluate the WD death line with a more consistent treatment of the relevant physical processes than the previous studies. We find that the pair creation process can occur for spin periods $P\lesssim100$~s, when the dipole field strength $B_{*,d}\lesssim10^{10}$~G, indicating that pair creation is difficult to sustain in currently known MAGNETic WDs. We discuss the implications of our model for rotation-powered activity in rapidly spinning isolated MAGNETic WDs and for the possible WD interpretation of long-period radio transients.
[abstract 34 / 62] (score: 3) - Title: JWST resolves JET-driven H2 and ionized outflows in RADIO GALAXy 3C305Authors: B. Sebastian, P. M. Ogle, P. Guillard, L. Lanz, R. Morganti, V. Reynaldi, I. E. Lopez, B. Emonts, S. Garcia-Burillo, C. Tadhunter, C. P. O'Dea, S. Baum, F. R. Faifer, A. Labiano, M. Lehnert, A. Togi, K. Alatalo, P. Appleton, R. Bhutkar, E. Egami,Comments: .Accepted for publication in ApJSubjects: astro-ph.GA astro-ph.COCreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
We present JWST MIRI MRS, NIRSpec, NIRCam, and MIRI imaging observations of 3C 305, a RADIO GALAXy with a compact JET that is confined within the galaxy. We use the H2 0-0 S(1)-S(7) lines, several mid-IR fine-structure lines, and PAH emission in the MIRI MRS spectrum to conduct a multiphase study of the radio JET's impact on the interstellar medium. Multiple tracers, including H2/PAH 11.3 um and [Fe II] 5.34 um, provide evidence for shocks at the JET termination locations. Two Gaussian components are required to reproduce the warm H2 kinematics adequately, with one representing the bulk low-velocity component and the other corresponding to an outflow. The ionized gas reaches higher outflow velocities than the H2 gas, and the sharp increase in velocity at the JET hotspots points to JET-driven outflows. We fit the H2 excitation diagram with a power-law temperature distribution and find that the hotspots exhibit flatter slopes, indicating a larger warm/hot gas mass fraction at these locations. Our MAPPINGS line-ratio analysis indicates that most of the mid-IR ionized gas can be fit by a shock-plus-precursor model. We find that strong radiative losses dominated by line cooling, together with moderate kinetic power in the molecular and ionized gas outflows, can account for the estimated JET power, indicating high JET coupling efficiency in 3C 305. Together with other studies of multiphase gas, our results show that JETs can efficiently shock-heat and accelerate the gas they encounter, driving massive, kiloparsec-scale, multiphase outflows.
[abstract 35 / 62] (score: 3) - Title: A Population of Little Red Dot-like Quasars in SDSSAuthors: Quinn O. Casey, Ryan C. Hickox, Nikko J. Cleri, Jonathan H. Cohn, David M. Alexander, Emmanuel Durodola, Kelly E. Whalen, Raphael E. Hviding, Tonima Tasnim Ananna,Comments: 20 pages, 7 figures (+2 appendix figures), 3 tables. Submitted to ApJ. Comments welcomeSubjects: astro-ph.GACreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Compact and red sources in the high redshift ($z\sim5$) Universe, known as "Little Red Dots" (LRDs), are among JWST's most intriguing discoveries. These sources have broad Balmer emission lines, weak X-ray emission, and unique spectral energy distributions (SEDs) poorly fit by either stellar or AGN templates. Local analogs of LRDs allow for detailed studies of the underlying physical processes with archival multi-wavelength datasets unavailable in the high-$z$ Universe. We show that the SDSS $ugriz$ filters at $z\approx0.4, 0.8$ overlap well with the JWST filters used to select LRDs at $z\sim5$. We use SDSS QUASARs to define a sample of $\sim1300$ Local Red Dots (LoRDs) which share the same photometric colors of LRDs. A subset of the LoRD sample selected to have V-shaped continua ($N=244$) show prominent higher-order Balmer absorption features and [NeV]$λ$3426 emission, both of which would likely be missed in JWST/PRISM observations given the low spectral resolution. A composite SED of the LoRDs differs from a typical QUASAR SED in the rest-frame UV/optical, but the two agree with each other in the NIR. The LoRD SED matches well with a stack of LRDs and can be modeled either as a reddened AGN combined with a host galaxy, or as a reddened AGN combined with a host galaxy and a cool blackbody. Interestingly, the LoRDs are X-ray detected at a rate comparable to typical QUASARs. However, the probability that LoRDs and typical QUASARs would go undetected, if subject to the LRD X-ray upper limits, is $>50\%$.
[abstract 36 / 62] (score: 2) - Title: A nonsingular, anisotropic universe in a BLACK HOLE with torsion and particle productionAuthors: Nikodem J. Popławski,Comments: 9 pages; published versionSubjects: gr-qc astro-ph.COCreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
We consider a universe formed in a BLACK HOLE in general relativity with spin and torsion. The interior of a Schwarzschild BLACK HOLE can be represented by the Kantowski$-$Sachs metric that describes a closed anisotropic universe. We use this metric to derive the Einstein$-$Cartan field equations with a RELATIVISTIC spin fluid as a source. We show that torsion may prevent a singularity and replace it with a nonsingular bounce if particle production dominates over shear. Particle production after the last bounce can generate a finite period of inflation, during which the universe expands and isotropizes to the current state. This scenario is only approximate: the Kantowski$-$Sachs metric is never reached and should be replaced with a more general metric that tends to that of a 3-sphere.
[abstract 37 / 62] (score: 2) - Title: Quasinormal modes from numerical relativity with Bayesian inferenceAuthors: Richard Dyer, Christopher J. Moore,Comments: Main text: 14 pages, 10 figures. Appendix: 7 pages, 11 figuresSubjects: gr-qc astro-ph.HECreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Numerical relativity (NR) enables the study of physics in strong and dynamical gravitational fields and provides predictions for the gravitational-wave signals produced by merging BLACK HOLEs. Despite the impressive accuracy of modern codes, the resulting waveforms inevitably contain numerical uncertainties. Quantifying these uncertainties is important, especially for studies probing subdominant or nonlinear effects around the merger and ringdown. This paper describes a flexible Gaussian-process model for the numerical uncertainties in all the spherical-harmonic waveform modes across a state-of-the-art catalog of NR waveforms and a highly efficient procedure for sampling the posteriors of quasinormal mode models without the need for expensive Markov chain Monte Carlo. The Gaussian-process model is used to define a likelihood function which allows many Bayesian data analysis techniques - already widely used in the analysis of experimental gravitational wave data - to be applied to NR waveforms as well. The efficacy of this approach is demonstrated by applying it to the analysis of quasinormal modes in Cauchy-characteristic evolved waveforms.
[abstract 38 / 62] (score: 2) - Title: Quasinormal mode content of binary BLACK HOLE ringdownsAuthors: Richard Dyer, Christopher J. Moore,Comments: Main text: 5 pages, 2 figures. Supplemental material: 2 pagesSubjects: gr-qc astro-ph.HECreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
We present a fully Bayesian, data-driven framework for identifying quasinormal modes in high-accuracy Cauchy-Characteristic Evolution (CCE) gravitational waveforms. Applying this to a public catalog, we identify QNM overtones, retrograde modes, and nonlinear modes up to cubic order in the ringdown. Multiple high-order overtones are found near the merger, confirming their physical significance for modeling the ringdown. The ringdown mode content is tabulated across a wide range of start times for all available simulations, providing a systematic reference for theoretical and observational studies. We also search for late-time power-law tails, which are, as expected, absent from the CCE waveforms.
[abstract 39 / 62] (score: 2) - Title: Fast Radio Bursts in the Era of the Vera C. Rubin Observatory's Legacy Survey of Space and TimeAuthors: C. W. James, B. Smith, K. Dage, A. L. Chies Santos, K. W. Bannister, M. Caleb, J. F. Crenshaw, A. T. Deller, K. G. Lee, L. Marnoch, K. M. Rajwade, S. D. Ryder, R. M. Shannon, B. Stappers, T. Zhang,Comments: 11 pages, 8 figures, 2 tables, Accepted by PASASubjects: astro-ph.HE astro-ph.COCreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Identifying the host galaxies of fast radio bursts (FRBs), and comparing their redshifts and dispersion measures, has unlocked a new probe of the cosmological distribution of ionised gas. However the necessary optical observations to identify FRB hosts, and measure their redshifts, are becoming increasingly onerous as the detection rate of precisely localised FRBs increases. Here we analyse the ability of the Legacy Survey of Space and Time (LSST), being conducted by the Vera C. Rubin Observatory, to identify FRB host galaxies, and the utility of LSST photometric redshifts for FRB cosmology. By combining a model of FRB host galaxy r-band magnitudes, $m_r$, with predictions for the FRB z-DM distribution, we create a method to predict the $m_r(z)$ distribution for the host galaxies of FRBs detected by radio surveys. We then predict these distributions for the coherent modes of the Australian Square Kilometre Array Pathfinder (ASKAP) and MeerKAT. We find that even a single visit with Rubin will be able to identify 65% of FRB host galaxies detected by ASKAP's coherent upgrade, `CRACO'; while the final 10 year co-added images will identify 81% of those from MeerKAT's tied array beams. We also simulate the impact of using photometric redshifts for a simplified analysis to determine $H_0$, finding that estimated photo-z errors result in a decreased precision of only 7% on $H_0$ for ASKAP's CRACO system. The impact of missing faint FRB hosts, which are likely at higher redshifts, is more significant, and might degrade sensitivity to $H_0$ by 47%, or 62% when combined with photo-z errors. All told, Rubin's LSST will be an incredibly powerful survey for facilitating FRB cosmology, although supplemental observations may be useful for particularly faint and distant host galaxies.
[abstract 40 / 62] (score: 2) - Title: Formation of Suprathermal Electron Populations in the Expanding, Turbulent Solar WindAuthors: Maximilien Péters de Bonhome, Fabio Bacchini, Luca Pezzini, Viviane Pierrard,Comments: 9 pages, 4 figuresSubjects: astro-ph.SR physics.plasm-phCreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Nonthermal features are ubiquitously observed in electron velocity distribution functions in the solar wind, yet their origin in the collisionless, turbulent, expanding solar-wind plasma remains unclear. We investigate how solar-wind expansion and Alfvénic turbulence jointly generate and regulate these features using the first fully kinetic particle-in-cell simulation of an expanding turbulent plasma under heliospheric conditions. In our setup, expansion-driven weakening of the MAGNETic field adiabatically cools the plasma perpendicularly to the mean field while leaving the parallel temperature largely unchanged, driving the system toward the firehose-instability threshold. Concurrently, strongly anisotropic turbulence leads to perpendicular heating and the development of nonthermal features. Subsequently, we find that suprathermal electron populations preferentially develop in the parallel direction, forming pronounced power-law tails even under weakly compressive, highly Alfvénic conditions, and persist despite anisotropy regulation by the firehose instability. The preferentially parallel energization suggests the involvement of parallel electric fields or resonant wave--particle interactions, rather than simple velocity-space redistribution. These results provide the first direct evidence of the emergence of nonthermal-electron features in a unified kinetic framework linking expansion, turbulence, and instabilities in the solar wind.
[abstract 41 / 62] (score: 2) - Title: Geometry-induced self-excited dynamo in a regular tetrahedronAuthors: Akira Kageyama,Comments: 8 pages, 5 figures; title revised and one sentence added to clarify the scope; results unchangedSubjects: physics.flu-dynCreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
We propose a minimal, rotation-free model of MAGNETohydrodynamic (MHD) dynamo action driven by laminar thermal convection in a regular tetrahedral cavity. Unlike canonical planetary-dynamo settings, where flow helicity is supplied by global rotation, the present system generates robust flow helicity purely through the geometric constraints imposed by tetrahedral boundaries. Direct numerical simulations show exponential amplification of a weak seed MAGNETic field and a nonlinear saturated state in which the MAGNETic energy exceeds the kinetic energy. The convective flow organizes into a highly symmetric pattern with \(D_4\) dihedral symmetry. The dynamo-generated MAGNETic field obeys a corresponding signed \(D_4\) symmetry involving antisymmetry under \(π\)-rotations about the two horizontal axes of the tetrahedron. The tetrahedral dynamo provides a conceptually transparent setting for isolating geometry-induced helicity, MAGNETic-field amplification, and a closed induction cycle in a non-rotating laminar flow.
[abstract 42 / 62] (score: 2) - Title: Line-of-sight MAGNETic-field propagation effects on axion-like particle constraints from GRB 221009AAuthors: Chengcheng Han, Zhanhong Lei, Jiajie Yang, Shutong Zhao,Comments: 30 pages, 9 figuresSubjects: hep-ph astro-ph.HECreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
High-energy photons from GRB 221009A provide a powerful opportunity to probe axion-like particles (ALPs) through photon-ALP oscillations in cosmic MAGNETic fields. We revisit the ALP constraints implied by the LHAASO observation of this burst, with particular emphasis on the MAGNETic-field environments encountered along the line of sight. We include the host-galaxy, intergalactic, and Milky-Way MAGNETic fields and assess their respective impacts on the photon survival probability and on the exclusion limits in the ALP mass-coupling plane. We show that the constraints are only mildly affected by the choice of host-galaxy and Galactic MAGNETic-field models, but can change significantly once the intergalactic MAGNETic field is varied. Its field strength, coherence scale, and stochastic properties can all leave visible imprints on the derived exclusion contours, and in some cases generate pronounced oscillatory features. This demonstrates that the intergalactic MAGNETic field constitutes the dominant astrophysical uncertainty in extracting ALP limits from GRB 221009A. Our analysis highlights the importance of realistic propagation modeling in future gamma-ray searches for ALPs.
[abstract 43 / 62] (score: 2) - Title: Remarks on atmospheric effect of D-foam in light of muon puzzleAuthors: Chengyi Li,Comments: 5 latex pages, no figure, accepted versionSubjects: hep-ph astro-ph.HE gr-qcCreated: 2026-06-22; Updated: 2026-06-25; Datestamp: 2026-06-25
In our recent paper arXiv:2509.00552, we used a stringy model for quantum space-time foam to suggest that the so-induced subluminal Lorentz violation~(LV) for photons would not lead to experimentally unacceptable changes in the developments of particle showers initiated by cosmic $γ$-rays in the Earth's atmosphere, in contrast to other approaches to LV. The result indicated, nonetheless, at the same time that the foam can mildly modify the electroMAGNETic cascades under certain conditions, by suppressing pair creation on nuclei by primary photons. In this addendum, we consider how this modification affects the detection of extensive air shower~(EAS) initiated by an ultrahigh-energy cosmic-ray particle~(viz., a primary hadron), like proton with $E \sim 10^{19}~\textrm{eV}$, given that secondary photon subshowers following $π^{0}$ decays could be similarly influenced. We argue that fewer electrons would reach the detector and hence the energy of the primary particle may be underestimated due to foam effects, enhancing in such a way the muon content in EASs. This opens up the possibility of interpreting the alleged ``excess'' of muons, as reported by Auger and Telescope Array collaborations recently and many other experiments on high-energy COSMIC RAYs, with a quantum-gravitational effect. Future observations are anticipated to confirm whether this anomaly really exists.
[abstract 44 / 62] (score: 2) - Title: Reconstruction of chaotic systems in invariant JET spaceAuthors: Evgeny Nikulchev,Comments: 18 pages, 2 figuresSubjects: eess.SY cs.SY nlin.CDCreated: 2026-06-21; Updated: 2026-06-25; Datestamp: 2026-06-25
Takens' theorem is the gold standard for attractor reconstruction from time series, but it guarantees only topological equivalence and does not preserve metric or group properties such as symmetries. We show that switching from delay-coordinate space to JET space (signal and its derivatives) allows one to exactly preserve the symmetry group of the original system. This statement is rigorously justified by a theorem on the isomorphism of Lie algebras under JET prolongation. Numerical experiments on the Lorenz and Rössler systems confirm that JET-space reconstruction preserves geometry and symmetries, whereas Takens embedding distorts them. As quantitative metrics we use a variational elastic energy functional and the correlation dimension. It is shown that JET-space reconstruction not only outperforms Takens embedding but in some cases yields more accurate estimates of invariants than projections of the original system. The proposed approach provides a coordinate-invariant criterion for the classification of strange attractors and can serve as a basis for detecting hidden attractors.
[abstract 45 / 62] (score: 2) - Title: Low-frequency VLBI with the SKA-LowAuthors: R. Timmerman, E. L. Escott, T. Vernstrom, L. K. Morabito, C. Reynolds,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Timmerman01Subjects: astro-ph.IMCreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
The Square Kilometre Array Observatory (SKAO) will provide unprecedented observational capabilities, revolutionizing radio astronomy in the next decade. Of particular interest for many science areas is the low-frequency component: the SKA-Low. This array, operating at frequencies between 50 and 350 MHz, will be able to observe the Southern hemisphere with an angular resolution of several arcseconds. However, many science cases demand finer angular resolutions than the current design baseline for the SKA-Low. In this chapter, we present the Low-frequency Australian Megametre-Baseline Demonstrator Array (LAMBDA) project: the construction of a several SKA-Low-like stations throughout Australia which can be employed to extend the SKA-Low's baselines to the scale of megameters. This allows LAMBDA to not only probe the scientific opportunities accessible at higher angular resolutions, but also prove the feasibility of a potential extension of the SKA-Low to such baselines. Finally, LAMBDA also serves to characterize the performance of the SKA-Low as part of a Very Long Baseline Interferometry (VLBI) network and by providing an early testbed for the calibration strategies which would be required. With LAMBDA, the SKA-Low will be able to make a major impact in many science areas, including but not limited to exoplanets, resolved ACTIVE GALACTIC NUCLEi (AGN), young stellar objects and SUPERNOVA remnants, pulsar astrometry and scintillometry, gravitational lensing and fast radio bursts (FRBs).
[abstract 46 / 62] (score: 2) - Title: Investigating BLACK HOLE accretion and feedback self-regulation in Seyfert galaxies using the FIRE-3 cosmological hydrodynamic simulationsAuthors: Jonathan Mercedes-Feliz, Daniel Anglés-Alcázar, Jose Cevallos, Boon Kiat Oh, Santiago García-Burillo, Rachel K. Cochrane, Cristina Ramos Almeida, Claude-André Faucher-Giguère, Almudena Alonso-Herrero, Alexander J. Richings, Miguel Pereira-Santaella, Jorge Moreno, Niranjan Chandra Roy, Tanio Díaz-Santos, Philip F. Hopkins,Comments: 21 pages, 11 figures. To be submitted to MNRASSubjects: astro-ph.GACreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
Recent observations of local Seyfert galaxies show an intriguing connection between Active Galactic Nuclei (AGN) luminosity and a deficit of molecular gas on ~50pc scales compared to 200pc, the plausible imprint of AGN feedback. Motivated by these findings, we investigate the interplay between supermassive BLACK HOLE (BH) accretion, AGN feedback, and nuclear gas reservoirs using high-resolution cosmological hydrodynamic simulations implementing FIRE-3 multi-phase interstellar medium (ISM) physics and multi-component BH accretion and feedback models. Focusing on the late-time evolution of four Milky Way-mass galaxies, we find recurrent cycles of increased gas inflow toward the accretion disc, enhanced BH accretion, feedback self-regulation, and suppressed gas inflow rate until the next fueling event. AGN winds interact with the ISM and escape preferentially through low-density polar channels after opening central cavities on ~10-500pc scales, regulating BH growth and producing episodic behaviour on ~10-100Myr timescales. The simulations reproduce the observed diversity of nuclear morphologies, gas concentrations, and AGN luminosities in late-type Seyfert galaxies, but do not exhibit a clear anti-correlation between gas concentration and AGN luminosity. Higher-luminosity AGN ($L_X$~$10^{41.5-43}$ erg s$^{-1}$) powered by the accretion disc reservoir can coexist with feedback-driven cavities, consistent with observations, but they are more common in simulated galaxies with centrally-peaked gas distributions. Although differences in sample selection, tracer choice, spatial resolution, and stochasticity in AGN fueling may impact underlying concentration-luminosity trends, the apparent tension between simulations and observations points to the timing between gas inflow, accretion-disc depletion, and feedback-driven clearing on ~50-200pc scales as a key constraint on AGN self-regulation models.
[abstract 47 / 62] (score: 2) - Title: Formation of Black Hole-White Dwarf X-ray Binaries in Globular ClustersAuthors: William Y. W. Yang, Kyle Kremer, James C. Lombardi,, Kristen C. Dage,Comments: 19 pages, 9 figures, 1 table. Submitted to ApJ. Comments are welcomeSubjects: astro-ph.HECreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
Globular clusters are host to significant populations of dynamically-active stellar remnants that connect to a variety of astrophysical sources. Using simulations performed with the Cluster Monte Carlo dynamics code, we study the formation of ultracompact binaries in which a stellar-mass BLACK HOLE accretes material from a white dwarf companion in a sub-hour orbit. These binary systems are prime multimessenger targets, as they can be observed as both luminous X-ray sources, and as millihertz gravitational wave sources detectable by the Laser Interferometer Space Antenna (LISA). We find that BLACK HOLE+giant collisions are the primary mechanism through which such systems form. We model the outcomes of these ``common envelope''-like events using the smoothed particle hydrodynamics code StarSmasher, and verify these collisions yield BLACK HOLE+white dwarf binaries that enter Roche contact on sub-Gyr timescales via gravitational wave inspiral. We construct a mock catalog of local ultracompact X-ray sources and compare to candidate sources observed in globular clusters in the Milky Way (e.g., 47 Tuc X9) and external galaxies (e.g., RZ 2109 in NGC 4472). Finally, we compute the gravitational wave strain for these sources, and show that of order one source may be resolvable in the Milky Way by LISA, representing a potentially powerful tool for observing new BLACK HOLEs in globular clusters.
[abstract 48 / 62] (score: 2) - Title: Evolution of AGN Across Cosmic Epochs with the SKAOAuthors: R. Kondapally, V. Singh, G. Mazzolari, I. Delvecchio, A. Datta, A. Kayal, B. Mingo, J. Moldon, J. Petley, I. Prandoni, K. Rubinur, S. Shabala, F. Shankar,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Kondapally01Subjects: astro-ph.GACreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
Understanding the evolution of ACTIVE GALACTIC NUCLEi (AGN) and their host galaxies across cosmic epochs is one of the key science drivers of extragalactic astronomy. The detection of AGN residing in dusty environments and at high redshifts is difficult due to obscuration and faintness which poses a challenge in understanding AGN evolution across cosmic time. Deep radio continuum surveys (rms noise $<$ 1 $μ$Jy~beam$^{-1}$) from the Square Kilometre Array Observatory (SKAO) will be an efficient means to detect and study a broad population of AGN across cosmic history. In this chapter, we present radio luminosity functions, source counts, and detection rates of AGN based on the SKAO simulated radio source catalogues. We demonstrate that the SKA-Mid multi-tiered surveys, in particular, reaching sub-$μ$Jy depths, will allow us to characterise the bulk of the radio-AGN complete down to $L_{\rm{1.4\,GHz}} \sim 10^{23}\,\rm{W\,Hz^{-1}}$ and enable us to probe the evolution of radio-AGN across a wide range of luminosities and all galaxy environments up to $z \sim 6$. Overall, our work highlights the importance of deep multi-tiered SKAO radio continuum surveys for studying the evolution of radio-AGN activity across cosmic time.
[abstract 49 / 62] (score: 2) - Title: Liquid Jet in Crossflow: Review of Breakup modes and Injector Geometry EffectsAuthors: Anubhav Sinha,Comments:Subjects: physics.flu-dynCreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
This review focuses on the liquid JET in crossflow (LJIC) configuration. LJIC is one of the most common strategies used for fuel injection in aerospace applications. It is popular due to its simplicity and efficient atomization characteristics. The aerodynamic force of the airflow is utilized to break liquid JET into small droplets. The objective of the present work is to give a basic overview of the physical processes involved in the breakup and penetration of LJIC. Breakup modes and underlying mechanisms are discussed in detail. Various modes are described and associated non-dimensional numbers are explained. Injector geometry which is often overlooked in literature is paid special attention. The mechanism of liquid JET instability getting triggered by velocity profile redistribution is explained using experimental and computational results. Surface waves on liquid JETs are discussed. A theoretical model used to predict the wavelength of surface waves is described. DNS results are used to demonstrate the growth of surface instability on a liquid JET. Jet penetration and trajectory in the presence of crossflow are discussed. Various trajectory equations and the parameters used are discussed in detail. Progress in computational studies for LJIC is highlighted and challenges are discussed.
[abstract 50 / 62] (score: 2) - Title: Slow Extraction Beam Commissioning for the Mu2e Experiment at FERMIlabAuthors: V. Nagaslaev, G. Annala, J. Berlioz, G. Deinlein, B. Drendel, J. Morgan, A. Narayanan, J. StJohn, D. Still, D. VanderMeulen,Comments: 17th International Particle Accelerator Conference (IPAC 2026)Subjects: physics.acc-phCreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
Following the successful completion of the Muon g-2 experiment run at FERMIlab, the Muon Campus facility has been reconfigured from delivering 3 GeV muon beams to the g-2 storage ring to providing slow-extracted 8 GeV proton beam spills for the Mu2e experiment. The first full-scale commissioning run with slow extraction was conducted during the 2025 run, followed by the second run in early 2026. We present the results and current status of this commissioning campaign.
[abstract 51 / 62] (score: 2) - Title: Dust destruction signals shock-accelerated outflows in the nearby active galaxy NGC\;1068Authors: Luke R. Holden, Clive N. Tadhunter, Daniel J. B. Smith, Martin A. Bourne, Marina I. Arnaudova, Isaac M. Mutie,Comments: 15 pages, 12 figures, 2 tables; accepted for publication in MNRASSubjects: astro-ph.GA astro-ph.HECreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
Massive gas outflows driven by ACTIVE GALACTIC NUCLEi (AGN) are a key ingredient in models of galaxy evolution, in which they are required to regulate STAR FORMATION and thus explain the observed properties of the galaxy population. However, it remains uncertain how such outflows are accelerated. Here, we use deep spectroscopic observations of the nearby active galaxy NGC 1068 to directly address this issue. Based on the flux ratios of high-ionisation [NeV]$λ$3425 and [FeVII]$λ$6087 coronal forbidden lines, we show that the non-outflowing gas in the disk of the galaxy is characterised by high levels of depletion of refractory elements onto dust grains, but the outflowing gas just above the disk is largely dust-free. Consistent results are also found for the ratios of lower-ionisation forbidden lines of refractory and non-refractory elements. Moreover, a range of diagnostic ratios demonstrate that the density of outflowing gas is a factor 19-110 times higher than that of the non-outflowing gas. Together, these results imply that the outflows in NGC 1068 are accelerated by fast shocks that both compress the gas and destroy much of the dust. Consistent with the idea that AGN-driven shocks play an important role in heating and accelerating the near-nuclear gas in galaxies, this study demonstrates that coronal emission lines are a key diagnostic of the destructive impact of AGN activity.
[abstract 52 / 62] (score: 2) - Title: Fast Radio Bursts probe Galaxy Evolution: Evidence and implications of a redshift-dependent FRB host DMAuthors: Lluis Mas-Ribas,Comments: SubmittedSubjects: astro-ph.GA astro-ph.HECreated: 2026-06-23; Updated: 2026-06-25; Datestamp: 2026-06-25
The redshift evolution of ionized gas in the full galaxy-halo system is a central open question in galaxy formation, because no existing observable is simultaneously sensitive to all ionized phases. Here we explore fast radio bursts (FRBs) as a probe of the density evolution of this gas through the redshift dependence of the FRB host dispersion measure, ${\rm DM_{host}}(z) \propto (1+z)^{n_z}$. The host DM denotes the electron column density of all ionized gas in the host along the FRB sightline, providing a unified tracer that complements existing phase-specific diagnostics. We apply a forward-modeling framework that accounts for instrumental effects to 90 localized FRBs (69 with confirmed host redshifts) from the DSA and ASKAP/CRAFT ICS surveys. Our inference yields $n_z = 1.62^{+1.48}_{-1.57}$, ruling out the non-evolving scenario ($n_z = 0$) at $1\,σ$, with both datasets independently favoring $n_z > 0$. The main $n_z$ degeneracy is with the mean host DM and parameters such as $H_0$, highlighting the need to account for a host evolution in inference analyses and DM-based host redshift estimates; overestimating redshifts by up to $Δz \approx 0.3$ for DM$_{\rm EG} \sim 1000 - 2000\,{\rm pc\,cm^{-3}}$ otherwise. About 100 ($300-350$) localized hosts from MeerTRAP in coherent mode (DSA/CRAFT) will yield $n_z$ uncertainties of $\sim0.7$. Precise $n_z$ measurements compared with the evolution of individual phases and galaxy scaling relations will shed light on ionized gas evolution in galaxies and halos, informing the dominant phase, the driver of the overall evolution, and FRB progenitor channels.
[abstract 53 / 62] (score: 2) - Title: A Free Sphere Reverses the Rebound Direction of a Near-Wall Cavitation BubbleAuthors: Chun-Zhu Ren, Jun Wen, Hai-Bao Hu, A-Man Zhang, Xiao Huang,Comments: 16 pages, 5 figures; includes Supplemental MaterialSubjects: physics.flu-dynCreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
A near-wall cavitation bubble is generally expected to acquire a wallward Kelvin-impulse bias and to rebound or JET toward the wall. Here we show that this canonical direction can be reversed by a wall-supported free sphere. High-speed imaging reveals a transition from away-from-wall to wallward rebound as the initial bubble--sphere separation is increased. By reconstructing the Kelvin impulse on a closed bubble boundary that includes both the visible free interface and the bubble-side contact closure, we find that the reversal is not governed primarily by the instantaneous velocity of the sphere. Instead, sphere displacement creates a contact closure on which the bubble-source contribution supplies an away-from-wall impulse. This contact-source impulse competes with a wallward background formed by the wall-image source and the quadrupolar component of the sphere-induced field. The resulting balance yields a calibrated geometric criterion, $\mathcal{M}_K$, and, in the comparable-size bubble--sphere regime, reduces to a contact number $a_z z_b/R_K^2$. These results identify a contact-geometric mechanism by which a movable particle can redirect the first-cycle JET and rebound bias of a near-wall cavitation bubble.
[abstract 54 / 62] (score: 2) - Title: Gravitational Light Deflection with SKA-VLBI and Its Application to Precision Tests of General RelativityAuthors: Y. J. Li, J. J. Li, Z. H. Lin, D. J. Liu, Y. W. Dong, C. J. Hao, Y. Xu,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Li01Subjects: astro-ph.IM astro-ph.HE gr-qcCreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Experimental test of general relativity remains an ongoing endeavour. Radio astrometry provides a vital tool for precisely measuring the light deflection caused by the Sun, testing general relativity, and discriminating between gravitational theories. The best accuracy for the post-Newtonian RELATIVISTIC parameter, $γ$, achieved with very long baseline interferometry is $9 \times 10^{-5}$. With 300-sec integration, SKA-VLBI can achieve a sensitivity of $\sim$15 $μ$Jy at 15 GHz over a bandwidth of 0.256 GHz. This enables detection of $\sim$36 extragalactic radio sources per square degree with flux densities of $\sim$1.5 mJy, and potentially detecting in-beam radio sources. Single-epoch SKA-VLBI observations may achieve an astrometric precision of $\sim$2 $μ$as. Utilising the Sun as a gravitational lens, 10-epoch positional tracking of extragalactic sources could improve $γ$ accuracy to $\sim$10$^{-7}$. Even with Jupiter as a lens, SKA-VLBI can measure $γ$ to $\sim$10$^{-4}$. Critically, it may conduct the first measurement of quadrupolar deflection of light caused by Jupiter, determining the physical oblateness of Jupiter, $J_{\mathrm{2, J}}$, to within $\sim${}$10^{-3}$. These advances are expected to rigorously test and improve gravitational theories or high-order parameterized post-Newtonian formalisms, while laying the foundations for (sub)$μ$as astrometry.
[abstract 55 / 62] (score: 2) - Title: The MAGNETic field in the Milky Way Galaxy: from large to small scalesAuthors: Xiaohui Sun, Jennifer West, Marijke Haverkorn, Andrea Bracco, Anna Ordog, Sui Ann Mao, Yik Ki Ma, Wenhui Jing, Thiem Hoang,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Sun01. Advancing Astrophysics with the SKA II (AASKAII) outlines the transformative scientific advances that will be enabled by the SKA telescopesSubjects: astro-ph.GACreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
The Milky Way is the galaxy in which we can study its MAGNETic field to the finest details, providing an ideal laboratory to understand the fundamental questions: how MAGNETic field is generated and evolves, and how it influences other components in the Galaxy. An SKA-Mid POLARIZATION survey will produce an all-sky rotation measure (RM) grid with a density of about 100 per square degree, which is approximately two orders of magnitude larger than what is currently available, and produce total intensity, polarized intensity, and RM all-sky images of diffuse emission covering scales from about 10 arcseconds upward after combination with single-dish observations. The dense RM grid and images of diffuse emission will allow us to determine the most complete picture of the MAGNETic field in the southern Galactic hemisphere from large to small scales.
[abstract 56 / 62] (score: 2) - Title: A 3D tomography of the Local Bubble with SKA-LowAuthors: Xiaohui Sun, George Heald, Andrea Bracco,Comments: Published in Advancing Astrophysics with the SKA II (AASKAII), 2026 (arXiv:2606.20366). Report-no:AASKAII/Sun02. Advancing Astrophysics with the SKA II (AASKAII) outlines the transformative scientific advances that will be enabled by the SKA telescopesSubjects: astro-ph.GACreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
We know we reside in the Local Bubble (LB), but we know little about the MAGNETized gas inside the LB. The SKA-Low with more than half of the total number of stations distributed within 1 km distance provides enough short baselines and thus great surface brightness sensitivity. An SKA-Low POLARIZATION survey covering the frequency range of 50-350 MHz will deliver high-sensitivity and high-resolution images of diffuse polarized emission that originates from the local interstellar medium (ISM) and is probably related with the LB. Such a survey will also determine precisely the rotation measures (RMs) for the polarized structures using RM synthesis. These will allow us to reveal the 3D structure of the MAGNETized medium in the LB and to understand how the LB forms and evolves.
[abstract 57 / 62] (score: 2) - Title: The Impact of Dense RM Grids on the Study of Intra-cluster and Intra-group Magnetic FieldsAuthors: Francesca Loi, Valentina Vacca, Shane P. O'Sullivan, Craig Anderson, Chiara Stuardi, Federica Govoni, Matteo Murgia, Annalisa Bonafede, Ettore Carretti, Filippo M. Maccagni, Tessa Versnstrom,Comments: Published in Advancing Astrophysics with the SJA II (AASKAII), 2026 (arXiv:2026.20366). Report-no: AASKAII/Loi01Subjects: astro-ph.COCreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
The presence of diffuse radio sources in galaxy clusters and the recent discovery of polarized signals associated with the tails of a jellyfish galaxy indicates that intra-cluster/intra-group MAGNETic fields can influence the physics of these environments and the evolution of the embedded galaxies. A better reconstruction of the properties of such fields is therefore fundamental to understand in detail the physical processes in galaxy groups and clusters and the evolution of the embedded sources. The SKAO represents a great opportunity to perform these studies through the analysis of the so-called rotation measure (RM) grid, since POLARIZATION properties of radio sources are modified by the intervening MAGNETic field. In this manuscript, we illustrate the prediction on the density of the RM grid considering the SKA-mid POLARIZATION survey planned by the SKA Magnetism Science Working Group. Moreover, we describe how it is possible to measure intra-cluster/intra-group MAGNETic fields with the RM grid. Eventually, we quantify the improvement in the precision and accuracy of the MAGNETic field measurements compared to what is achievable with current surveys such as the POSSUM survey.
[abstract 58 / 62] (score: 2) - Title: Constraining supermassive primordial BLACK HOLE clustering with the angular auto-correlation of $z\simeq 6$ QUASARsAuthors: Zhan-He Wang, Hai-Long Huang, Yun-Song Piao,Comments: 23 pages, 5 figures, 1 tableSubjects: astro-ph.CO gr-qc hep-phCreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
High-redshift QUASARs provide a direct probe of the origin and environment of the earliest supermassive BLACK HOLEs. We use their angular auto-correlation function at $z\simeq 6$ to test scenarios in which supermassive primordial BLACK HOLEs (SMPBHs) are associated with the observed QUASAR population. The evolved PBH correlation functions, for both Poisson fluctuations and initial PBH clustering, are projected over the QUASAR redshift window and compared with the measured angular correlation function using Markov chain Monte Carlo inference. It is observed that for the Poisson model, the posterior favors a small abundance, $f_{\rm PBH}\sim 10^{-3}$, and a supermassive effective mass scale, $m_{\rm PBH}\sim 10^{12}M_\odot$, interpreted here as a scale controlling QUASAR host-halo formation and clustering, and for the initially clustered model, the data prefer an effective clustering amplitude $ξ_{\rm eff}\simeq 2.1$ and a top-hat boundary scale $r_{\rm cl}\simeq 76\,{\rm Mpc}$, corresponding to weak relative contraction of PBH pairs in comoving coordinates.
[abstract 59 / 62] (score: 2) - Title: New Online Database of Symbiotic Variables: Catalog and Statistical Overview of Symbiotic BinariesAuthors: Jaroslav Merc, Rudolf Gális, Marek Wolf,Comments: 15 pages, 5 figures; accepted in ApJSSubjects: astro-ph.SR astro-ph.GACreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
We present the New Online Database of Symbiotic Variables (NODSV), a comprehensive and publicly accessible catalog of known and candidate symbiotic stars in the Milky Way and nearby galaxies. The database provides an up-to-date census of confirmed symbiotic binaries and systematically compiles information previously scattered across the literature, including photometric and spectroscopic properties, orbital parameters, and characteristics of both their cool and hot stellar components. It further records auxiliary diagnostics such as detected emission lines, flickering, X-ray emission, JETs, or information about outburst activity. In its current release, NODSV contains nearly 1 400 objects, classified into confirmed symbiotic stars, three categories of candidates, and misidentified sources. Based on the collected data, though originating from heterogeneous studies, we present a statistical overview of the confirmed symbiotic population, highlighting the distributions of orbital parameters and the properties of the cool giants and their hot companions. Designed as a dynamic and evolving resource, NODSV provides a foundation for future observational campaigns and theoretical investigations of symbiotic binaries.
[abstract 60 / 62] (score: 2) - Title: Multi-thermal dynamics and transverse oscillations of solar spicules revealed by coordinated SST, IRIS, and SDO observationsAuthors: Ravi Chaurasiya, Tiago M. D. Pereira, A. Raja Bayanna,Comments: Accepted for Publication in A&ASubjects: astro-ph.SRCreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
% context heading (optional) {Solar spicules are highly dynamic chromospheric JETs that play an important role in the mass and energy balance of the solar atmosphere, though their connection to the transition region and corona remains unclear.} % aims heading (mandatory) {We investigate the dynamical and multi-thermal properties of spicules, their connection to higher atmospheric layers, and their transverse oscillations and associated energy flux.} % methods heading (mandatory) {We analyse coordinated high-resolution observations from the Swedish 1-m Solar Telescope (SST) in H$α$, the Interface Region Imaging Spectrograph (IRIS) in \ion{Si}{iv} 1400~Å, and the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) coronal channels. Space-time diagrams, spectral analysis, and wavelet techniques are used to study temporal evolution, Doppler velocities, and oscillatory properties. Transverse displacements of spicules are tracked to estimate wave properties and energy flux.} % results heading {Space-time analysis reveals a clear correspondence between chromospheric spicules and coronal emission in AIA 171~Å, evolving coherently with spicule extension. Doppler velocities from H$α$ and \ion{Si}{iv} show opposite signs, indicating multi-thermal plasma flows. Wavelet analysis reveals frequently dominant $\sim$3-minute oscillations, along with high-frequency transverse oscillations (65--270~s) with velocity amplitudes of 3.3--9.9~km~s$^{-1}$ and a mean energy flux of $(2.14 \pm 0.78)\times10^{3}$~W~m$^{-2}$.} % conclusions heading (optional) {These results demonstrate that spicules are multithermal, dynamic structures connected to the transition region and corona, and that transverse waves carry substantial energy, highlighting their role in coronal heating.}
[abstract 61 / 62] (score: 2) - Title: Stages of turbulence generation and decay in a T-shaped mixerAuthors: Mohammad Mehdi Zamani Asl, Marc Avila,Comments:Subjects: physics.flu-dynCreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
The T-shaped mixer is widely used in fundamental studies of chemical engineering. Its transitional regime is well understood, whereas the turbulent dynamics has received scarce attention so far. Here we perform direct numerical simulations of the turbulent regime for Reynolds numbers up to $Re=2000$ at Schmidt number $Sc=1$. Our analysis reveals two distinct stages along the mixing channel prior to relaxation toward duct flow. Near the junction, a JET-like flow forms and exhibits the approximately self-similar behaviour of transitional planar JETs. Subsequently, a decay region characterised by power-law decay of turbulent kinetic energy, dissipation and scalar variance emerges. For the velocity field, the observed exponents are consistent with those of decaying turbulence in bounded domains, whereas the scalar-variance exponent is consistent with that of unbounded turbulence. We argue that this apparent discrepancy is a consequence of the mixing process progressing from the center of the channel toward the side walls in the decay region, while turbulence already fills the channel cross-section entirely at the end of the JET region.The time-averaged mixing state presents error-function profiles of the scalar in the transverse direction, similar to the laminar cases, and is quantified here through a stream-wise evolving effective diffusion coefficient.
[abstract 62 / 62] (score: 2) - Title: UsingSKA-Low to Detect PeV Gamma-rays from Galactic SourcesAuthors: Anna Nelles, Philipp Laub, Haoning He, Felix Schlüter, Sjoerd Bouma, Justin Bray, Stijn Buitink, Arthur Corstanje, Vital De Henau, Edwin Dickinson, Brian Hare, Jörg Hörandel, Tim Huege, Clancy James, Xingyu Li, Hermann-Josef Mathes, Katharine Mulrey, Subhadip Saha, Olaf Scholten, Ralph Spencer, Christopher Sterpka, Karen Terveer, Satyendra Thoudam, Gia Trinh, Paulina Turekova, Darko Veberic, Keito Watanabe, Hiroaki Yamamoto, Chao Zhang, Pengfei Zhang, Yi Zhang,Comments: Published in Advancing Astrophysics with the SKAII(AASKAII), 2026(arXiv:2606.20366). Report-no:AASKAII/Nelles01Subjects: astro-ph.HECreated: 2026-06-24; Updated: 2026-06-25; Datestamp: 2026-06-25
Detecting so called PeVatrons is considered one of the prime goals of $γ$-ray astronomy. PeVatrons are astrophysical objects in the Galaxy that are sources of COSMIC RAYs exceeding PeV ($10^{15}$ eV) energies, the highest in our Galaxy. Their nature is unknown as of now, with some candidates reaching barely above PeV energies just having been identified. Serendipitously, the energy threshold of air shower detection using radio emission, has been proven at 50 PeV. There is a case to be made that SKA-Low with its unprecedented number of antennas, can reach lower in energy, while the size of the core is sufficiently large provide a significant effective area to measure PeV fluxes. While this promises a novel angle towards understanding the COSMIC RAY accelerators in our Galaxy, it also would be the first detection of $γ$-ray air showers using radio emission.
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