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ORIGINAL RESEARCH article
Front. Astron. Space Sci.
Sec. Cosmology
Volume 11 - 2024 |
doi: 10.3389/fspas.2024.1386305
This article is part of the Research Topic The Dynamic Universe: Realizing the Potential of Time Domain and Multimessenger Astrophysics View all 12 articles
Frontiers in Astronomy Cosmic ray contributions from rapidly rotating stellar mass black holes: Cosmic Ray GeV to EeV proton and anti-proton sources 1
Provisionally accepted- 1 Washington State University, Pullman, United States
- 2 Max Planck Institute for Radioastronomy, Bonn, North Rhine-Westphalia, Germany
- 3 National Institute of Astrophysics (INAF), Rome, Italy
- 4 Faculty of Physics and Astronomy, Ruhr University Bochum, Bochum, North Rhine-Westphalia, Germany
- 5 University of Münster, Münster, North Rhine-Westphalia, Germany
- 6 Department of Theoretical Physics, University of Szeged, Szeged, Hungary
- 7 University of Alabama, Tuscaloosa, Alabama, United States
- 8 Other, India, India
- 9 Department of Physics, University of Toronto, Toronto, Canada
- 10 North Carolina Agricultural and Technical State University, Greensboro, North Carolina, United States
- 11 University of Maryland, Baltimore, Maryland, United States
- 12 The Bartol Research Institute, University of Delaware, Newark, California, United States
In Radio Super Novae (RSNe) a magnetic field of (B × r) = 10 16.0±0.12 Gauss × cm is observed; these are the same numbers for Blue Super Giant (BSG) star explosions as for Red Super Giant (RSG) star explosions, despite their very different wind properties. The EHT data for M87 as well for low power radio galaxies all show consistency with just this value of the quantity (B × r), key for angular momentum and energy transport, and can be derived from the radio jet data. We interpret this as a property of the near surroundings of a black hole (BH) at near maximal rotation, independent of BH mass. In the commonly used green onion model, in which a 2 π flow changes over to a jet flow we interpret this as a wind emanating from the BH/accretion disk system and its surroundings. Near the BH collisions in the wind can produce a large fraction of anti-protons. In this scenario the cosmic Ray (CR) population from the wind/jet is proposed to be visible as EeV protons and anti-protons in the CR data to EeV energy, with a E -7/3 spectrum. This can be connected to a concept of inner and outer Penrose zones in the ergo-region. The observed
Keywords: cosmic rays, Acceleration, supernovae, black holes, Magnetic Fields, Antiproton
Received: 15 Feb 2024; Accepted: 30 Aug 2024.
Copyright: © 2024 Allen, Biermann, Chieffi, Chini, Frekers, Gergely, Harms, Jaroschewski, Joshi, Kronberg, Kun, Meli, Seo and Stanev. This is an open-access article distributed under the terms of the Creative Commons Attribution License (CC BY). The use, distribution or reproduction in other forums is permitted, provided the original author(s) or licensor are credited and that the original publication in this journal is cited, in accordance with accepted academic practice. No use, distribution or reproduction is permitted which does not comply with these terms.
* Correspondence:
Peter Biermann, Max Planck Institute for Radioastronomy, Bonn, North Rhine-Westphalia, Germany
Athina Meli, North Carolina Agricultural and Technical State University, Greensboro, 27411, North Carolina, United States
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