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Hybrid magnetic structures around spinning black holes connected to a surrounding accretion disk

Published online by Cambridge University Press:  20 January 2023

I. El Mellah Open the ORCID record for I. El Mellah [Opens in a new window] ,
B. Cerutti ,
B. Crinquand  and
K. Parfrey
I. El Mellah
Affiliation:
Univ. Grenoble Alpes, CNRS, IPAG School of Mathematics, Trinity College Dublin
B. Cerutti
Affiliation:
Univ. Grenoble Alpes, CNRS, IPAG School of Mathematics, Trinity College Dublin
B. Crinquand
Affiliation:
Univ. Grenoble Alpes, CNRS, IPAG School of Mathematics, Trinity College Dublin
K. Parfrey
Affiliation:
Univ. Grenoble Alpes, CNRS, IPAG School of Mathematics, Trinity College Dublin
Rights & Permissions [Opens in a new window]

Abstract

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The hot accretion flow around Kerr black holes is strongly magnetized. Magnetic field loops sustained by a surrounding accretion disk can close within the event horizon. We performed particle-in-cell simulations in Kerr metric to capture the dynamics of the electromagnetic field and of the ambient collisionless plasma in this coupled configuration. We find that a hybrid magnetic topology develops with a closed magnetosphere co-existing with open field lines threading the horizon reminiscent of the Blandford-Znajek solution. Further in the disk, highly inclined open magnetic field lines can launch a magnetically-driven wind. While the plasma is essentially force-free, a current sheet forms above the disk where magnetic reconnection produces macroscopic plasmoids and accelerates particles up to relativistic Lorentz factors. A highly dynamic Y-point forms on the furthest closed magnetic field line, with episodic reconnection events responsible for transient synchrotron emission and coronal heating.

Keywords

acceleration of particlesmagnetic reconnectionblack hole physicsradiation mechanisms: non-thermalmethods: numerical
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S362: The Predictive Power of Computational Astrophysics as a Discovery Tool , June 2020 , pp. 184 - 189
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

References

Blandford, R. et al. 1977, MNRAS, 179Google Scholar
Blandford, R. et al. 1982, MNRAS, 199Google Scholar
Cangemi, F. et al. 2021, A&A, 650Google Scholar
Cerutti, B. et al. 2013, ApJ, 770CrossRefGoogle Scholar
Cerutti, B. et al. 2015, MNRAS, 448Google Scholar
Crinquand, B. et al. 2021, A&A, 650Google Scholar
Dexter, J. and Agol, E. 2009, ApJ, 696Google Scholar
El Mellah, I. et al. 2021, A&A (in press), arXiv:2112.03933Google Scholar
Gierlinski, M. et al. 2003, MNRAS, 343Google Scholar
The Event Horizon Telescope collaboration 2021, ApJ Letters, 910, 1, L12 Google Scholar
The Event Horizon Telescope collaboration 2021, ApJ Letters, 910, 1, L13 Google Scholar
The Gravity collaboration 2018, A&A, 618Google Scholar
Miller-Jones, J. et al. 2021, Science, 371Google Scholar
Parfrey, K. et al. 2019, PRL, 122Google Scholar
Tchekhovskoy, A. et al. 2011, MNRAS, 418Google Scholar
Uzdensky, D. 2005, ApJ, 620Google Scholar
Yee, K. 1966, IEEE Transactions on Antennas and Propagation, 14Google Scholar
Yuan, Y. et al. 2019, MNRAS, 484Google Scholar