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Electromagnetic emission from a binary black hole merger remnant in plasma: Field alignment and plasma temperature

Kelly, Bernard J. and Etienne, Zachariah B. and Golomb, Jacob and Schnittman, Jeremy D. and Baker, John G. and Noble, Scott C. and Ryan, Geoffrey (2021) Electromagnetic emission from a binary black hole merger remnant in plasma: Field alignment and plasma temperature. Physical Review D, 103 (6). Art. No. 063039. ISSN 2470-0010. doi:10.1103/physrevd.103.063039.

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Comparable-mass black-hole mergers generically result in moderate to highly spinning holes, whose spacetime curvature will significantly affect nearby matter in observable ways. We investigate how the moderate spin of a postmerger Kerr black hole immersed in a plasma with initially uniform density and uniform magnetic field affects potentially observable accretion rates and energy fluxes. Varying the initial specific internal energy of the plasma over two decades, we find very little change in steady-state mass accretion rate or Poynting luminosity, except at the lowest internal energies, where fluxes do not exhibit steady-state behavior during the simulation timescale. Fixing the internal energy and varying the initial fixed magnetic-field amplitude and orientation, we find that the steady-state Poynting luminosity depends strongly on the initial field angle with respect to the black hole spin axis, while the matter accretion rate is more stable until the field angle exceeds ∼45°. The protojet formed along the black hole spin axis conforms to a thin, elongated cylinder near the hole, while aligning with the asymptotic magnetic field at large distances.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Kelly, Bernard J.0000-0002-3326-4454
Etienne, Zachariah B.0000-0002-6838-9185
Schnittman, Jeremy D.0000-0002-2942-8399
Noble, Scott C.0000-0003-3547-8306
Ryan, Geoffrey0000-0001-9068-7157
Additional Information:© 2021 American Physical Society. Received 26 October 2020; accepted 12 February 2021; published 26 March 2021. Support for this research was provided by NASA’s Astrophysics Science Division Research Program. S. C. N. was supported in part by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center administrated by USRA through a contract with NASA. Z. B. E. gratefully acknowledges the NSF for financial support from Grants No. OIA-1458952, No. PHY-1806596, and No. OAC-2004311; and NASA for financial support from Grants No. ISFM-80NSSC18K0538 and No. TCAN-80NSSC18K1488. G. R. acknowledges the support from the University of Maryland through the Joint Space Science Institute Prize Postdoctoral Fellowship. The new numerical simulations presented in this paper were performed in part on the Pleiades cluster at the Ames Research Center, with support provided by the NASA High-End Computing (HEC) Program. Computational resources were also provided by West Virginia University’s Spruce Knob high-performance computing cluster, funded in part by NSF EPSCoR Research Infrastructure Improvement Cooperative Agreement No. 1003907, the state of West Virginia (WVEPSCoR via the Higher Education Policy Commission), and West Virginia University.
Funding AgencyGrant Number
NASA Postdoctoral ProgramUNSPECIFIED
University of MarylandUNSPECIFIED
State of West VirginiaUNSPECIFIED
West Virginia UniversityUNSPECIFIED
Issue or Number:6
Record Number:CaltechAUTHORS:20210421-154343020
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:108791
Deposited By: Tony Diaz
Deposited On:22 Apr 2021 21:38
Last Modified:22 Apr 2021 21:38

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