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Disk Emission from Magnetohydrodynamic Simulations of Spinning Black HolesWe present the results of a new series of global, three-dimensional, relativistic magnetohydrodynamic (MHD) simulations of thin accretion disks around spinning black holes. The disks have aspect ratios of H/R approx. 0.05 and spin parameters of a/M = 0, 0.5, 0.9, and 0.99. Using the ray-tracing code Pandurata, we generate broadband thermal spectra and polarization signatures from the MHD simulations. We find that the simulated spectra can be well fit with a simple, universal emissivity profile that better reproduces the behavior of the emission from the inner disk, compared to traditional analyses carried out using a Novikov-Thorne thin disk model. Finally, we show how spectropolarization observations can be used to convincingly break the spin-inclination degeneracy well known to the continuum-fitting method of measuring black hole spin.
Document ID
20170003256
Document Type
Reprint (Version printed in journal)
Authors
Schnittman, Jeremy D. (NASA Goddard Space Flight Center Greenbelt, MD United States)
Krolik, Julian H. (Johns Hopkins Univ. Baltimore, MD, United States)
Noble, Scott C. (Tulsa Univ. OK, United States)
Date Acquired
April 7, 2017
Publication Date
February 26, 2016
Publication Information
Publication: The Astrophysical Journal
Volume: 819
Issue: 1
ISSN: 0004-637X
Subject Category
Astrophysics
Report/Patent Number
GSFC-E-DAA-TN41349
Funding Number(s)
CONTRACT_GRANT: NNX14AB43G
CONTRACT_GRANT: AST-0908336
CONTRACT_GRANT: ATP12-0139
Distribution Limits
Public
Copyright
Other
Keywords
accretion
accretion disks – black hole physics – X-rays: binaries