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General Relativistic Radiative Transfer and General Relativistic MHD Simulations of Accretion and Outflows of Black HolesWe have calculated the emission from relativistic flows in black hole systems using a fully general relativistic radiative transfer, with flow structures obtained by general relativistic magnetohydrodynamic simulations. We consider thermal free-free emission and thermal synchrotron emission. Bright filament-like features are found protruding (visually) from the accretion disk surface, which are enhancements of synchrotron emission when the magnetic field is roughly aligned with the line-of-sight in the co-moving frame. The features move back and forth as the accretion flow evolves, but their visibility and morphology are robust. We propose that variations and location drifts of the features are responsible for certain X-ray quasi-periodic oscillations (QPOs) observed in black-hole X-ray binaries.
Document ID
20070013707
Acquisition Source
Marshall Space Flight Center
Document Type
Preprint (Draft being sent to journal)
Authors
Fuerst, Steven V.
(Kavli Inst. for Particle Astrophysics and Cosmology Stanford, CA, United States)
Mizuno, Yosuke
(NASA Marshall Space Flight Center Huntsville, AL, United States)
Nishikawa, Ken-Ichi
(National Space Science and Technology Center Huntsville, AL, United States)
Wu, Kinwah
(University Coll. London, United Kingdom)
Date Acquired
August 23, 2013
Publication Date
January 1, 2007
Subject Category
Astrophysics
Distribution Limits
Public
Copyright
Other

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