Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 687, Issue 1, Pages L25-L28Publisher
IOP PUBLISHING LTD
DOI: 10.1086/593148
Keywords
accretion, accretion disks; binaries: close; black hole physics; X-rays: stars
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Funding
- NASA [NNH07ZDA001N]
- NSF [AST 08-05832]
- NASA's Chandra Postdoctoral Fellowship [PF7-80048]
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [0805832] Funding Source: National Science Foundation
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We describe three-dimensional general relativistic magnetohydrodynamic simulations of a geometrically thin accretion disk around a nonspinning black hole. The disk has a thickness h/r similar to 0.05-0.1 over the radial range (2-20)GM/c(2).In steady state, the specific angular momentum profile of the inflowing magnetized gas deviates by less than 2% from that of the standard thin disk model of Novikov and Thorne. Also, the magnetic torque at the radius of the innermost stable circular orbit (ISCO) is only similar to 2% of the inward flux of angular momentum at this radius. Both results indicate that magnetic coupling across the ISCO is relatively unimportant for geometrically thin disks.
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