Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...378..266m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 378, Sept. 1, 1991, p. 266-270.
Astronomy and Astrophysics
Astrophysics
2
Accretion Disks, Convective Flow, Energy Transfer, Magnetohydrodynamic Turbulence, X Ray Binaries, Flow Stability, Gas Pressure, Milky Way Galaxy, X Ray Sources
Scientific paper
Allowance for turbulent pressure pulsations, convection, and dependence of the turbulence along z in accretion disks results in turbulent scale length much less than the disk (semi) scale height, more effectiveness for the convectile energy transport against instability, and gas pressure dominance in the flow, even for sonic regimes. Solution for the convective disk exists only for beta (0) not less than 0.14 and forces instability to depend on the turbulence level of the disk. For the viscosity law adopted (and for the standard one), the disk will be stable up to alpha (turbulent Mach number) about 1 (sonic regime). When applied to Galactic and extragalactic X-ray sources, these results suggest that absence (presence) of fluctuations may indicate subsonic (supersonic) turbulent regime as well as confirm (refute) the assumed viscosity law, rather than be a clue for externally (internally) produced photons cooled by the thermal plasma.
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