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The nature of accretion disks of close binary stars: overreflection instability and developed turbulence

 a, b, c,  b
a Department of Physics, University of California, Santa Barbara, CA, USA
b Institute of Astronomy, Russian Academy of Sciences, ul. Pyatnitskaya 48, Moscow, 119017, Russian Federation
c Russian Research Centre Kurchatov Institute, Institute ofPhysics ofStochastic Structures, pl. Kurchatova 1, Moscow, 123182, Russian Federation

The current status of the physics of accretion disks in close binary stars is reviewed, with an emphasis on the hydrodynamic overreflection instability, which is a factor leading to the accretion disk turbulence. The estimated turbulent viscosity coefficients are in good agreement with observations and explain the high angular momentum transfer rate and the measured accretion rate. Based on the observations, a power-law spectrum for the developed turbulence is obtained.

Fulltext pdf (1.4 MB)
Fulltext is also available at DOI: 10.1070/PU2008v051n06ABEH006583
PACS: 47.27.−i, 97.10.Gz, 97.80.−d (all)
DOI: 10.1070/PU2008v051n06ABEH006583
URL: https://ufn.ru/en/articles/2008/6/b/
000260064600002
2-s2.0-53849095143
2008PhyU...51..551F
Citation: Fridman A M, Bisikalo D V "The nature of accretion disks of close binary stars: overreflection instability and developed turbulence" Phys. Usp. 51 551–576 (2008)
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:   ,    « :   » 178 577–604 (2008); DOI: 10.3367/UFNr.0178.200806b.0577

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