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

A.M. Fridman^a, b, c, D.V. Bisikalo^b
^aDepartment of Physics, University of California, Santa Barbara, CA, USA
^bInstitute of Astronomy, Russian Academy of Sciences, ul. Pyatnitskaya 48, Moscow, 119017, Russian Federation
^cRussian Research Centre ‘Kurchatov Institute’, Institute of Physics of Stochastic 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.

PACS: 47.27.−i, 97.10.Gz, 97.80.−d (all)
DOI: 10.1070/PU2008v051n06ABEH006583
URL: https://ufn.ru/en/articles/2008/6/b/
Web of Science

000260064600002
Scopus

2-s2.0-53849095143
ADS NASA

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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Оригинал: Фридман А М, Бисикало Д В «Природа аккреционных дисков тесных двойных звезд: неустойчивость сверхотражения и развитая турбулентность» УФН 178 577–604 (2008); DOI: 10.3367/UFNr.0178.200806b.0577

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