Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980azh....57..311r&link_type=abstract
(Astronomicheskii Zhurnal, vol. 57, Mar.-Apr. 1980, p. 311-320.) Soviet Astronomy, vol. 24, Mar.-Apr. 1980, p. 182-187. Transla
Astronomy and Astrophysics
Astrophysics
4
Astrophysics, Dynamo Theory, Milky Way Galaxy, Rotating Disks, X Ray Sources, Binary Stars, Black Holes (Astronomy), Numerical Integration, Stellar Mass Accretion
Scientific paper
The large-scale magnetic field in a rotating, turbulent gaseous disk will be generated by a dynamo process (the alpha-omega-dynamo) determined by the differential rotation omega (r) and the spirality function alpha (z). The generation is best described by a difference approximation to the dynamo equations, using a step greater than the turbulence correlation length and a smooth function alpha (z). The critical dynamo-number for exciting the lowest even quadrupole mode is Dq = -8. The odd dipole mode will be excited only for large dynamo-numbers, /Dd/ equal to or greater than 500. When /D/ equal to or greater than 20, all modes other than the lowest quadrupole mode (for which the threshold D = -500) are oscillatory. The results are applied to the Galaxy (D = -10; characteristic growth time, 3 x 10 to the 8th yr) and to accretion disks in binary systems containing a black hole, where several oscillatory modes can be excited.
Ruzmaikin Aleksandr
Sokoloff Dimitry
Turchaninoff V. I.
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