Turbulence in Keplerian accretion disks

Details Turbulence in Keplerian accretion disks Turbulence in Keplerian accretion disks

Nov 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000phdt........78g&link_type=abstract

Thesis (PhD). THE UNIVERSITY OF TEXAS AT AUSTIN, Source DAI-B 61/08, p. 4207, Feb 2001, 116 pages.

Astronomy and Astrophysics

Astronomy

Scientific paper

Accretion disks are astronomical objects exhibiting ample varieties of turbulences such as convection driven by negative entropy gradients, MHD turbulence driven by magnetic shear, and global waves excited by tidal forces. The outcomes of this turbulence is manifested by turbulent transport (including energy, angular momentum, and magnetic field transports) and by turbulent dynamos. In Chapter 1, I describe how the ideas in this field have been developing for the past few years. Thermal convection and MHD turbulence induced by hydrodynamic and hydromagnetic instabilities in Keplerian accretion disks are reviewed in Chapter 2. Based upon the modification of mixing-length theory of convection in the turbulent Keplerian disks presented in Chapter 3, I show in Chapter 4 how the thermal equilibrium curves change by including the vertical energy transport via MHD turbulence. In Chapter 5, I estimate the helicities of an ambipolar dynamo driven by internal waves in the framework of mean- field dynamo theory. A summary and a perspective of my graduate work are given in the last Chapter.

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