Astronomy and Astrophysics – Astronomy
Scientific paper
May 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aps..apr.k1002k&link_type=abstract
American Physical Society, April Meeting, 2004, May 1-4, 2004, Denver, Colorado April 2004, MEETING ID: APR04, abstract #K1.002
Astronomy and Astrophysics
Astronomy
Scientific paper
A central problem in the study of accretion disks is the process by which angular momentum is transported outward at a rate sufficient to explain the observed luminosity of accretion-powered astronomical sources. One possibility that has been considered relies on axisymmetric modes such as the Magneto-Rotational Instability. However, our previous work [1] showed that when vertically confined in a thin accretion disk, the MRI modes became of the ballooning type instead, with radial oscillations, reduced growth rates, and additional limitations on the magnetic field strengths compatible with their excitation. We review the relevant analytical approaches and expand our previous results with numerical studies of axisymmetric modes in vertically stratified thin accretion disks, intended both to verify our previous work and to incorporate additional physical effects unsuited to an analytic approach. [1] Coppi, B. and Keyes, E.A., ApJ 595:1000-1008 (2003).
Coppi Bruno
Keyes Edward
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