The viscous evolution of elliptical accretion discs

Details The viscous evolution of elliptical accretion discs The viscous evolution of elliptical accretion discs

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.255...92s&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 255, March 1, 1992, p. 92-104.

Astronomy and Astrophysics

Astrophysics

35

Accretion Disks, Ellipticity, Galactic Evolution, Stellar Evolution, Viscous Flow, Cataclysmic Variables, Galactic Nuclei, Gas Dynamics, Line Spectra, Perturbation Theory, Protostars

Scientific paper

The widely accepted assumption that an accretion flow should circularize on a time-scale much shorter than the viscous time-scale is examined. An analytic calculation is provided, supplemented by a generalization of the circular disks of Shakura and Sunyaev, and some 'sticky-particle' numerical simulations, both of which suggest that the converse might be the case (i.e., that initially elliptical disks could retain their shape over a viscous time-scale, or even become more elliptical). It is argued that there are astrophysical implications of such a result for initially eccentric streams of gas, either in a Kepler potential, or where the accretion rate is high compared to the rate of differential precession of streamlines.

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