Stability of accretion column flows

Details Stability of accretion column flows Stability of accretion column flows

Oct 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26a....90..359h&link_type=abstract

Astronomy and Astrophysics, vol. 90, no. 3, Oct. 1980, p. 359-365.

Astronomy and Astrophysics

Astrophysics

15

Flow Stability, Stellar Mass Accretion, X Ray Sources, Optical Thickness, Small Perturbation Flow, Taylor Instability

Scientific paper

The stability of both a spherically symmetric optically thin accretion and an optically thick accretion column are examined. For optically thick conditions, it is shown that radiation-pressure dominated flows near the Eddington limit are, under the usual physical conditions, unstable to a Rayleigh-Taylor type of instability. Yet an optically thin flow is stable against radial modes, both in cases where a time lag between accretion fluctuations and the resulting changes in luminosity is incorporated or not. These studies indicate that realistic accretion models should take into account strong micro-inhomogeneity likely to be present in accretion columns.

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