Further numerical studies of the Rayleigh-Taylor instability in the context of accreting X-ray sources

Details Further numerical studies of the Rayleigh-Taylor instability in the context of accreting X-ray sources Further numerical studies of the Rayleigh-Taylor instability in the context of accreting X-ray sources

Jun 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...135...66w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 135, no. 1, June 1984, p. 66-76. Research supported by the Deutsche Forschungs

Astronomy and Astrophysics

Astrophysics

10

Magnetohydrodynamic Stability, Neutron Stars, Stellar Mass Accretion, Taylor Instability, X Ray Sources, Earth Magnetosphere, Pulsars, Rayleigh Scattering, Stellar Magnetic Fields

Scientific paper

An earlier investigation of the nonlinear Rayleigh-Taylor instability for accreting X-ray sources is extended to allow for more realistic initial conditions. The two-dimensional computations show the heavy and light fluids undergoing complementary circulatory motions which result in the formation of alternating inverted and upright 'mushroom' structures along the interface. The structures develop independently of the shape of the initial perturbation. Short wavelength modes have a strong tendency to dominate long ones, with the lower bound being set by viscous damping. A relatively modest vertical magnetic field will act to suppress the vortex motions and produce a 'bubble and spike' structure. A crude simulation of the instability occurring in a radiation-supported accretion column is presented; after a slow start, the magnetically constrained plasma drips down into the photon medium in the form of long narrow fingers, the dominant scale-length being determined by radiative viscosity.

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