A numerical investigation of the Kelvin-Helmholtz instability in the context of accreting neutron stars

Details A numerical investigation of the Kelvin-Helmholtz instability in the context of accreting neutron stars A numerical investigation of the Kelvin-Helmholtz instability in the context of accreting neutron stars

Oct 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...139...93w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 139, no. 1, Oct. 1984, p. 93-103. Research supported by the Max-Planck-Gesells

Statistics

Computation

24

Computational Astrophysics, Kelvin-Helmholtz Instability, Magnetopause, Neutron Stars, Stellar Mass Accretion, X Ray Sources, Mach Number, Pulsars, Stellar Gravitation, Stellar Magnetic Fields

Scientific paper

The development of the Kelvin-Helmoltz instability is investigated numerically using a two-dimensional magnetohydrodynamic code. First, some idealized field-free configurations involving two initially uniform fluids in relative motion are considered. Attention is given to the formation and evolution of vortices, the width and structure of the developing shear layer, the nonlinear growth rate and saturation of the Kelvin-Helmholtz modes, and their dominant scale. The effect of a magnetic field frozen into one of the fluids and aligned parallel or perpendicular to the direction of streaming is then examined. A vertical gravitational field is introduced, and the transition from Rayleigh-Taylor to Kelvin-Helmholtz instability as the Mach number of the flow increases is discussed. Finally, the astrophysical implications are briefly examined.

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