Interaction of fast and slow solar wind streams and origin of the Kelvin-Helmholtz instability

Details Interaction of fast and slow solar wind streams and origin of the Kelvin-Helmholtz instability Interaction of fast and slow solar wind streams and origin of the Kelvin-Helmholtz instability

May 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997spd....28.0271o&link_type=abstract

American Astronomical Society, SPD meeting #28, #02.71; Bulletin of the American Astronomical Society, Vol. 29, p.905

Astronomy and Astrophysics

Astronomy

Scientific paper

A high-resolution two-dimensional numerical model for the simulation of solar wind problems based on the modified TVD-LF scheme is used. A heliospheric plasma sheet is specified at the inner boundary and the time-dependent evolution of a transition region between fast and slow solar wind flows is investigated. Two simple situations with the plasma sheet assumed to be within and perpendicular to the equatorial plane are considered. Small temporal perturbations are applied to initiate the Kelvin-Helmholtz instability. Stabilization effect of non-parallel interaction (meridional plasma sheet) is shown and details of the vortex flow structures for parallel interaction equatorial plasma sheet) are presented.

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