MHD solution of interplanetary disturbances generated by simulated velocity perturbations

Details MHD solution of interplanetary disturbances generated by simulated velocity perturbations MHD solution of interplanetary disturbances generated by simulated velocity perturbations

Nov 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976jgr....81.5413d&link_type=abstract

Journal of Geophysical Research, vol. 81, Nov. 1, 1976, p. 5413-5419.

Physics

15

Digital Simulation, Interplanetary Magnetic Fields, Magnetic Disturbances, Magnetohydrodynamic Flow, Shock Wave Propagation, Solar Activity Effects, Solar Wind Velocity, Plasma Density, Radial Velocity, Solar Corona, Spatial Distribution, Time Dependence

Scientific paper

An MHD time-dependent numerical simulation, restricted to the solar equatorial plane, is used to demonstrate the interplanetary disturbances caused by several simplified coronal holes. Each 'hole' is assumed to have a configuration such that the higher solar wind velocity produced within their longitudinal extent is Gaussian over a 7-day period at the inner boundary (0.3 AU) of the numerical simulation. A second, twin coronal hole is assumed to rotate on the solar disk behind its predecessor. It is shown that the first coronal hole-produced interplanetary shock ensemble is overtaken by the second ensemble because of the higher velocity, lower density environment into which the latter propagates. A number of features predicted by MHD similarity theory are confirmed by the numerical simulation. These features include (1) strong azimuthal magnetic and plasma density compression, accompanied with average temperature depression, at the contact surface between forward and reverse shock ensembles, and (2) increasing spatial separation distance between forward and reverse shocks.

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