MHD Shock Interactions in Coronal Structures

Details MHD Shock Interactions in Coronal Structures MHD Shock Interactions in Coronal Structures

Nov 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996soph..169..151g&link_type=abstract

Solar Physics, Volume 169, Issue 1, pp.151-166

Physics

4

Scientific paper

We consider the magnetohydrodynamic (MHD) interactions of solar coronal fast shock waves of flare and/or nonflare origin with the boundaries of coronal streamers and coronal holes. Boundaries are treated as MHD tangential discontinuities (TD). Different parameters of the observed corona are used in the investigation. The general case of the oblique interaction is studied. It is shown that a solar fast shock wave must be refracted usually as a fast shock wave inside the coronal streamer. For the special case of the velocity shear across TD, a slow shock wave is generated. On the contrary, the shock wave refracted inside the coronal hole is indeed a slow shock wave. The significance of different effects due to the interaction of fast and slow shock waves on the coronal magnetic field is noticed, especially at the time of a coronal mass ejection (CME). It is also shown, that an oblique fast MHD coronal shock wave may trigger an instability at the boundary of a streamer considered as a TD. It might have a relation with the observed process of abrupt disappearance of the streamer's boundary in the solar corona.

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