Evolution of fast and slow shock interactions in the inner heliosphere

Details Evolution of fast and slow shock interactions in the inner heliosphere Evolution of fast and slow shock interactions in the inner heliosphere

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004soph..223..259w&link_type=abstract

Solar Physics, Volume 223, Issue 1-2, pp. 259-282

Physics

6

Scientific paper

We use a one-dimensional, time-dependent adaptive grid MHD code to study the interaction between fast and slow shocks in the solar wind. Our results show that: (1) a forward slow shock (FSS) can be destroyed by a forward fast shock (FFS) that overtakes it from behind; (2) two propagating FSSs can merge into a stronger FSS; (3) a strong FSS can survive by following a strong forward fast shock; and (4) the strength of a FSS is decreased by following an FFS. These simulation results reproduce an important feature of the Helios observations (Richter, 1987) where transient fast shocks were more frequently followed within a few hours by slow shock ype discontinuities rather than by fast reverse shocks.

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