Shock Formation and Energy Dissipation of Slow Magnetosonic Waves in Coronal Plumes

Details Shock Formation and Energy Dissipation of Slow Magnetosonic Waves in Coronal Plumes Shock Formation and Energy Dissipation of Slow Magnetosonic Waves in Coronal Plumes

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003csss...12..624c&link_type=abstract

The Future of Cool-Star Astrophysics: 12th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (2001 July 30 - August

Astronomy and Astrophysics

Astrophysics

Sun, Shock Waves, Magnetohydrodynamics, Solar Wind, Solar Corona

Scientific paper

We study the shock formation and energy dissipation of slow magnetosonic waves in coronal plumes. The wave parameters and the spreading function of the plumes as well as the base magnetic field strength are given by empirical constraints mostly from SOHO/UVCS. Our models show that shock formation occurs at low coronal heights, i.e., within 1.3 R

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