POSTER PAPER 1.10
Shock Formation and Energy Dissipation of
Slow Magnetosonic Waves in Coronal Plumes
M. Cuntz,S. T. Suess
Institute: Department of Physics, University of Texas at Arlington
Institute: Space Science Laboratory, NASA Marshall Space Flight Center
Contact Email: cuntz@uta.edu
Abstract:
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 RSun,
depending on the model parameters. In addition, following
analytical estimates, we show that scale height of energy dissipation
by the shocks ranges between 0.15 and 0.45 RSun. This
implies that shock heating by slow magnetosonic waves
is relevant at most heights, even though this type of waves
is apparently not a solely operating energy supply mechanism.
Index Keywords: Sun; Shock Waves; Magnetohydrodynamics; Solar Wind; Solar Corona
Previous: Doyle
Next: Vauclair
Up: Poster Index
Up: Top Index
Manuscript submitted: 2001-Sep-17
"The Future of Cool-Star Astrophysics", 2003, Eds. A. Brown,
G. M. Harper, & T. R. Ayres.
Proceedings of 12th Cambridge Workshop on Cool Stars, Stellar Systems,
& The Sun,
© 2003 University of Colorado.