Transport of Magnetohydrodynamic Fluctuations in the Solar Corona

Details Transport of Magnetohydrodynamic Fluctuations in the Solar Corona Transport of Magnetohydrodynamic Fluctuations in the Solar Corona

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh41a19m&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH41A-19

Mathematics

Logic

2149 Mhd Waves And Turbulence, 7509 Corona, 7859 Transport Processes, 7863 Turbulence

Scientific paper

Transport and dissipation of turbulent fluctuations may play an active role both in solar coronal heating and solar wind acceleration. We assume coronal conditions, and make use of the reduced magnetohydrodynamic approximation. The fluctuations are thus transported by a smooth background plasma density and magnetic field. The background velocity field is assumed to be much smaller than the background magnetic field. The effect of the non-linearities is modeled phenomenologically, with special consideration of the role of the cross and magnetic helicities. A set of transport equations, as well as some preliminary solutions, are presented. This research is supported by NASA grants NAG5-7164 and NAG5-8134 (SECTP) and by NSF under grant ATM-9713595.

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