Plasma flow around coronal loops

Details Plasma flow around coronal loops Plasma flow around coronal loops

Sep 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982soph...80..173h&link_type=abstract

Solar Physics, vol. 80, Sept. 1982, p. 173-183.

Physics

4

Coronal Loops, Current Density, Energy Transfer, Magnetohydrodynamic Flow, Photosphere, Magnetohydrodynamic Stability, Solar Corona, Stellar Models, Time Dependence

Scientific paper

Current dissipation models of coronal loop heating are studied. Turbulent current dissipation is shown to lead to a time dependent process because of an enormous mass motion induced in the current layer. A stationary heating process involves only ohmic heating, which requires a large current layer. To insure MHD stability, the loop must be composed of many elements with the oppositely directed currents. A stationary current dissipation process induces the plasma motion across the magnetic field into the loop and down the loop with the speeds of about ten thousand and twenty thousand cm/s, respectively. The pressure of the loop is also estimated to be proportional to the current density: p/J = 6.3 x 10 to the -8th dyn/statamp.

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