Streamer Waves and Associated Coronal Seismological Study

Details Streamer Waves and Associated Coronal Seismological Study Streamer Waves and Associated Coronal Seismological Study

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh11b1651c&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH11B-1651

Physics

Plasma Physics

[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7836] Space Plasma Physics / Mhd Waves And Instabilities

Scientific paper

Streamer waves, excited by the CME attack on the streamer structure, represent one of the largest wave phenomena ever observed in the solar corona. One typical such event was recorded by LASCO/SOHO on July 6th of 2004 (Chen et al., ApJ, 2010). At the beginning of the event, the streamer was pushed aside from their equilibrium position upon the hit of the rapidly outgoing and expanding CME ejecta; then, the streamer structure, mainly the bright streamer stalk, exhibited elegant large scale sinusoidal wavelike motions. The motions were apparently driven by the restoring magnetic forces resulting from the CME impingement, suggestive of the fast-body kink mode supported by and propagating outwards along the plasma sheet of the streamer. With the whitelight coronagraph data, we show that the streamer wave has a period of about 1 hour, a wavelength varying from 2 to 4 solar radii, an amplitude of about a few tens of solar radii, and a propagating phase speed in the range 300 to 500 km/s. With these measurements and available observational constraints on the solar wind parameters, we develop a seimological technique to diagnose the radial profiles of the Alfven speed and magnetic field strength in the region surrouding the plasma sheet structure from 3 to 10 solar radii.

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