Microflares and Hot Coronal Loop Oscillations

Details Microflares and Hot Coronal Loop Oscillations Microflares and Hot Coronal Loop Oscillations

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.1316t&link_type=abstract

American Astronomical Society, SPD meeting #37, #13.16; Bulletin of the American Astronomical Society, Vol. 38, p.243

Astronomy and Astrophysics

Astronomy

Scientific paper

Detailed observations of waves and oscillations in coronal loops may be useful in the diagnostics of coronal plasma (Roberts et. al 1984). Very recent SOHO/SUMER spectroscopic observations have revealed strongly damped slow-mode oscillations in the hot coronal loops (e.g. Wang et al. 2002). They can be seen in the hot flare-like lines (e.g. Fe XIX) as intensity and Doppler shift fluctuations with large initial Doppler velocities. They are triggered by microflares, small A to C class X-ray brightenings that occur at a rate of about 10 per hour in an 'average' active region (Shimizu et al. 1992). We study the basic characteristics of the oscillations and discuss their importance in the context of models of microflare loop excitation.

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