Slow magnetoacoustic waves in coronal loops

Details Slow magnetoacoustic waves in coronal loops Slow magnetoacoustic waves in coronal loops

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.506..705n&link_type=abstract

In: Solar variability: from core to outer frontiers. The 10th European Solar Physics Meeting, 9 - 14 September 2002, Prague, Cze

Physics

2

Solar Corona, Mhd Waves, Coronal Heating

Scientific paper

Propagating disturbances of EUV emission, recently discovered in coronal loops with SOHO/EIT and TRACE, are interpreted as slow magnetoacoustic waves. This interpretation is based upon several observational findings: (a) the disturbances seem to propagate along the magnetic field (b) at a constant speed which is below the estimated sound speed, (c) the perturbations are compressible, (d) the periods are shorter than the acoustic cut-off period in the corona. A theoretical model describing the wave evolution and incorporating effects of dissipation, stratification and weak nonlinearity is created. In particular, the model explains why only the upwardly propagating waves are observed. The interpretation suggested is in a good agreement with obervational findings. It is shown that wide spectrum slow magnetoacoustic waves, consistent with currently available observations in the low frequency part of the spectrum, can provide the rate of heat deposition sufficient to heat the loop. In this scenario, the heat would be deposited near the loop footpoints which also agrees with the current observational data. The analysis of simultaneous observations of propagating EUV disturbances in 171 Å and 195 Å bandpasses of TRACE telescope shows high correlation which systematically decreases with the distance along the loop.

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