期刊
ASTRONOMY & ASTROPHYSICS
卷 379, 期 3, 页码 1106-1112出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361:20011378
关键词
magnetohydrodynamics (MHD); waves; Sun : activity; Sun : corona; Sun : oscillations; Sun : UV radiation
A model interpreting variations of EUV brightness upward propagating in solar coronal loops as slow magnetoacoustic waves is developed. A loop is considered to have a non-zero plane inclination angle and offset of the circular loop centre from the baseline. The model also incorporates effects of dissipation and gravitational stratification. A linear evolutionary equation is derived and applied to investigations of slow wave dynamics. Both the non-zero plane inclination and the offset decrease the growth of the wave amplitude due to stratification. It is shown that wide-spectrum slow magnetoacoustic waves, consistent with currently available observations in the low frequency part of the spectrum, can provide a rate of heat deposition sufficient to heat the loop. In this scenario, the heat would be deposited near the loop footpoints, which agrees with the current observational data.
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