Slow magnetoacoustic waves in coronal loops
UNSPECIFIED. (2000) Slow magnetoacoustic waves in coronal loops. ASTRONOMY & ASTROPHYSICS, 362 (3). pp. 1151-1157. ISSN 0004-6361Full text not available from this repository.
A theoretical model interpreting propagating disturbances of EUV emission intensity, recently observed in coronal loops, is constructed in terms of slow magnetoacoustic waves. The model is one-dimensional and incorporates effects of nonlinearity, dissipation due to finite viscosity and thermal conduction, and gravitational stratification of plasma in the loop. It has been found that, for the observationally detected parameters of the waves, the main factors influencing the wave evolution are dissipation and stratification. The upwardly propagating waves of observed periods (5-20 min) are found to decay significantly in the vicinity of the loop apex, explaining the rarity of observational detection of downwardly propagating waves. The model provides a theoretical basis for development of MHD seismology of the coronal loops.
|Item Type:||Journal Article|
|Subjects:||Q Science > QB Astronomy|
|Journal or Publication Title:||ASTRONOMY & ASTROPHYSICS|
|Official Date:||October 2000|
|Number of Pages:||7|
|Page Range:||pp. 1151-1157|
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