Slow magnetoacoustic waves in coronal loops

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

Oct 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26a...362.1151n&link_type=abstract

Astronomy and Astrophysics, v.362, p.1151-1157 (2000)

Astronomy and Astrophysics

Astrophysics

78

Magnetohydrodynamics (Mhd), Waves, Sun: Activity, Sun: Corona, Sun: Oscillations, Sun: Uv Radiation

Scientific paper

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.

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