Slow magnetoacoustic waves in coronal loops
V.M. Nakariakov 1,
E. Verwichte 2,
D. Berghmans 2 and
E. Robbrecht 2,3
Received 29 June 2000 / Accepted 31 August 2000
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.
Key words: Magnetohydrodynamics (MHD) waves Sun: activity Sun: corona Sun: oscillations Sun: UV radiation
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© European Southern Observatory (ESO) 2000
Online publication: October 30, 2000