Solar Corona Seismology

Details Solar Corona Seismology Solar Corona Seismology

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006lnea....2...91b&link_type=abstract

Lecture Notes and Essays in Astrophysics, vol. 2, p. 91-110.

Astronomy and Astrophysics

Astrophysics

1

Solar Corona, Solar Seismology, Magnetohydrodynamic Waves

Scientific paper

The presence of oscillations in solar coronal structures has been known for more than seventy years. Observational reports about the presence of oscillatory motions in solar filaments go back to 1930 while in the case of other coronal structures (loops, plumes, etc) direct evidence has been recently obtained thanks to the detailed observations made by SoHO and TRACE. Due to these satellites, as well as to ground-based observations, evidence of magnetohydrodynamic (MHD) waves in the solar corona has risen dramatically. MHD coronal seismology provides with an indirect path to determine the physical conditions and parameters of the solar corona [coronal magnetic field, transport coefficients (viscosity, resistivity, thermal conductivity, etc.), heating function, filling factors] which are difficult to measure accurately. In essence, it is similar to the acoustic diagnostic of the solar interior (Helioseismology) and to MHD spectroscopy used to determine physical helioseismology parameters of laboratory plasmas. In spite that there are many solar coronal structures in which oscillations have been detected (prominences, loops, plumes, coronal holes, etc.), in the following we will concentrate in prominences and coronal loops trying to summarize part of our current knowledge about their oscillations as well as about the theoretical models developed to explain those oscillations in terms of MHD waves.

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