An overview of coronal seismology.
The idea of exploiting observed oscillations as a diagnostic tool for determining the physical conditions of the coronal plasma was first suggested several decades ago (Roberts et al. 1984 Astrophys. J. 279, 857). Until recently, the application of this idea has been very limited by a lack of high-quality observations of coronal oscillations. However, during the last few years, this situation has changed dramatically, especially due to space-based observations by the Solar and Heliospheric Observatory and the Transition Region and Coronal Explorer and waves and oscillations have now been observed in a wide variety of solar structures, such as coronal loops, polar plumes and prominences. This paper will briefly summarize MHD wave theory, which forms the basis for coronal seismology, as well as present an overview of the variety of recently observed waves and oscillations in the solar corona. The present state of coronal seismology will also be discussed. Currently, the uncertainty associated with the obtained parameters is still considerable and, hence, the results require a cautious interpretation. However, these examples do show that coronal seismology is rapidly being transformed from a theoretical possibility to a viable technique.
De Moortel
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University of St Andrews School of Mathematics and Statistics North Haugh, St Andrews KY16 9SS, UK. inecke@mcs.st-and.ac.uk
D003198:Computer Simulation; D005740:Gases / Q000737:chemistry*; D005844:Geology / Q000379:methods*; D006358:Hot Temperature; D008956:Models, Chemical; D009991:Oscillometry / Q000379:methods*; D012212:Rheology / Q000379:methods*; D019445:Solar Activity; D016082:Solar System; D014732:Vibration
D005740:Gases