Abstract
The solar corona is an extremely hot (106 K or about 0.1 keV), almost fully ionised plasma which extends from a few thousand km above the Sun’s visible surface or photosphere (6000 K) to where it freely expands into the solar system as the solar wind. The exact reasons for its high temperature are still being debated despite more than 50 years of research, but magnetic fields are believed to be responsible for this heating. This article reviews some recent progress in our understanding, using data from spacecraft (Yohkoh, SOHO and TRACE) and from ground-based eclipse observations.
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Dwivedi, B.N. (2003). The Solar Corona. In: Antia, H.M., Bhatnagar, A., Ulmschneider, P. (eds) Lectures on Solar Physics. Lecture Notes in Physics, vol 619. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-36963-5_8
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DOI: https://doi.org/10.1007/3-540-36963-5_8
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