Models for magnetic heating of the solar atmosphere
نویسنده
چکیده
Sustaining the hot solar corona requires an energy flux of up to about 10erg cm−2s−1 whose source must be the photospheric motions below. However, the precise way this energy is transferred and damped still remains an open question. Here a review of recent advances in theoretical models for coronal heating, in the light of the fundamental observational results of the last decade, will be
منابع مشابه
ar X iv : a st ro - p h / 07 03 57 5 v 1 2 1 M ar 2 00 7 Modeling the ( upper ) solar atmosphere including themagnetic field ⋆
The atmosphere of the Sun is highly structured and dynamic in nature. From the photosphere and chromosphere into the transition region and the corona plasma-β changes from above to below one, i.e. while in the lower atmosphere the energy density of the plasma dominates, in the upper atmosphere the magnetic field plays the governing role — one might speak of a " magnetic transition ". Therefore ...
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