Abstract
Energy is transmitted into, out of and across the solar atmosphere by such physical processes as radiation, thermal conduction, waves and so forth. Estimates can be made of the magnitudes of some of these and hence an energy budget drawn up for different regions of the atmosphere. In particular it appears that the energy requirements of coronal hole regions of the solar surface are substantially greater than those of other regions. The main factor determining this conclusion is an estimate of the energy required to accelerate the solar wind in regions above coronal holes. Of two possible mechanisms for the acceleration of the solar wind, namely thermal plasma pressure and Alfvén waves, it may be shown that the former places even more severe demands on the energy budget of these regions, whereas the latter is more easily accommodated.
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Schedule a callMore From: Philosophical Transactions of the Royal Society of London. Series A, Mathematical and Physical Sciences
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