Abstract
New results of the numerical modeling of the response of the outer atmosphere of the Sun to an impulsive heating are presented. Features of the general process are considered both for powerful and weak solar flares. For the most powerful flares it is necessary to take into account the effect of a saturation of the heat flow. Though for the most powerful solar flares the saturation of a thermal flow is not such large, the influence of this effect is important for cases of powerful flares on red dwarf stars, strongly limiting the input of the thermal energy downwards. The response of the atmosphere, which consists of the chromosphere, the transition region and the corona, to weak heating is characterized by creation no one as usually but two ascending coronal flows. The occurrence of the additional flow at coronal heights is caused by the inhomogeneous initial heating of the outer atmosphere. Some types of soft X-ray and UV-jets can be associated with such additional flow.
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