The temperature structure, mass, and energy flow in the corona and inner solar wind
The temperature structure, mass, and energy flow in the corona and inner solar wind
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DOI：
10.1086/166015
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发表时间：
1988-02
期刊：
影响因子：
--
通讯作者：
G. Withbroe
中科院分区：
文献类型：
--
作者：
G. Withbroe
Remote-sensing and in situ data are used to constrain a radiative energy balance model in order to study the radial variations of coronal temperatures, densities, and outflow speeds in several types of coronal holes and in an unstructured quiet region of the corona. A one-fluid solar wind model is used which takes into account the effects of radiative and inward conductive losses in the low corona and the chromospheric-coronal transition region. The results show that the total nonradiative energy input in magnetically open coronal regions is 5 + or - 10 to the 5th ergs/sq cm, and that most of the energy heating the coronal plasma is dissipated within 2 solar radii of the solar surface. 106 references.
