Nonequilibrium ionization in solar and stellar winds
Nonequilibrium ionization in solar and stellar winds
复制标题
太阳风和恒星风中的非平衡电离
DOI：
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发表时间：
1979
期刊：
影响因子：
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通讯作者：
P. Shapiro
中科院分区：
文献类型：
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作者：
A. Dupree;R. Moore;P. Shapiro
当质量外流存在时，在太阳过渡区和日冕中可能发生大量和系统的电离平衡偏离。模拟计算说明了这些区域电离平衡的一般特征。非平衡条件的存在为在太阳翼上观测到的EUV线发射扩展区域提供了一种自然的解释。与观测到的日冕洞的比较表明，直到温度达到约250000 K时才会开始流出。其他后果包括日冕洞的紫外线和射电观测之间的密度差异的缩小，以及对太阳和恒星大气中能量平衡的潜在影响。
Substantial and systematic departures from ionization equilibrium can occur in the solar transition region and corona when mass outflows are present. Modeling calculations illustrate the general characteristics of the ionization balance in such regions. The presence of nonequilibrium conditions suggests a natural explanation for the extended region of EUV line emission that is observed above the solar limb. Comparison with observations of a coronal hole on the disk indicates that outflow may not start until temperatures of about 250,000 K are reached. Additional consequences include a diminution of the density discrepancy between ultraviolet and radio observations of coronal holes, and potential effects on the energy balance in solar and stellar atmospheres undergoing mass loss.