The Structure of the Static Corona and Transition Region,
STANFORD UNIV CA CENTER FOR SPACE SCIENCE AND ASTROPHYSICS
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Static models of coronal loops are investigated. For loops that are low-flying, heights above the chromosphere somewhat 5000 km, it is shown that a new type of solution appears to the static equations, in addition to the well known coronal loop solution. The new solution is characterized by a maximum plasma temperature somewhat 100000 K. The structure and properties of these cool solutions are discussed. We calculate the differential emission measure QT expected for a magnetic arcade, which we argue must naturally contain both hot and cool loops. It is shown that the cool loops have a dramatic effect on the form of QT in the lower transition region. In particular, they can account for the observed rise in Q at low T, which has long been thought to be incomparable with the static-loop model. Finally, we dicuss the implications of the cool loops on other observations of both solar and stellar coronae and transition regions.