Role of plasma flow in determining structure of the chromosphere-corona transition zone of the sun

✍ Scribed by W. M. Glencross

• Publisher: Springer
• Year: 1981
• Tongue: English
• Weight: 650 KB
• Volume: 73
• Category: Article
• ISSN: 0038-0938
• DOI: 10.1007/bf00153145

✦ Synopsis

Transfer of material between the chromosphere and corona of the Sun must occur whenever the geometry of any interconnecting magnetic structure changes, and there will also be a flow of plasma along field lines caused by any pressure difference between the two feet of each arch. Part of the energy conducted downwards towards the chromosphere is required to heat plasma rising into the corona, whereas material falling back towards the solar surface gives up energy to reinforce the conducted flow.

This study shows that the term associated with flow is comparable to the radiation-loss term in the energy budget of the transition zone if the plasma speed at the base of the corona reaches about 3 km s -1. This value is probably exceeded within most flux tubes during some period of their development, and speeds an order of magnitude higher can occur in favourable regions.

This paper also examines limits to the temperature gradient of the transition zone set by the requirement of continuity of plasma flow.