NASA Logo

NTRS

NTRS - NASA Technical Reports Server

Back to Results
Basic properties and models of solar prominencesProminences are relatively cool (10,000 K) and dense plasma clouds which may persist for 100 days or more in the midst of the much hotter (1 million K) and more tenuous (10 exp 9/cu cm) corona. Many observations imply that the magnetic field in and around prominences is responsible both for isolating prominences from the corona and for supporting them against gravity. It is not at all obvious how the magnetic field can do both these tasks, but the limited theoretical models that are available suggest that a magnetic-flux rope is involved. Using a new analytical model, it is argued that the flux rope could also play a key role in the eruption of a prominence by supplying the magnetic energy necessary to drive the prominence outwards.
Document ID
19920048616
Acquisition Source
Legacy CDMS
Document Type
Conference Proceedings
Authors
Forbes, T. G.
(New Hampshire, University Durham, United States)
Date Acquired
August 15, 2013
Publication Date
January 1, 1990
Subject Category
Solar Physics
Accession Number
92A31240
Funding Number(s)
CONTRACT_GRANT: NAGW-76
CONTRACT_GRANT: NSF ATM-87-11089
Distribution Limits
Public
Copyright
Other

Available Downloads

There are no available downloads for this record.
No Preview Available