Coronal prominence structure and dynamics: A magnetic flux rope interpretation
The solar prominence is an example of a space physics phenomenon that can be modeled as a twisted magnetic flux tube or magnetic flux "rope." In such models the prominence is one observable part of a larger magnetic structure capable of storing magnetic energy to drive eruptions. We show how a flux rope model explains a range of observations of prominences and associated structures such as cavities and soft X-ray sigmoids and discuss in particular the observational and dynamic consequences of three-dimensional reconnections in and around the evolving magnetic flux rope. We demonstrate that the flux rope model can describe the prominence's preeruption structure and dynamics, loss of equilibrium, and behavior during and after an eruption in which part of the flux rope is expelled from the corona.
document
https://n2t.org/ark:/85065/d7r49qz0
eng
geoscientificInformation
Text
publication
2016-01-01T00:00:00Z
publication
2006-12-09T00:00:00Z
Copyright 2006 American Geophysical Union.
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