Computer Science
Scientific paper
Jun 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987natur.327..685a&link_type=abstract
Nature (ISSN 0028-0836), vol. 327, June 25, 1987, p. 685-687.
Computer Science
10
Coronal Loops, Flow Distribution, Magnetohydrodynamic Flow, Solar Magnetic Field, Magnetic Field Configurations, Solar Atmosphere, Solar Wind
Scientific paper
The existence of the solar wind requires a net outflow of material at all depths in the solar atmosphere. Thus, the observation of a prevalent downflow at temperatures near 100,000 K presents a considerable challenge. Two classes of flow models have been suggested, each involving flow along closed magnetic-field lines that extend above the chromosphere into the hotter transition region and corona. Type-(1) models assume unidirectional equilibrium flows along field lines and rely on asymmetry in the flow and plasma properties to produce an apparent downflow. Type-(2) models, by comparison, assume a series of episodic upflows and subsequent downflows along each line of force and rely on asymmetry in the plasma properties and flow durations to produce a statistically prevalent downflow. Here it is argued that observational evidence strongly suggests that both types of flow are present but that type-(2) flow is predominant.
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