Effects of rapidly diverging flow, heat addition, and momentum addition in the solar wind and stellar winds

Details Effects of rapidly diverging flow, heat addition, and momentum addition in the solar wind and stellar winds Effects of rapidly diverging flow, heat addition, and momentum addition in the solar wind and stellar winds

Jan 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977jgr....82...23h&link_type=abstract

Journal of Geophysical Research, vol. 82, Jan. 1, 1977, p. 23-35.

Physics

97

Heat Transfer, Momentum Transfer, Solar Wind, Stellar Winds, Critical Point, Divergence, Electron Energy, Flow Geometry, Supersonic Flow, Topology, Two Fluid Models

Scientific paper

One-fluid models of the solar wind and stellar winds are presented taking account of rapid flow tube divergence and heat and momentum addition, and two-fluid models of the solar wind are presented taking account of heat addition. It is found that heat addition, momentum addition, or the rapid divergence of a flow tube can produce more than one critical point in the solution topologies of the solar and stellar wind equations. For the solar wind, additional critical points associated with rapid flow tube divergence and/or with momentum addition can lead to high expansion speeds near the coronal base. These high speeds together with a rapid flow tube divergence allow for the possibility of an enhancement of conductive energy per unit mass supplied to the coronal expansion. For radiation-driven stellar winds the additional critical points associated with rapid flow tube divergence can lead to supersonic flow much deeper in the stellar atmosphere than is predicted by radial, spherically symmetric flow models.

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