On the kinetics of solar wind acceleration

Details On the kinetics of solar wind acceleration On the kinetics of solar wind acceleration

Mar 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977a%26a....55..229b&link_type=abstract

Astronomy and Astrophysics, vol. 55, no. 2, Mar. 1977, p. 229-237.

Astronomy and Astrophysics

Astrophysics

1

Hydrogen Plasma, Magnetohydrodynamic Stability, Plasma Acceleration, Solar Wind Velocity, Astrophysics, Solar Protons, Stellar Models

Scientific paper

A two-stream model of solar-wind hydrogen-plasma expansion is outlined in which protons at any one level of flux generation are divided into those that collide rapidly relative to their expansion times and those that leave the sun without significant relaxation. Proton evaporation is explicitly taken into account along with momentum and energy gains due to friction with escaping protons. This model is investigated numerically by an iteration technique, assuming a lateral expansion of the solar wind. It is found that for very low temperatures, proton acceleration is caused mainly by a lack of fast-particle collisions and that the collisional population is more accelerated and denser at higher temperatures. The results also show that evaporation over a large extent of height reduces the solar-wind heating requirements to the region of the low corona. Examination of the physical stability of the solar-wind plasma in this model indicates that no electrostatic two-stream instability can arise, the firehose-instability condition could be satisfied only with very low temperatures near the level of full evaporation, and a point of serious instability with respect to magnetosonic whistlers occurs at a heliocentric distance of about 10 solar radii.

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