The acceleration of the solar wind

Journal Article · Sat Jul 20 04:00:00 EDT 1996 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.51363· OSTI ID:21163525

Axford, W I; McKenzie, J F ^[1]

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1. Max Planck Institut fuer Aeronomie, 37191 Katlenburg-Lindau (Germany)

We review the observed properties of the solar wind with the aim of finding a simple and straightforward understanding of its origin and acceleration. A theory is developed for the high speed solar wind based on a simple dissipation length assumption for hydromagnetic wave heating of the coronal plasma close to the Sun. Solutions with the correct particle and energy fluxes and with a realistic magnetic field, match the requirements on the density at the base of the corona provided the dissipation length is relatively small ({approx}0.25-0.5 solar radii). The significant features are that the acceleration is rapid, with the sonic point within {approx}2 solar radii, and the proton temperatures are high, namely 8-10x10{sup 6} K. Such efficient dissipation requires any Alfven waves responsible to have frequencies in the range 0.01 Hz-10 kHz. This has implications for the nature of the plasma and energy source in the supergranular network.

• OSTI ID: 21163525
• Journal Information: AIP Conference Proceedings, Journal Name: AIP Conference Proceedings Journal Issue: 1 Vol. 382; ISSN 0094-243X; ISSN APCPCS
• Country of Publication: United States
• Language: English

Related Subjects

70 PLASMA PHYSICS AND FUSION TECHNOLOGY
ACCELERATION
ALFVEN WAVES
ASTROPHYSICS
HEATING
KHZ RANGE
LENGTH
MAGNETIC FIELDS
MATHEMATICAL SOLUTIONS
PLASMA
PLASMA DENSITY
PROTON TEMPERATURE
SOLAR CORONA
SOLAR WIND
VELOCITY