Observational limits on the coronal hole flow geometry in an Alfven wave-driven solar wind

Details Observational limits on the coronal hole flow geometry in an Alfven wave-driven solar wind Observational limits on the coronal hole flow geometry in an Alfven wave-driven solar wind

Sep 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...344..513j&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 344, Sept. 1, 1989, p. 513-521. Research supported by CNPq.

Astronomy and Astrophysics

Astrophysics

24

Coronal Holes, Solar Corona, Solar Magnetic Field, Solar Wind, Magnetic Field Configurations, Magnetohydrodynamic Waves, Stellar Models

Scientific paper

A model for a coronal hole geometry in the sun is proposed, asuming Alfven wave momentum deposition in the wind. For a wide range of characteristic damping lengths, it is shown that the observational data are not satisfied by the initial rapid divergence flow geometry of Hollweg (1986) and Kuin and Hearn (1982). Also, it is suggested that the slow, spherically symmetric divergent geometry of Hammer (1982) does not agree with observations either. It is found that Alfven wave deposition and observational data require a combination of a slow divergence in a coronal hole up to 0.01-0.1 solar radius, with a rapid divergence after about 1 solar radius.

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