Solar wind flow upstream of the coronal slow shock

Details Solar wind flow upstream of the coronal slow shock Solar wind flow upstream of the coronal slow shock

Aug 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...307..838w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 307, Aug. 15, 1986, p. 838-846.

Astronomy and Astrophysics

Astrophysics

10

Magnetohydrodynamic Flow, Shock Wave Propagation, Solar Corona, Solar Wind, Axisymmetric Flow, Coronal Holes, Flow Geometry, Stellar Models

Scientific paper

Slow shocks have been predicted to exist embedded in large coronal holes at low altitude. Two or more curved slow shocks may link together to form a composite discontinuity surface around the sun which may be called the coronal slow shock (CSS). Here a solar-wind model is studied under the assumption that a standing CSS exists and cororates with the sun at a constant angular velocity. A steady, axisymmetrical one-fluid model is introduced to study the expansion of solar wind in the open-field region upstream of the CSS. The model requires that the conditions downstream of the CSS near the equatorial plane can produce a solar wind agreeable with the observations made near the earth's orbit. The paper presents an illustrative calculation in which the polar caps within 60 deg of the polar angle are assumed to be the source region of the solar wind.

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