Nearly sonic and trans-sonic convective motions in the solar atmosphere related to the solar wind origin

Details Nearly sonic and trans-sonic convective motions in the solar atmosphere related to the solar wind origin Nearly sonic and trans-sonic convective motions in the solar atmosphere related to the solar wind origin

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aipc..382..161v&link_type=abstract

Proceedings of the eigth international solar wind conference: Solar wind eight. AIP Conference Proceedings, Volume 382, pp. 161

Physics

2

Particle Emission, Solar Wind, Magnetohydrodynamics And Plasmas

Scientific paper

Dissipative MHD regimes in the solar atmosphere are considered. Dimensionless parameters in the energy and momentum transport equations are analysed to understand the scaling relations between the dominant physical mechanisms in the solar atmosphere. The solar wind originates as a more or less regular tiny flow when the streamlines are temporary splitted from the powerful transsonic convective motions with ascending and descending nonstationary vortices in the solar atmosphere. There is no smooth quasistationary ``critical surface'' around the Sun where the sonic transition takes place.

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