A Model for the Sources of the Slow Solar Wind

Details A Model for the Sources of the Slow Solar Wind A Model for the Sources of the Slow Solar Wind

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21640521a&link_type=abstract

American Astronomical Society, AAS Meeting #216, #405.21; Bulletin of the American Astronomical Society, Vol. 41, p.892

Astronomy and Astrophysics

Astronomy

Scientific paper

Models for the origin of the slow solar wind must account for two seemingly contradictory observations: The slow wind has the composition of the closed-field corona, implying that it originates at the open-closed field boundary layer, but it also has large angular width, up to 40 degrees. We propose a model that can explain both observations. The key idea is that the source of the slow wind at the Sun is a network of narrow (possibly singular) open-field corridors that map to a web of separatrices and quasi-separatrix layers in the heliosphere. We calculate with high numerical resolution, the quasi-steady solar wind and magnetic field for a Carrington rotation centered about the August 1, 2008 total solar eclipse. Our numerical results demonstrate that, at least for this time period, a web of separatrices (S-web) forms with sufficient density and extent in the heliosphere to account for the observed properties of the slow wind. We discuss the implications of our S-web model for the structure and dynamics of the corona and heliosphere, and propose further tests of the model.
This work was supported, in part, by the NASA HTP, TR&T and SR&T programs.

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