Three-Dimensional MHD Simulation of Solar Wind Structure

Details Three-Dimensional MHD Simulation of Solar Wind Structure Three-Dimensional MHD Simulation of Solar Wind Structure

Sep 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aipc..679..133r&link_type=abstract

SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP Conference Proceedings, Volume 679, pp. 133-1

Other

Particle Emission, Solar Wind, Solar Wind Plasma, Sources Of Solar Wind, Interplanetary Magnetic Fields

Scientific paper

We examine the 3-D structure of field lines in the expanding solar wind using an MHD code that allows the imposition of streams, a current sheet, flux tubes, microstreams, waves, and quasi-2-D turbulence. We find the natural development of closed field lines and lines with more complex geometry in the current sheet region. We show that microstreams cause an increased divergence of the field lines. The various initially strange looking heliospheric field lines we find have observational support in early work by K. Schatten and others, who found very similar structures using simple projection methods, as well in more recent work examining the nature of current sheet crossings. Our simulations exhibit most of the solar wind field configurations suggested by Schatten in his Solar Wind Two review.

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