Fast and slow solar wind properties obtained from a thermally conductive MHD model of a coronal hole

Details Fast and slow solar wind properties obtained from a thermally conductive MHD model of a coronal hole Fast and slow solar wind properties obtained from a thermally conductive MHD model of a coronal hole

Jan 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997adspr..20...39s&link_type=abstract

Advances in Space Research, vol. 20, p. 39

Astronomy and Astrophysics

Astronomy

1

Solar Wind Velocity, Thermal Conductivity, Coronal Holes, Self Consistent Fields, Plasma Diagnostics, Astronomical Models, Polar Regions, Photosphere

Scientific paper

In the present self-consistent, thermally conductive MHD model of the solar wind from a polar coronal hole in a dipolar photospheric field, solar minimum conditions are approximated through alignment with the rotation axis. As the model essentially applies from the coronal temperature maximum to the Earth, an examination of the plasma parameters found in the solar corona by these means clarifies the coronal conditions implied by solar wind parameters at 1 AU. It is found that latitudinal gradients of velocity, density, and temperature appear close to the sun.

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