The Effect of Proton Temperature Anisotropy on the Solar Minimum Corona and Wind

Details The Effect of Proton Temperature Anisotropy on the Solar Minimum Corona and Wind The Effect of Proton Temperature Anisotropy on the Solar Minimum Corona and Wind

2003-10-29

arxiv.org/abs/astro-ph/0310846v1

Astrophys.J. 598 (2003) 1361-1374

Astronomy and Astrophysics

Astrophysics

36 pages, 13 figures. AAS LaTeX Macros v5.0. To appear in The Astrophysical Journal, Vol. 598, No. 2, Issue December 1, 2003

Scientific paper

10.1086/379008

A semi-empirical, axisymmetric model of the solar minimum corona is developed by solving the equations for conservation of mass and momentum with prescribed anisotropic temperature distributions. In the high-latitude regions, the proton temperature anisotropy is strong and the associated mirror force plays an important role in driving the fast solar wind; the critical point where the outflow velocity equals the parallel sound speed is reached already at 1.5 Rsun from Sun center. The slow wind arises from a region with open field lines and weak anisotropy surrounding the equatorial streamer belt. The model parameters were chosen to reproduce the observed latitudinal extent of the equatorial streamer in the corona and at large distance from the Sun. We find that the magnetic cusp of the closed-field streamer core lies at about 1.95 Rsun. The transition from fast to slow wind is due to a decrease in temperature anisotropy combined with the non-monotonic behavior of the non-radial expansion factor in flow tubes that pass near the streamer cusp. In the slow wind, the plasma beta is of order unity and the critical point lies at about 5 Rsun, well beyond the magnetic cusp. The predicted outflow velocities are consistent with OVI Doppler dimming measurements from UVCS/SOHO. We also find good agreement with polarized brightness (pB) measurements from LASCO/SOHO and HI Ly-alpha images from UVCS/SOHO.

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