Physics
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh42b..02s&link_type=abstract
American Geophysical Union, Fall Meeting 2001, abstract #SH42B-02
Physics
2164 Solar Wind Plasma, 2169 Sources Of The Solar Wind, 7509 Corona, 7524 Magnetic Fields
Scientific paper
Recent observations suggest that the lower Solar corona is composed of a hierarchy of coronal loops and that the coronal magnetic field is entirely reconfigured on timescales of order 1.5 days. It is likely then that open flux, rooted at the Sun and extending through the heliosphere, reconnects continually with the medium of coronal loops. The reconnection process itself releases Poynting flux into the corona. Fisk Schwadron and Zurbuchen, 1999, argued that the release of Poynting flux due to flux emergence releases sufficient energy to drive the fast solar wind. In this talk, a theory is presented which relates the speed and mass flux of fast and slow solar wind to loop properties (e.g., height and mean temperature). A 1D, two-fluid, time-dependent MHD model is formulated that includes resistive ohmic heating and MHD wave-energy. The model is utilized to calculate the solar wind profiles of density, flux, proton/electron temperatures and wave energy consistent with the release of Poynting flux after reconnection with coronal loops. Based on the electron temperature profiles, charge states of carbon and oxygen are modeled and compared with observations in fast and slow wind. Charge-state observations may then be used with the aid of the model to test the theory, constrain possible wave-energy dissipation profiles, and wave modes responsible for converting Poynting flux into heating and momentum transfer.
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