Incorporating Kinetic Effects into Global Models of the Solar Wind (Invited)

Details Incorporating Kinetic Effects into Global Models of the Solar Wind (Invited) Incorporating Kinetic Effects into Global Models of the Solar Wind (Invited)

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm33e..02c&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SM33E-02

Physics

Plasma Physics

[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7836] Space Plasma Physics / Mhd Waves And Instabilities, [7863] Space Plasma Physics / Turbulence

Scientific paper

The origins of the hot solar corona and the supersonically expanding solar wind are still the subject of much debate. Far from there being a shortage of ideas, there is in fact a surplus of proposed physical mechanisms, each of which requires testing by comparison with observations. This process is difficult not only because the empirical measurements are limited, but also because many of the proposed mechanisms act on a wide range of spatial scales (from centimeters to solar radii) with feedback effects that are not yet well understood. Many of these mechanisms are related to the dissipation of solar MHD waves, and many involve multiple steps of energy conversion between waves, turbulence, current sheets, and other nonlinear plasma features. This presentation will give a summary of wave/turbulence models that seem to succeed in explaining the time-steady properties of the corona and the existence of fast and slow solar wind streams. A new global model of nonlinear MHD wave transport and dissipation in polar coronal holes, which includes both compressible and incompressible fluctuations, will also be presented. The goal of this model is to predict the kinetic partitioning of heat deposition between electrons, protons, and heavy ions, with as few free parameters as possible.

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