Physics – Plasma Physics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh53a2026l&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #SH53A-2026
Physics
Plasma Physics
[7500] Solar Physics, Astrophysics, And Astronomy, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7859] Space Plasma Physics / Transport Processes, [7863] Space Plasma Physics / Turbulence
Scientific paper
Intrinsically multi-dimensional and involving the transition from the collision-dominated to the collisionless regime, the solar wind proves challenging to model. In this presentation we present a consistent numerical scheme that treats the two major ion species, namely protons and alpha particles, on an equal footing, and that readily incorporates such effects as wave/turbulence heating and field-aligned electron heat flux. The model uses as input the observation-based boundary conditions at the solar surface and produces as output the global distribution of fluid, magnetic field as well as wave/turbulence parameters out to the Earth orbit and beyond. Several representative results we will present are: 1) How well does the parallel cascade scenario work in shaping the proton temperature anisotropy? 2) What is the role of finite-wavelength (non-WKB) Alfven waves in coupling the two ion species? 3) What is the role of waves/turbulence in shaping the ion differential streaming? On the one hand, the available remote-sensing and in situ measurements provide critical constraints for solar wind heating/acceleration mechanisms. On the other hand, applying the forward modeling approach to the model outputs helps us make better use of the remote-sensing data, those made with SOHO/UVCS in particular.
Li Baowen
Li Xiaoliang
Rifai Habbal Shadia
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