Physics – Plasma Physics
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmng21a..07o&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #NG21A-07
Physics
Plasma Physics
[4455] Nonlinear Geophysics / Nonlinear Waves, Shock Waves, Solitons, [7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7863] Space Plasma Physics / Turbulence, [7959] Space Weather / Models
Scientific paper
The mechanisms responsible for plasma heating in the solar corona and solar wind acceleration are still not well understood. Turbulent MHD waves have been suggested as a possible mechanism, which both heats the plasma via wave energy dissipation and accelerates it due to the wave pressure gradient force. In order to account for these processes, a self-consistent model of the solar corona and solar wind must include the wave transport equation. Coupling this equation to the 3D MHD equations allows the exchange of momentum and energy between the wave field and the background plasma. This coupled system of equations is solved in a recently developed computational model of MHD wave turbulence, implemented within the SWMF/BATSRUS. The model is based on a wave transport equation for low frequency Alfven waves derived in Sokolov et. al. (2009). In every spatial cell a frequency grid is constructed, allowing the detailed description of the wave energy spectral evolution, making the model effectively 4D. Recent Hinode observations of chromospheric Alfven waves have shown that their energy flux could constitute a sufficient energy source to drive the solar wind. In this work we examined the possible effects of Alfven wave turbulence by imposing a Kolmogorov - type spectrum as the inner boundary condition for the 4D solar corona model. We found that the solar wind can indeed be totally driven by the Alfven wave pressure. The 4D solar corona model is coupled to an MHD model of the inner heliosphere, which extends the simulation results to larger heliocentric distances. This allows us to compare our results to solar wind in situ data at 1AU.
Frazin Richard A.
Gombosi Tamas I.
Oran Rona
Roussev Ilia I.
Sokolov Iu. I.
No associations
LandOfFree
Turbulent Alfven Waves as a Solar Wind Driver: Results from a new 4D model for the Solar Corona and Solar Wind does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Turbulent Alfven Waves as a Solar Wind Driver: Results from a new 4D model for the Solar Corona and Solar Wind, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Turbulent Alfven Waves as a Solar Wind Driver: Results from a new 4D model for the Solar Corona and Solar Wind will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1777213