A 3D Two-Temperature Solar Wind Model with Alfven Wave Heating

Computer Science – Performance

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Scientific paper

The Space Weather Modeling Framework (SWMF), developed at the University of Michigan, is a high performance simulation tool to model a wide variety physics domains ranging from solar corona and heliosphere to the magnetosphere, ionosphere and thermosphere of the Earth and can run these models in a coupled fashion.
We have developed a new physically consistent, three-dimensional solar wind model within the SWMF, that account for the different electron and ion temperatures. We use field-aligned heat conduction for both the electron and ions. The collisions between the electrons and ions are taken into account: Close to the sun the electrons and ions are tightly coupled, but completely decouple beyond approximately 1.5 solar radii. In our model, we use Alfven waves to accelerate the wind. The ions are heated by the Kolmogorov dissipation of the Alfven waves. The velocities at 1AU obtained from the semi-emperical Wang-Sheeley-Arge model in combination with conservation of total energy along the field lines determines the Alfven wave amplitude at the photospheric level. The density and temperature at the solar boundary are obtained from EUVI tomography. This new model is validated for Carrington rotation 2077 at 1AU. We compare this two-temperature model with a one-temperature model. Since we properly treat the thermodynamics in the new solar wind model, we expect great improvement for the modeling of coronal mass ejections (CMEs) and CME-driven shocks.

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