- Conference date: 17-31 June 2002
- Location: Pisa (Italy)
We have developed a three‐dimensional magnetohydrodynamic (MHD) model of the solar corona and of the solar wind. We specify a magnetic flux distribution on the solar surface and integrate the time dependent MHD equations to steady state. The model originally employed a polytropic energy equation. In order to improve the physics in our algorithm, we have incorporated thermal conduction along the magnetic field, radiation losses, and heating into the energy equation. The 2D version of the model is able to reproduce the contrast in density between the open and closed magnetic structures in the corona and the fast and slow streams of the solar wind. We now present preliminary results of 3D MHD simulations with improved thermodynamics. The results can be tested against observations by spacecraft and Earth based observatories, in situ solar wind and magnetic field measurements, heliospheric current sheet crossings.
- Solar wind
- Magnetohydrodynamic equations
- Solar corona
- Wind energy
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