An optimization principle for computing stationary MHD equilibria with solar wind flow
Abstract
Knowledge about the magnetic field and plasma environment is importantfor almost all physical processes in the solar atmosphere. Precisemeasurements of the magnetic field vector are done routinely only inthe photosphere, e.g. by SDO/HMI. These measurements are used asboundary condition for modelling the solar chromosphere and corona,whereas some model assumptions have to be made. In the low-plasma-betacorona the Lorentz-force vanishes and the magnetic fieldis reconstructed with a nonlinear force-free model. In the mixed-betachromosphere plasma forces have to be taken into account with thehelp of a magnetostatic model. And finally for modelling the globalcorona far beyond the source surface the solar wind flow has tobe incorporated within a stationary MHD model.To do so, we generalize a nonlinear force-free and magneto-static optimizationcode by the inclusion of a field aligned compressible plasma flow.Applications are the implementation of the solar wind onglobal scale. This allows to reconstruct the coronal magnetic field furtheroutwards than with potential field, nonlinear force-free and magneto-static models.This way the model might help in future to provide the magnetic connectivityfor joint observations of remote sensing and in-situ instruments on SolarOrbiter and Parker Solar Probe.
- Publication:
-
EGU General Assembly Conference Abstracts
- Pub Date:
- May 2020
- DOI:
- 10.5194/egusphere-egu2020-3029
- Bibcode:
- 2020EGUGA..22.3029W