Stuttgart 2012 – scientific programme

Parts | Days | Selection | Search | Updates | Downloads | Help

EP: Fachverband Extraterrestrische Physik

EP 19: Sonne und Heliosphäre II

EP 19.6: Talk

Friday, March 16, 2012, 12:00–12:15, V55.21

MHD simulation of the inner-heliospheric magnetic field — •Tobias Wiengarten — Institut für Theoretische Physik IV, Ruhr-Universität Bochum

Maps of the radial magnetic field at a heliocentric distance of ten solar radii are used as boundary conditions in the MHD code CRONOS to simulate a 3D inner-heliospheric solar wind emanating from the rotating Sun. The input data for the magnetic field are the result of solar surface flux transport modelling (Jiang et al.(2010)) using observational data of sunspot groups coupled with a current–sheet source surface model. Amongst several advancements, this allows for higher angular resolution than that of comparable observational data from synoptic magnetograms. The required initial conditions for the other MHD quantities are obtained following the empirical approach by Detman et al.(2006), who use an inverse relation between flux tube expansion and radial solar wind speed. The computations are performed for representative solar minimum and maximum conditions, and results at the Earth’s orbit are obtained. After a successful comparison of the latter with observational data, they can be used to drive outer-heliospheric models.