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Solar and stellar magnetohydrodynamics
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Solar and stellar magnetohydrodynamics

Theory group

SolarMHD Logo Magnetohydrodynamics (MHD) describes the dynamical interaction between flows and magnetic fields in a collisionally dominated plasma. The work of the MHD group at MPS is mainly concerned with MHD processes in the interior and atmosphere of the Sun and other stars. Using large-scale numerical simulations and analytical tools, this work aims at understanding the origin of solar and stellar magnetism as well as its rich variety of manifestations in the form of magnetic activity.

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Science objectives

Magnetic fields are responsible for the restless activity of the Sun and other stars. Magnetohydrodynamics (MHD) describes the interaction of a magnetic field with an electrically conducting dense plasma. The research areas of the MHD group at MPS include

  • interaction of magnetic fields with radiative convection near the solar surface
  • formation and dynamics of magnetic flux tubes in the solar convection zone
  • generation of magnetic flux in a self-excited dynamo process
  • stellar activity throughout the Hertzsprung-Russell diagram
  • development of methods and codes for the numerical simulation of (radiative) MHD processes
Our work is closely connected to solar and stellar observations.

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