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Solar and stellar magnetohydrodynamics
Theory group
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.
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
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interaction of magnetic fields with radiative convection near
the solar surface
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formation and dynamics of magnetic flux tubes in the solar convection zone
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generation of magnetic flux in a self-excited dynamo process
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stellar activity throughout the Hertzsprung-Russell diagram
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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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