Affiliation
Kiepenheuer-Institut für Sonnenphysik, Freiburg & Istituto Ricerche Solari Locarno
Main category
Natural Sciences (Astrophysics and Astrononmy)
Abstract
From observations of the Sun, we know of the existence of a small-scale magnetism
in the form of photospheric magnetic flux concentrations of granular and sub-granular
scales. This small-scale magnetic structur has consequences for global quantities
such as the total solar irradiance or the convective blueshift. Here we have a look at
properties of the small-scale magnetism of cool stellar atmospheres, in particular at effects
on the radiative intensity and flux from the stellar surface. Lack of direct
observations, these properties are derived from three-dimensional radiation
magnetohydrodynamic simulations, which start with either, a homogeneous vertical
magnetic field, or, for comparison, without a magnetic field. The two settings are
thought to represent states of high and low small-scale magnetic activity corresponding
to maximum and minimum of a stellar magnetic cycle. Besides radiative, we also discuss
interesting magnetic properties of the stellar small-scale magnetism.
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