Thermodynamic fluctuations in solar photospheric three-dimensional convection simulations and observations
Context. Numerical three-dimensional (3D) radiative (magneto-)hydrodynamical [(M)HD] simulations of solar convection are nowadays used to understand the physical properties of the solar photosphere and convective envelope, and, in particular, to determine the Sun's photospheric chemical abundances. To validate this approach, it is important to
Beck, C. et al.
Fecha de publicación:
9
2013