Simulations of the solar atmosphere and solar limbs

Details Simulations of the solar atmosphere and solar limbs Simulations of the solar atmosphere and solar limbs

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011sf2a.conf..407p&link_type=abstract

SF2A-2011: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics Eds.: G. Alecian, K. Belkacem,

Astronomy and Astrophysics

Astrophysics

Solar Atmosphere, Magnetic Activity, Simulation, Limb Darkening.

Scientific paper

We perform simulations of the solar atmosphere either using the 1D hydrostatic code Atlas12 or the 3D (magneto)hydrodynamic code Stagger. The former numerical tool relies on a phenomenology of convection whereas the later one addresses the surface convection directly and accounts for its dynamical effects. Once the average atmosphere stratification is obtained it is used to perform radiative transfer at speficic wavelengths in order to compute the solar limb darkening. We report a ≈ 60 mas shift between inflection point positions of limb profiles computed from 1D and 3D models. This is due to turbulent support present in 3D simulations but not 1D. We further report a slight decrease of the turbulent support when a moderate magnetic field is included in the simulation which suggests that the solar radius should be anti-correlated with the solar activity cycle.

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