NSO Workshop #23, Solar MHD: Theory and Observations - a High Spatial Resolution Perspective, Sac Peak, USA, 2005

ASP Conf. Series 354, 301 (2006)

Sven Wedemeyer-Böhm (Kiepenheuer-Institut für Sonnenphysik, Schöneckstrasse 6, 79104 Freiburg, Germany)
Inga Kamp (Space Telescope Science Institute, 3700 San Martin Drive, Baltimore MD 21218, USA)
Jo Bruls (Kiepenheuer-Institut für Sonnenphysik, Schöneckstrasse 6, 79104 Freiburg, Germany)
Bernd Freytag (Department for Astronomy and Space Physics, Uppsala University, Box~515, 75120~Uppsala, Sweden)
Matthias Steffen (Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany)

A first three-dimensional model for the carbon monoxide concentration in the solar atmosphere


The time-dependent and self-consistent treatment of carbon monoxide (CO) has been added to the radiation chemo-hydrodynamics code CO5BOLD. It includes the solution of a chemical reaction network and the advection of the resulting particle densities with the hydrodynamic flow field. Here we present a first 3D simulation of the non-magnetic solar photosphere and low chromosphere, calculated with the upgraded code. In the resulting model, the highest amount of CO is located in the cool regions of the reversed granulation pattern in the middle photosphere. A large fraction of carbon is bound by CO throughout the chromosphere with exception of hot shock waves where the CO concentration is strongly reduced. The distribution of carbon monoxide is very inhomogeneous due to co-existing regions of hot and cool gas caused by the hydrodynamic flow. High-resolution observations of CO could thus provide important constraints for the thermal structure of the solar photosphere and chromosphere.


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