CO Spectral Line Formation in the Sun: Convective Simulation, Line Profiles and Isotopic Abundance Measures
CO spectral line formation in the Sun was modelled using realistic, ab initio, timedependent 3D radiative-hydrodynamical model atmospheres. Three `phases' of 3D model atmospheres were utilised. In Phase 1, strong CO lines formed in very high atmospheric layers were modelled using the established model (Asplund et al. 2000b). This produced less than perfect agreement with observed line asymmetries measured in the ATMOS disc-centre solar atlas. The velocity, temperature and density fields were...[Show more]
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