Three-dimensional hydrodynamic models of solar granulation and their application to a spectral analysis problem

Details Three-dimensional hydrodynamic models of solar granulation and their application to a spectral analysis problem Three-dimensional hydrodynamic models of solar granulation and their application to a spectral analysis problem

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...291..635a&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 291, no. 2, p. 635-656

Astronomy and Astrophysics

Astrophysics

36

Hydrodynamic Equations, Iron, Mixing Length Flow Theory, Radiative Transfer, Solar Granulation, Spectrum Analysis, Three Dimensional Models, Abundance, Algorithms, Hydrodynamics, Solar Atmosphere, Stellar Composition, Temperature Distribution, Velocity Distribution

Scientific paper

The results of three-dimensional hydrodynamic simulations of solar granulation, obtained using two different algorithms are presented. Sequences of 3-D hydrodynamic, time-dependent models have been used to determine iron abundance in the solar photosphere. The results of iron abundance determination from the equivalent widths and central depths of 42 FeI and 32 Fe II lines are presented. The iron abundance has also been estimated from the line asymmetries and their absolute shifts. The conclusion was made that Fe II lines are the most suitable for iron abundance determination in the local thermodynamic equilibrium (LTE) approximation, since they are not very sensitive to the temperature structure of models and to NLTE effects. To clear up the influence of the inhomogeneous structure of 3-D models on spectral line calculations, computations on the basis of 1-D models were carried out. The results of hydrodynamic simulations of granulation on Procyon, using the numerical technique developed for modelling solar granulation, are presented in comparison with the ones obtained for the Sun. The inhomogeneous models of the photosphere of Procyon permitted us to reproduce line asymmetries, observed in the spectrum of Procyon, and to estimate the rotation velocity Ve sin i of this star as 3.5 km/s. The temperature structure of the 3-D models of Sun and Procyon was also approximated by the mixing length theory with variable alpha (i.e. it was supported that mixing length parameter alpha is varied with depth).

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