Granulation in K-type Dwarf Stars. II. Hydrodynamic simulations and 3D spectrum synthesis

Details Granulation in K-type Dwarf Stars. II. Hydrodynamic simulations and 3D spectrum synthesis Granulation in K-type Dwarf Stars. II. Hydrodynamic simulations and 3D spectrum synthesis

2009-05-19

arxiv.org/abs/0905.3101v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

A&A, in press

Scientific paper

We construct a 3D radiative-hydrodynamic model atmosphere of parameters Teff = 4820 K, log g = 4.5, and solar chemical composition. The theoretical line profiles computed with this model are asymmetric, with their bisectors having a characteristic C-shape and their core wavelengths shifted with respect to their laboratory values. The line bisectors span from about 10 to 250 m/s, depending on line strength, with the stronger features showing larger span. The corresponding core wavelength shifts range from about -200 m/s for the weak Fe I lines to almost +100 m/s in the strong Fe I features. Based on observational results for the Sun, we argue that there should be no core wavelength shift for Fe I lines of EW > 100 mA. The cores of the strongest lines show contributions from the uncertain top layers of the model, where non-LTE effects and the presence of the chromosphere, which are important in real stars, are not accounted for. The comparison of model predictions to observed Fe I line bisectors and core wavelength shifts for a reference star, HIP86400, shows excellent agreement, with the exception of the core wavelength shifts of the strongest features, for which we suspect inaccurate theoretical values. Since this limitation does not affect the predicted line equivalent widths significantly, we consider our 3D model validated for photospheric abundance work.

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