Granulation in K-type dwarf stars - II. Hydrodynamic simulations and 3D spectrum synthesis

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Table 1:

Strong Fe I lines added to the line list of Ramírez et al. (2007) for the 3D calculation of synthetic line profiles.
Wavelength	$\log gf^{{a}}$	EP	$\sigma^{{b}}$	$\alpha^{{b}}$
(Å)		(eV)	(AU)
5741.85	-1.67	4.26	725	0.232
6252.56	-1.77	2.40	326	0.245
6335.32	-2.18	2.20	275	0.261
6411.65	-0.72	3.65	820	0.247
6430.85	-1.95	2.18	272	0.257
6677.99	-1.42	2.69	313	0.268

^a Transition probabilities are from the laboratory measurements of the Oxford group (e.g., Blackwell et al. 1976). ^b The last two columns are the van der Waals damping constants obtained by Barklem et al. (2000); $\sigma$ is the broadening cross section for an atom-perturber relative velocity v₀=10⁶ cm s^-1, given in atomic units ( $1~\mathrm{AU}=2.8\times10^{-17}~\mathrm{cm}^2$ ), and $\alpha$ the velocity parameter, which is related to the temperature dependence of the cross-section ( $\sigma\propto T^{(1-\alpha)/2}$ ).

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