Free Access
Volume 502, Number 2, August I 2009
Page(s) L1 - L4
Section Letters
Published online 02 July 2009

Online Material

Appendix A: Graphical representation of the 3D temperature correction, ${\Delta }$T, the quality of the fit, QF, and the sensitivity of the fit, ${\sigma _{{T}_{eff}}}$

\end{figure} Figure A.1:

The temperature differences (3D - 1D) using 1D models with $\alpha $ = 0.5, $\alpha $ = 1.0 and $\alpha $ = 2.0, for H$\alpha $, H$\beta $, and H$\gamma $ for all of the six models considered. The uncertainties related to each temperature difference measurement are displayed as boxes. The value of the uncertainty on the x-axis corresponds to the associated $\sigma _{T_{\rm eff}}$ (sensitivity) values, while the uncertainty on the y-axis corresponds to the associated QF (quality of fit) values. See Table 2 and the text for details.

Appendix B: 3D-1D temperature correction and the lithium abundance in metal-poor F-type dwarfs

\end{figure} Figure B.1:

3D-1D abundance correction versus effective temperature difference for the test case of a metal-poor F-type dwarf. For details see text.

Here we present an example where it is advantageous to use a 1D model corrected for the 3D-1D temperature difference when deriving the chemical abundance from spectral line analysis: the abundance of lithium in a metal-poor F-type dwarf obtained from the 670.7 nm resonance line. We performed a 3D-NLTE spectrum synthesis calculation for the line on the 3D model with \ensuremath{T_{\rm eff}} = 6280 K, \ensuremath{\log g} = 4.0, [M/H] = -2.0 (cf. Table 1). We considered the resulting spectrum as representing an observation. Unlike a real observation, however, the underlying lithium abundance and stellar parameters are exactly known. According to Table 3 the temperature correction from H$\alpha $ fitting amounts to 74 K in this case, i.e. the 1D model that fits the 3D H$\alpha $ profile best is 74 K cooler than the 3D model. We then calculated for a series of thirteen 1D (LHD) models of different effective temperatures 1D lithium line profiles in LTE and NLTE. In the 1D spectrum synthesis, we assumed a microturbulence velocity of 1 km s-1; however, the actual value is not important since the line was chosen to be very weak. We derived for each model the lithium abundance matching the line strength obtained in 3D. Figure B.1 depicts the resulting abundance differences between the underlying lithium abundance assumed in the 3D model and the derived 1D abundance, versus the effective temperature differences between 1D models and the 3D model. As evident from the plot, one reduces the abundance error resulting from the erroneous effective temperature of the 1D model when applying the 3D-1D temperature correction. This holds irrespective of whether the 1D abundance analysis is performed in LTE or NLTE. Not surprisingly, the figure also shows that the correction of the effective temperature does not result in a perfect match of the lithium abundances in a 1D analysis.

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