All Tables

Table 1: The predicted line strengths in pm (=10 mÅ) for the OH A-X and Be lines using 1D MARCS and Holweger-Müller solar model atmospheres calculated with different combinations of microturbulence ( $\xi _{\rm turb}$ ) and additional continuous opacity over standard values ( $\Delta \kappa _\nu ^{\rm cont}/\kappa _\nu ^{\rm cont}$ ). The "observed" equivalent widths used for the 3D calculations are those computed using $\Delta \kappa _\nu ^{\rm cont}/\kappa _\nu ^{\rm cont} = 0.60$ (i.e. 60% extra opacity) and $\xi _{\rm turb}=1.0$ , as found by Balachandran & Bell (1998).
Table 2: The predicted line strengths in pm for the OH A-X and Be lines using a 3D hydrodynamical solar model atmosphere. The OH lines are computed for log $~\epsilon_{\rm O}=8.66$ and the Be line for log $~\epsilon_{\rm Be}=1.38$ .