Implementation of New OPAL Tables in Eggleton's Stellar Evolution Code

Abstract

Based on the work of OPAL (Iglesias & Rogers 1996) and Alexander & Ferguson (1994), we construct a series of opacity tables for various metallicities Z=0, 0.00001, 0.00003, 0.0001, 0.0003, 0.001, 0.004, 0.01, 0.02, 0.03, 0.04, 0.05, 0.06, 0.08 and 0.1. These tables can be easily used in Eggleton's stellar evolution code in place of the old tables without changing the code. The OPAL tables are used for ${\log }_{10}(T/\mathrm{K})>3.95$ and Alexander's for ${\log }_{10}(T/\mathrm{K})<3.95$. At ${\log }_{10}(T/\mathrm{K})=3.95$, the two groups' data fit well for all hydrogen mass fractions. Conductive opacities are included by reciprocal addition according to the formulae of Yakovlev & Urpin (1980). For different metallicities $1M_{\odot }$ models are constructed with the new opacity tables. Comparison of 1 and $5M\odot$ models constructed with the older OPAL tables (Iglesias & Rogers 1992) shows that the new opacities have most effect in the late stages of evolution, the extension of the blue loop during helium burning for intermediate-mass and massive stars.

8 pages, 5 figures

References in corpus (2)

• Approximate input physics for stellar modelling
• A more detailed look at the Opacities for Enriched Carbon and Oxygen Mixtures

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