Grids of stellar models including second harmonic and colours: Solar composition

TL;DR

This paper presents comprehensive grids of stellar evolution models with updated solar abundances, including effects of rotation and second harmonic, useful for various astrophysical applications and validated against observational data.

Contribution

It introduces a new grid of stellar models with updated ingredients, detailed second harmonic calculations, and rotation effects, facilitating improved analysis of diverse stellar phenomena.

Findings

Models match observational data for Sun, Hyades, and Am stars.

Second harmonic values are provided for eclipsing binary analysis.

Rotation effects are quantified and incorporated into stellar models.

Abstract

Grids of stellar evolution are required in many fields of astronomy/astrophysics, such as planet hosting stars, binaries, clusters, chemically peculiar stars, etc. In this study, a grid of stellar evolution models with updated ingredients and {recently determined solar abundaces} is presented. The solar values for the initial abundances of hydrogen, heavy elements and mixing-length parameter are 0.0172, 0.7024 and 1.98, respectively. The mass step is small enough (0.01 M$_\odot$) that interpolation for a given star mass is not required. The range of stellar mass is 0.74 to 10.00 M$_\odot$. We present results in different forms of tables for easy and general application. The second stellar harmonic, required for analysis of apsidal motion of eclipsing binaries, is also listed. We also construct rotating models to determine effect of rotation on stellar structure and derive fitting formula for luminosity, radius and the second stellar harmonic as a function of rotational parameter. We also compute and list colours and bolometric corrections of models required for transformation between theoretical and observational results. The results are tested for the Sun, the Hyades cluster, the slowly rotating chemically peculiar Am stars and the eclipsing binaries with apsidal motion. The theoretical and observational results along isochrones are in good agreement. The grids are also applicable to rotating stars provided that equatorial velocity is given.