Effects of Helium Enrichment in Globular Clusters I.Theoretical Plane with PGPUC stellar evolution code

TL;DR

This paper presents theoretical stellar evolution models incorporating helium enrichment to understand multiple populations in globular clusters, highlighting observable effects on color-magnitude diagrams and horizontal branch morphology.

Contribution

It introduces updated PGPUC stellar evolution tracks and isochrones with variable helium content across a range of metallicities, aiding indirect helium abundance determination.

Findings

Helium enrichment causes splits in the main sequence and subgiant branch.

Increased Y affects luminosity and temperature at key evolutionary stages.

Higher Y leads to brighter and more extended horizontal branch morphologies.

Abstract

Recently, the study of globular cluster (GC) CMDs has shown that some of them harbor multiple populations with different chemical compositions and/or ages. In the first case, the most common candidate is a spread in the initial helium abundance, but this quantity is difficult to determine spectroscopically due to the fact that helium absorption lines are not present in cooler stars, whereas for hotter GC stars gravitational settling of helium becomes important. As a consequence, indirect methods to determine the initial Y among populations are necessary. For that reason, in this series of papers, we investigate the effects of a Y enrichment in populations covering the range of GC metallicities. In this first paper, we present the theoretical evolutionary tracks, isochrones, and ZAHB loci calculated with the Princeton-Goddard-PUC (PGPUC) stellar evolutionary code, which has been updated with the most recent input physics and compared with other theoretical databases. The chemical composition grid covers 9 Z ranging from Z=1.60x10^-4 to 1.57x10^-2, 7 Y from Y=0.230 to 0.370, and an alpha-element enhancement of [alpha/Fe]=0.3. The effects of different helium abundances that can be observed in isochrones are: splits in the MS, differences in the L and Teff of the turn off point, splits in the SGB being more prominent for lower ages or higher metallicities, splits in the lower red giant branch being more prominent for higher ages or higher metallicities, differences in L of the RGB bump (with small changes in Teff), and differences in L at the RGB tip. At the ZAHB, when Y is increased there is an increase of L for low Teff, which is affected in different degrees depending on the age of the GC being studied. Finally, the ZAHB morphology distribution depending on the age explains how for higher GC metallicities a population with higher helium abundance could be hidden at the red ZAHB locus.