An Extensive Grid of Models Producing Extreme Horizontal Branch Stars

TL;DR

This study uses the STAREV code to produce a comprehensive grid of models for Extreme Horizontal Branch stars, exploring how metallicity, helium abundance, and mass loss influence their formation and properties.

Contribution

It provides the first extensive, self-consistent parameter study of EHB star formation across a wide range of metallicities and initial conditions, including He-enrichment effects.

Findings

He-enrichment alone does not produce EHB stars without increased mass loss.

The hottest HB stars result from combined He-enrichment and high mass loss.

EHB stars significantly contribute to UV flux in their host systems.

Abstract

Horizontal branch (HB) morphology is a complex multiple-parameter problem. Besides the metallicity, two other leading parameters are the mass loss rate (MLR) and the initial He abundance of the HB progenitors. Using the STAREV stellar evolution code, we produce a wide array of Extreme Horizontal Branch (EHB) stars and also examine their post-HB evolution. EHB stars are produced in our calculations by the so called `delayed (late) hot core flash' scenario. The MLR is increased on the red giant branch (RGB) to the extent that, prior to reaching core flash conditions, only a very thin H-rich envelope remains and helium ignition takes place at hotter positions on the HRD. We perform an extensive, self-consistent parameter study, covering populations I and II (Z=0.0001-0.03), for both normal initial helium abundances and He-enriched models (up to Y=0.40). For completeness of the study and in order to point to complete trends, we chose NOT to cut out several combinations (or results of) that may extend beyond realistic limits. We present results and complete evolutionary tracks for the covered parameter space, showing in particular that: a) Increased He abundance ON ITS OWN -- without having a significant-enough MLR on the RGB -- DOES NOT lead to the production of EHB stars; however, b) The bluest (hottest) HB positions do result from the COMBINED effect of He-enhancement and increased MLR; c) The general trend is that the effective temperature on the HB increases with decreasing metallicity, but there is an indication for a halt, or even a reversal of this trend, as Z further decreases below $10^{-3}$; d) EHB stars can serve as major contributors to the UV flux emanating from their host system. Thus, the present comprehensive study both complements and lends support to previous, more restricted studies of the HB phase, and adds results for unexplored regions of the parameter space.