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arXiv · 1510.07870

The red giant branch phase transition: Implications for the RGB luminosity function bump and detections of Li-rich red clump stars

Santi Cassisi·Maurizio Salaris·Adriano Pietrinferni
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Abstract

We performed a detailed study of the evolution of the luminosity of He-ignition stage and of the red giant branch bump luminosity during the red giant branch phase transition for various metallicities. To this purpose we calculated a grid of stellar models that sample the mass range of the transition with a fine mass step equal to ${\rm 0.01M_\odot}$. We find that for a stellar population with a given initial chemical composition, there is a critical age (of 1.1-1.2~Gyr) around which a decrease in age of just 20-30 million years causes a drastic drop in the red giant branch tip brightness. We also find a narrow age range (a few $10^7$ yr) around the transition, characterized by the luminosity of the red giant branch bump being brighter than the luminosity of He ignition. We discuss a possible link between this occurrence and observations of Li-rich core He-burning stars.

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Santi Cassisi, Maurizio Salaris, Adriano Pietrinferni. 2015-10-27. The red giant branch phase transition: Implications for the RGB luminosity function bump and detections of Li-rich red clump stars. https://doi.org/10.1051/0004-6361%2F201527412

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