Hot subluminous stars of spectral type B and O are core helium-burning stars at the blue end
of the horizontal branch or have evolved even beyond that stage. Most hot subdwarf stars …

We show that the masses of red giant stars can be well predicted from their photospheric
carbon and nitrogen abundances, in conjunction with their spectroscopic stellar labels log g …

Common envelope evolution is the most important phase in the lives of many significant
classes of binary stars. During a common envelope phase, the stars temporarily share the …

Helium white dwarfs (HeWDs) are thought to form from low-mass red giant stars
experiencing binary interaction. Because the helium core mass of a red giant star is closely …

The formation mechanism for blue hook (BHk) stars in globular clusters (GCs) is still unclear.
Following one of the possible scenarios, called the late hot flash scenario, we propose that a …

Context. TZ Fornacis (TZ For) is an evolved detached binary system that is difficult to model
and interpret, but very useful for testing stellar evolution theory and physics. Aims. We aim to …

Employing tidally enhanced stellar wind, we studied in binaries the effects of metallicity,
mass ratio of primary to secondary, tidal enhancement efficiency and helium abundance on …

Context. The color and luminosity distribution of horizontal branch (HB) stars in globular
clusters (GCs) are sensitive probes of the original helium abundances of those clusters. In …

Tidally enhanced stellar wind may affect horizontal branch (HB) morphology in globular
clusters (GCs) by enhancing the mass loss of primary star during binary evolution. Lei et …