A model for the population of helium stars in the Galaxy: Low-mass stars

Abstract

We model the Galactic ensemble of helium stars using population synthesis techniques, assuming that all helium stars are formed in binaries. In this picture, single helium stars are produced by mergers of helium remnants of the components of close binaries (mainly, the merging of helium white dwarfs) or in the disruption of binaries with helium components during supernova explosions. The estimated total birthrate of helium stars in the Galaxy is 0.043 yr−1; the total number is 4 × 106; and the binarity rate is 76%. We construct a subsample of low-mass (M He ≲ 2M ⊙) helium stars defined by observational selection effects: the limiting magnitude (V He ≤ 16), ratio of the magnitudes of the components in binaries (V He ≤ V comp), and lower limit for the semiamplitude of the radial velocity required for detecting binarity (K min = 30 km s−1). The parameters of this subsample are in satisfactory agreement with observations of helium subdwarfs. In particular, the binarity rate in the selection-limited sample is 58%. We analyze the relations between the orbital periods and masses of helium subdwarfs and their companions in systems with various combinations of components. We predict that the overwhelming majority (∼97%) of unobserved companions to helium stars will be white dwarfs, predominantly, carbon-oxygen white dwarfs.