The mass loss rates of sdB stars

TL;DR

This paper investigates the theoretical existence of weak radiatively driven winds in subdwarf B stars, highlighting their dependence on stellar parameters and the potential for metal-only mass loss.

Contribution

It presents a theoretical analysis of weak wind existence in sdB stars, emphasizing multicomponent effects and metal-only ejection in certain stellar conditions.

Findings

Weak winds may exist only in the most luminous sdB stars.

Decoupling of metals from hydrogen and helium occurs in more compact sdB stars.

Metals can be expelled while hydrogen and helium remain in hydrostatic equilibrium.

Abstract

The effects of gravitational settling and radiative levitation in the stellar atmospheres and envelopes of subdwarf B (sdB) stars strongly depend on the presence of weak winds. In the paper the existence of weak radiatively driven winds is investigated from a theoretical point of view for sdB stars of half a solar mass, effective temperatures between 25000 K and 35000 K, and surface gravities log g between about 5.0 and 6.0 (cgs units). According to the results, weak winds with mass-loss rates of the order E-11 solar masses per year may exist only for the most luminous sdB stars. For the more compact ones, the decoupling of the metals from the bulk matter (hydrogen and helium) is expected in the wind region, because the momentum exchange via Coulomb collisions is not effective enough. Thus multicomponent effects are of great importance. We suggest that only the metals may be expelled from the star, whereas hydrogen and helium are in hydrostatic equilibrium.