stars have been calculated by using a stellar code described in Paper I by [@Bahena2010]. These models assume the standard quasistatic non-rotating configuration of the stars. A semiconvection treatment for convective transport of energy has been used. In addition to the assumptions on the underlying physics used in Paper I, we include now also a mass loss parametrization.

In view of the uncertainty in the dominant mass loss process in the Population III stars, the corresponding mass loss rates and their changes with the stellar parameters as summarized in the previous Section, we have adopted a simple parametrization of the mass loss rate, based on the first relations proposed by [@Lucy1970] and [@Barlow1977] to explain the mass loss for hot luminous stars,

$$\label{MLR}
 \dot{M}=N L/c^2\; ,$$

where $L$ is the luminosity of the star, $c$ is the speed of light, and $N$ is a mass loss parameter. This parameter is taken as an average measure of the mass loss rate and it is kept constant in the course of the whole evolution. It is based on the simplifying assumption that the mass-energy output of the star in the form of non-zero rest-mass particles is proportional to its radiative output.

Different 