burning.[]{data-label="bar_fig16"}](figure16.eps){width="82mm"}

$$

  -----------------------------------------------------------------------------------------------------------------------
      $Z$       log $T_{\rm c}$   log $\rho_{\rm c}$   log $\displaystyle{\frac{L}{L_{\odot}}}$   log $T_{\rm   log $R$
                                                                                                     eff}$     
  ------------ ----------------- -------------------- ------------------------------------------ ------------- ----------
   10$^{-6}$        7.84650            0.87274                         6.08715                      4.84250     11.72763

   10$^{-7}$        7.92150            1.09791                         6.09132                      4.88074     11.65323

   10$^{-8}$        8.00027            1.33451                         6.09652                      4.92088     11.57558

   10$^{-9}$        8.08323            1.58381                         6.10314                      4.96315     11.49433

   10$^{-10}$       8.17087            1.84730                         6.11174                      5.00775     11.40942
  -----------------------------------------------------------------------------------------------------------------------

  : Some characteristics of lower-metallicity $100\,M_{\odot}$ stars when settle down on the main-sequence. Models become more hotter, denser, luminous and compact, as metallicity is decreasing.\[tbl-1\]

$$

As a result of their high mass and temperature, very massive stars are dominated by radiation pressure and they have luminosities closer to the Eddington limit. The specific luminosity $L_{\nu}\sim
L_{\rm Edd}\sim M$, and the total luminosity depends on the total mass of stars only but it is independent of the IMF [@Bromm2001], which is a unique characteristic of very massive stars.

Mass loss can affect the stellar evolution in a variety of ways. In the present work, nuclear lifetimes for mass losing stars with a mass loss parameter $N=50$ are similar to those in the conservative case.

Hydrogen and helium burning lifetimes are decreasing with increasing stellar mass. On the other hand, the nuclear lifetimes are increasing with increasing 