Abstract
A fully relativistic evolution of 103 M ⊙ is described for initial composition ofY=Z=0. Our results show that (a) a great part of the star is in radiative equilibrium, (b) the maximal red-shift for main-sequence 103 M ⊙ stars is significantly less than for isentropic models, and (c) a very low amount of CNO elements (<10−8 by mass) is formed at any stage before hydrogen is completely consumed and hence such stars cannot be the progenitors of Population II stars.
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