Relativistic evolution of 103M star

A. Kovetz*, G. Shaviv

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review


A fully relativistic evolution of 103M is described for initial composition of Y=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 103M 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.

Original languageEnglish
Pages (from-to)378-388
Number of pages11
JournalAstrophysics and Space Science
Issue number2
StatePublished - Dec 1971
Externally publishedYes


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