Relativistic evolution of 103M⊙ star

A. Kovetz; G. Shaviv

doi:10.1007/BF00653324

Relativistic evolution of 10³M_⊙ star

A. Kovetz^*
, G. Shaviv

^*Corresponding author for this work

University of Montreal
Tel Aviv University

Research output: Contribution to journal › Article › peer-review

3 Scopus citations

Abstract

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 language	English
Pages (from-to)	378-388
Number of pages	11
Journal	Astrophysics and Space Science
Volume	14
Issue number	2
DOIs	https://doi.org/10.1007/BF00653324
State	Published - Dec 1971
Externally published	Yes

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abstract = "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.",

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N2 - 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.

AB - 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.

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JO - Astrophysics and Space Science

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ER -

Relativistic evolution of 10³M_⊙ star

Abstract

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