First stars. II. Evolution with mass loss

The first stars are assumed to be predominantly massive. Although, due to the low initial abundances of heavy elements the line-driven stellar winds are supposed to be inefficient in the first stars, these stars may loose a significant amount of their initial mass by other mechanisms. In this work,...

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Bibliographic Details
Published in:Astrophysics and space science 2012-02, Vol.337 (2), p.651-663
Main Authors: Bahena, D., Hadrava, P.
Format: Article
Language:English
Subjects:
Astrobiology
Astronomy
Astrophysics
Astrophysics and Astroparticles
Cosmology
Evolution
Heavy elements
Metallicity
Observations and Techniques
Original Article
Phases
Physics
Physics and Astronomy
Population III stars
Space Exploration and Astronautics
Space Sciences (including Extraterrestrial Physics
Stars
Stars & galaxies
Stellar evolution
Universe
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Summary:The first stars are assumed to be predominantly massive. Although, due to the low initial abundances of heavy elements the line-driven stellar winds are supposed to be inefficient in the first stars, these stars may loose a significant amount of their initial mass by other mechanisms. In this work, we study the evolution with a prescribed mass loss rate of very massive, galactic and pregalactic, Population III stars, with initial metallicities Z =10 −6 and Z =10 −9 , respectively, and initial masses 100, 120, 150, 200, and 250 M ⊙ during the hydrogen and helium burning phases. The evolution of these stars depends on their initial mass, metallicity and the mass loss rate. Low metallicity stars are hotter, compact and luminous, and they are shifted to the blue upper part in the Hertzprung-Russell diagram. With mass loss these stars provide an efficient mixing of nucleosynthetic products, and depending on the He-core mass their final fate could be either pair-instability supernovae or energetic hypernovae. These stars contributed to the reionization of the universe and its enrichment with heavy elements, which influences the subsequent star formation properties.
ISSN:0004-640X
1572-946X
DOI:10.1007/s10509-011-0898-0