First Stars. II. Evolution with mass loss

Abstract

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$M_{\odot }$ 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.

Accepted for publication in Astrophysics & Space Science. 15 pages, 18 figures

References in corpus (9)

• Mass loss from hot massive stars
• Dynamical Simulations of Magnetically Channeled Line-Driven Stellar Winds: II. The Effects of Field-Aligned Rotation
• Mass loss from late-type WN stars and its Z-dependence: very massive stars approaching the Eddington limit
• Wind modelling of very massive stars up to 300 solar masses
• Rotation Speed of the First Stars
• Mass and angular momentum loss via decretion disks
• Numerical simulations of continuum-driven winds of super-Eddington stars
• CNO driven winds of hot first stars
• Continuum driven winds from super-Eddington stars. A tale of two limits

Cited by in corpus (1)

• A model for microquasars of Population III