منابع مشابه
First Stars . I . Evolution without mass loss
The first generation of stars was formed from primordial gas. Numerical simulations suggest that the first stars were predominantly very massive, with typical masses M ≥ 100M⊙. These stars were responsible for the reionization of the universe, the initial enrichment of the intergalactic medium with heavy elements, and other cosmological consequences. In this work, we study the structure of Zero...
متن کاملCarbon Stars
In this review we rst describe basic information for carbon stars starting with the most recent spectral classi cation system of P.C. Keenan and luminosities derived from data in the Hipparcos Catalogue. For the SRb and Lb variables MK = 6:8 1:2 (21 stars). Only two R stars (non-variables) have measured K magnitudes and showMK = 5:2. The four N stars show MV = +0:76 1:06. Using the Magellanic C...
متن کاملPresupernova Evolution of Rotating Massive Stars I: Numerical Method and Evolution of the Internal Stellar Structure
The evolution of rotating stars with zero-age main sequence (ZAMS) masses in the range 8M⊙ to 25M⊙ is followed through all stages of stable evolution. The initial angular momentum is chosen such that the star’s equatorial rotational velocity on the ZAMS ranges from zero to ∼ 70% of break-up. The stars rotate rigidly on the ZAMS as a consequence of angular momentum redistribution during the pre-...
متن کاملEvolution of Protoneutron Stars
We study the thermal and chemical evolution during the Kelvin-Helmholtz phase of the birth of a neutron star, employing neutrino opacities that are consistently calculated with the underlying equation of state (EOS). Expressions for the diffusion coefficients appropriate for general relativistic neutrino transport in the equilibrium diffusion approximation are derived. The diffusion coefficient...
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ژورنال
عنوان ژورنال: Progress of Theoretical Physics
سال: 1968
ISSN: 0033-068X
DOI: 10.1143/ptp.39.619