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2009MNRAS.395.1857K - Mon. Not. R. Astron. Soc., 395, 1857-1874 (2009/June-1)
A new, efficient stellar evolution code for calculating complete evolutionary tracks.
KOVETZ A., YARON O. and PRIALNIK D.
Abstract (from CDS):
The code is based on a fully implicit, adaptive-grid numerical scheme that solves simultaneously for structure, mesh and chemical composition. Full details are given for the treatment of convection, equation of state, opacity, nuclear reactions and mass loss.
Results of evolutionary calculations are shown for a solar model that matches the characteristics of the present sun to an accuracy of better than 1 per cent; a 1M☉ model for a wide range of metallicities; a series of models of stellar Populations I and II, for the mass range 0.25 to 64M☉, followed from pre-main-sequence to a cool white dwarf or core collapse. An initial-final mass relationship is derived and compared with previous studies. Finally, we briefly address the evolution of non-canonical configurations, merger products of low-mass main-sequence parents.
Abstract Copyright: © 2009 The Authors. Journal compilation © 2009 RAS
Journal keyword(s): methods: numerical - stars: evolution - stars: general - Hertzsprung-Russell (HR) diagram - stars: interiors
Simbad objects: 5
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