2008/09/30 by A. Kovetz, Attay Kovetz, O. Yaron +2 · 35 citations
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Biology #Code (set theory) #Computer science #Context (archaeology) #Gamma-ray bursts and supernovae #Physics #Programming language #Range (aeronautics) #Set (abstract data type) #Star (game theory) #Stars #Stellar evolution #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2009.14670.x
published in Monthly Notices of the Royal Astronomical Society 395(4), 1857-1874 (Oxford University Press) · MNRAS, in press; several sections and figures revised
arxiv created 2009/03/05 · openalex publication_date 2009/04/30 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present a new stellar evolution code and a set of results, demonstrating its capability at calculating full evolutionary tracks for a wide range of masses and metallicities. The code is fast and efficient, and is capable of following through all evolutionary phases, without interruption or human intervention. It is meant to be used also in the context of modelling the evolution of dense stellar systems, for performing live calculations for both normal star models and merger products. 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 1 M⊙ model for a wide range of metallicities; a series of models of stellar Populations I and II, for the mass range 0.25 to 64 M⊙, 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.