The Evolutionary History of a 25 Msolar Star

Details The Evolutionary History of a 25 Msolar Star The Evolutionary History of a 25 Msolar Star

Feb 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997nupha.621..453l&link_type=abstract

Nuclear Physics A, v. 621, p. 453-456.

Physics

Nuclear Physics

1

Scientific paper

We present the first test evolution of a massive star (25 Msolar) having a solar chemical composition, from the main sequence phase up to the onset of the iron core collapse. This evolution has been obtained by means of the latest version (release 8.2) of our hydrostatic evolutionary code, FRANEC (Frascati RAphson Newton Evolutionary Code). The main properties of this updated version of our CODE are: a) the full set of the chemical and physical equations governing the evolution of the star model are fully coupled and integrated without any kind of approximation of (quasi or full) nuclear statistical equilibrium up to 4 billions degrees (only above this temperature we shift to an NSE-network) and without the use of a tabulated coefficient of nuclear energy generation, b) time dependent convection is allowed by adopting a technique firstly introduced by Sparks and Endal, c) the detailed behavior of each nuclear species in a convective layer (i.e. the balance between local burning and mixing) is obtained by a very simple but also effective method developped by us.

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