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Titolo:
The evolution of a 25 M-circle dot star from the main sequence up to the onset of the iron core collapse
Autore:
Chieffi, A; Limongi, M; Straniero, O;
Indirizzi:
CNR, Ist Astrofis Spaziale, I-00044 Frascati, Italy CNR Frascati Italy I-00044 st Astrofis Spaziale, I-00044 Frascati, Italy Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy Osservatorio Astron Roma Monte Porzio Catone Italy I-00040 Catone, Italy Osservatorio Astron Collurania, I-64100 Teramo, Italy Osservatorio Astron Collurania Teramo Italy I-64100 -64100 Teramo, Italy
Titolo Testata:
ASTROPHYSICAL JOURNAL
fascicolo: 2, volume: 502, anno: 1998,
parte:, 1
pagine: 737 - 762
SICI:
0004-637X(19980801)502:2<737:TEOA2M>2.0.ZU;2-V
Fonte:
ISI
Lingua:
ENG
Soggetto:
THERMONUCLEAR REACTION-RATES; HORIZONTAL-BRANCH STARS; WEAK-INTERACTION RATES; POPULATION-I STARS; MASSIVE STARS; STELLAR MODELS; PRESUPERNOVA EVOLUTION; RADIATIVE OPACITIES; 120 M(CIRCLE-DOT); MAGELLANIC CLOUD;
Keywords:
nuclear reactions, nucleosynthesis, abundances; stars : evolution; stars : interiors; supernovae : general;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
87
Recensione:
Indirizzi per estratti:
Indirizzo: Chieffi, A CNR, Ist Astrofis Spaziale, CP 67, I-00044 Frascati, Italy CNR CP 67 Frascati Italy I-00044 P 67, I-00044 Frascati, Italy
Citazione:
A. Chieffi et al., "The evolution of a 25 M-circle dot star from the main sequence up to the onset of the iron core collapse", ASTROPHYS J, 502(2), 1998, pp. 737-762

Abstract

We present the evolution of a 25 M. star model having solar chemical composition from the premain-sequence phase up to the onset of the iron core collapse. This evolution has been obtained with the latest version (release 4.0) of our hydrostatic evolutionary code FRANEC, and hence it is totally homogeneous with all of our stellar evolutions concerning low and intermediate-mass stars. A network including 149 nuclear species has been fully coupledto the equations describing the temporal variations of the physical quantities. No quasi-nuclear statistical equilibrium approximation has been adopted up to 4 x 10(9) K. All of the evolutionary properties of the stellar model are discussed in detail. Whenever possible, comparisons with similar evolutions available in the literature have been performed. An iron core mass smaller than the values recently quoted in the literature for the same massand solar chemical composition has been obtained (M-Fe = 1.513 M.).

ASDD Area Sistemi Dipartimentali e Documentali, Università di Bologna, Catalogo delle riviste ed altri periodici
Documento generato il 04/12/20 alle ore 12:32:57