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Titolo:
Influence of the C-12(alpha,gamma)O-16 reaction rate on the evolution of a15 M-circle dot star
Autore:
Imbriani, G; Straniero, O; Terrasi, F; Limongi, M; Chieffi, A;
Indirizzi:
Univ Naples Federico II, Dipartimento Sci Fis, I-80126 Naples, Italy Univ Naples Federico II Naples Italy I-80126 Fis, I-80126 Naples, Italy Ist Nazl Fis Nucl, I-80125 Naples, Italy Ist Nazl Fis Nucl Naples Italy I-80125 l Fis Nucl, I-80125 Naples, Italy Osservatorio Astron Capodimonte, I-80131 Naples, Italy Osservatorio AstronCapodimonte Naples Italy I-80131 80131 Naples, Italy Univ Naples 2, Dipartimento Sci Ambientali, Caserta, ITA-81100 Caserta, Italy Univ Naples 2 Caserta Italy ITA-81100 Caserta, ITA-81100 Caserta, Italy Osservatorio Astron Collurania, Teramo, Italy Osservatorio Astron Collurania Teramo Italy n Collurania, Teramo, Italy Osservatorio Astron Roma, I-00136 Rome, Italy Osservatorio Astron Roma Rome Italy I-00136 on Roma, I-00136 Rome, Italy CNR, Ist Astrofis Spaziale, Rome, Italy CNR Rome ItalyCNR, Ist Astrofis Spaziale, Rome, Italy
Titolo Testata:
NUCLEAR PHYSICS A
fascicolo: 1-2, volume: 688, anno: 2001,
pagine: 249C - 253C
SICI:
0375-9474(20010521)688:1-2<249C:IOTCRR>2.0.ZU;2-N
Fonte:
ISI
Lingua:
ENG
Soggetto:
THERMONUCLEAR REACTION-RATES; CROSS-SECTION; STELLAR ENERGIES; MASSIVE STARS;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
19
Recensione:
Indirizzi per estratti:
Indirizzo: Imbriani, G Univ Naples Federico II, Dipartimento Sci Fis, I-80126 Naples,Italy Univ Naples Federico II Naples Italy I-80126 6 Naples, Italy
Citazione:
G. Imbriani et al., "Influence of the C-12(alpha,gamma)O-16 reaction rate on the evolution of a15 M-circle dot star", NUCL PHYS A, 688(1-2), 2001, pp. 249C-253C

Abstract

In this paper we present the evolution of various 15M(circle dot) stellar models of solar and subsolar chemical composition, calculated using different values for the C-12(alpha, gamma)O-16 reaction rate. This process influences the evolution of a star because it directly operates during the heliumburning and it determines the final abundances of (12)G and O-16 left by this burning. Since this reaction works in a convective environment an analysis of its influence on the evolution of a star cannot be disentangled by the behavior of the convective core. Indeed the final C-12 and O-16 abundances largely depend on a delicate balance between the efficiency of this rateand the treatment of the convective core. We will show some tests which indicate quantitavely this interplay.

ASDD Area Sistemi Dipartimentali e Documentali, Università di Bologna, Catalogo delle riviste ed altri periodici
Documento generato il 04/12/20 alle ore 13:25:46