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Titolo:
Intermediate-mass stars: Updated models
Autore:
Dominguez, I; Chieffi, A; Limongi, M; Straniero, O;
Indirizzi:
Univ Granada, Granada, Spain Univ Granada Granada SpainUniv Granada, Granada, Spain 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: 1, volume: 524, anno: 1999,
parte:, 1
pagine: 226 - 241
SICI:
0004-637X(19991010)524:1<226:ISUM>2.0.ZU;2-U
Fonte:
ISI
Lingua:
ENG
Soggetto:
ASYMPTOTIC GIANT BRANCH; THERMONUCLEAR REACTION-RATES; OLD OPEN CLUSTERS; STELLAR MODELS; CONVECTIVE CORES; EVOLUTIONARY SEQUENCES; RADIATIVE OPACITIES; GLOBULAR-CLUSTERS; MAIN-SEQUENCE; DREDGE-UP;
Keywords:
open clusters and associations : general; stars : evolution; stars : interiors;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
80
Recensione:
Indirizzi per estratti:
Indirizzo: Dominguez, I Univ Granada, Granada, Spain Univ Granada Granada SpainUniv Granada, Granada, Spain
Citazione:
I. Dominguez et al., "Intermediate-mass stars: Updated models", ASTROPHYS J, 524(1), 1999, pp. 226-241

Abstract

A new set of stellar models in the mass range 1.2-9 M. is presented. The adopted chemical compositions cover the typical Galactic values,namely, 0.0001 less than or equal to Z less than or equal to 0.02 and 0.23 less than orequal to Y less than or equal to 0.28. A comparison of the most recent compilations of similar stellar models is also discussed. The main conclusion is that the differences among the various evolutionary results are still rather large. For example, we found that the H-burning evolutionary time may differ up to 20%. An even larger disagreement is found for the He-burning phase (up to 40%-50%). Since the connection between the various input physics and the numerical algorithms could amplify or counterbalance the effect of a single ingredient on the resulting stellar model, the origin of these discrepancies is not evident. However most of these discrepancies, which areclearly found in the evolutionary tracks, are reduced on the isochrones. By means of our updated models we show that the ages inferred by the theory of stellar evolution is in excellent agreement with those obtained by usingother independent methods applied to the nearby open clusters. Finally, the theoretical initial/final mass relation is revised.

ASDD Area Sistemi Dipartimentali e Documentali, Università di Bologna, Catalogo delle riviste ed altri periodici
Documento generato il 04/12/20 alle ore 13:19:55