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Titolo:
Structure and evolution of low-mass Population II stars
Autore:
Montalban, J; DAntona, F; Mazzitelli, I;
Indirizzi:
Osservatorio Roma, I-00040 Rome, Italy Osservatorio Roma Rome Italy I-00040 ervatorio Roma, I-00040 Rome, Italy Inst Astrofis Canarias, E-38200 La Laguna, Tenerife, Spain Inst Astrofis Canarias La Laguna Tenerife Spain E-38200 , Tenerife, Spain Ist Astrofis Spaziale, I-00133 Rome, Italy Ist Astrofis Spaziale Rome Italy I-00133 s Spaziale, I-00133 Rome, Italy
Titolo Testata:
ASTRONOMY AND ASTROPHYSICS
fascicolo: 3, volume: 360, anno: 2000,
pagine: 935 - 951
SICI:
0004-6361(200008)360:3<935:SAEOLP>2.0.ZU;2-Y
Fonte:
ISI
Lingua:
ENG
Soggetto:
GLOBULAR-CLUSTER AGES; BROWN DWARFS; TURBULENT CONVECTION; MAIN-SEQUENCE; STELLAR; STATE; METALLICITY; LUMINOSITY; EQUATION; MODELS;
Keywords:
stars : evolution; stars : low-mass, brown dwarfs; stars : luminosity function, mass function; stars : Population II; Galaxy : globular clusters : individual : NGC 6397, M92, M4;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
55
Recensione:
Indirizzi per estratti:
Indirizzo: D'Antona, F Osservatorio Roma, I-00040 Rome, Italy Osservatorio Roma Rome Italy I-00040 ma, I-00040 Rome, Italy
Citazione:
J. Montalban et al., "Structure and evolution of low-mass Population II stars", ASTRON ASTR, 360(3), 2000, pp. 935-951

Abstract

The focus of the present paper is on the detailed description of the internal structures of low mass, population II stars, to clarify some issues about these stellar models and, mainly, their present reliability for observational comparisons. We then explore 1) the role of the local convective model; 2) the differences between "grey" and "non grey" models, and between models in which the photospheric boundary conditions are set at different optical depths (tau(ph) = 3 or 100); 3) the role of the equation of state (EoS), both in the atmospheric models and in the interior. One of the major conclusions of the paper is a cautionary note about the usage of the additive volume law in EoS calculations. The dependence of the HR diagram locations and mass luminosity relations on metal and helium content are also discussed. A few comparisons with globular cluster stars show that: 1) general consistency of distance scales and morphologies in the HR diagram is found, when comparing ground based measurements in the Johnson B and V bands and observations in the HST bands; 2) adiscrepancy between models and observations may exist for more metal rich clusters 3) the plausible hypothesis that the mass function in the globularcluster NGC 6397 behaves smoothly until the lower limit of the main sequence poses constraints on the mass-luminosity relation at the lowest end of the main sequence. The evolutionary tracks are available at the WEB location http://www.mporzio.astro.it.

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Documento generato il 05/12/20 alle ore 08:08:48