EDP Sciences
Free access
Issue
A&A
Volume 370, Number 3, May II 2001
Page(s) 982 - 990
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20010284


A&A 370, 982-990 (2001)
DOI: 10.1051/0004-6361:20010284

Convection in the atmospheres and envelopes of turnoff and giant branch stars of globular clusters

J. Montalbán1, 2, F. Kupka3, F. D'Antona1 and W. Schmidt3, 4

1  Osservatorio Astronomico di Roma, 00040 Monteporzio, Italy
2  Instituto de Astrofísica de Canarias, 38200-La Laguna (Tenerife), Spain
3  Institute for Astronomy, University of Vienna, Türkenschanzstraße 17, 1180 Wien, Austria
4  Department of Physics and Astronomy, University of Wales, Cardiff, PO Box 913, Cardiff CF2 3YB, UK

(Received 30 November 2000 / Accepted 16 February 2001)

Abstract
We explore the dependence of ${T}_{\rm eff}$'s and colors of stellar models on the treatment of over-adiabatic convection, both in the atmosphere and in the interior. We compute main sequence, turnoff, and subgiant models for low metallicity stars ( Z=2 10-4) using as boundary conditions two new sets of model atmospheres by the Wien group (Kupka 1996; Smalley & Kupka 1997; Heiter et al. 2001). In these models convection is treated either in the Mixing Length Theory (MLT) or in the Full Spectrum of Turbulence (FST) formulation. We check the dependence of the ${T}_{\rm eff}$ location of the HR diagram both on the optical depth $\tau$ at which the atmospheric boundary conditions are fixed, and on the convective model adopted in the atmosphere and interior. Obviously, full selfconsistency of the result is obtained only if the treatment of convection is the same in the outer layers and in the interior. We show that it is not appropriate to use MLT convection in the atmosphere and FST in the interior; if we wish to test the effect of changing the l/Hp in the MLT, the atmospheric integration must be limited to $\tau=1$. We construct isochrones for ages of 10 Gyr and greater, and transform the theoretical ${T}_{\rm eff}$ and gravity values to the Johnson B and V magnitudes. The two sets of model atmospheres give small differences (up to ~0.03 mag) for the B-V color, a result of the different temperature stratification in the model atmosphere with FST convection treatment compared to that one based on MLT. The FST boundary conditions provide relative locations of turnoff and giant branch which differ from the MLT solutions, and are in better agreement with the HR diagram morphology of the Globular Cluster M 92.


Key words: stars: evolution -- stars: atmospheres -- convection -- Galaxy: globular clusters: individual: M 92

Offprint request: J. Montalbán, montalbn@coma.mporzio.astro.it
The isochrones are available at the WEB location http://www.mporzio.astro.it/~dantona

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