Evolutionary models for solar metallicity low-mass stars: Mass-magnitude relationships and color-magnitude diagrams
Baraffe, Isabelle Chabrier, Gilles Allard, France Hauschildt, Peter H.
Baraffe, Isabelle
Chabrier, Gilles
Allard, France
Hauschildt, Peter H.
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Time Period
Advisors
Original Date
Digitization Date
Issue Date
1998
Type
Article
Genre
Keywords
Stars: Atmospheres,Stars: Evolution,Stars: Hertzsprung-russel (hr) And C-m Diagrams,Stars: Interiors,Stars: Low-mass, Brown Dwarfs
Subjects (LCSH)
Citation
Baraffe, Isabelle & Chabrier, Gilles & Allard, F. & Hauschildt, Peter. (1998). Evolutionary models for solar metallicity low-mass stars: Mass-magnitude relationships and color-magnitude diagrams. Astronomy and Astrophysics. 337.
Abstract
We present evolutionary models for low mass stars from 0.075 to 1 M<inf>⊙</inf> for solar-type metallicities [M/H]= 0 and -0.5. The calculations include the most recent interior physics and the latest generation of non-grey atmosphere models. We provide mass-age-color-magnitude relationships for both metallicities. The mass-M<inf>V</inf> and mass-M<inf>K</inf>- relations are in excellent agreement with the empirical relations derived observationally. The theoretical color-magnitude diagrams are compared with the sequences of globular clusters (47 Tucanae) and open clusters (NGC2420 and NGC2477) observed with the Hubble Space Telescope. Comparison is also made with field star sequences in M<inf>V</inf>-(V - I), M<inf>K</inf>-(I - K) and M<inf>K</inf>-(J - K) diagrams. These comparisons show that the most recent improvements performed in low-mass star atmosphere models yield now reliable stellar models in the near-infrared. These models can be used for metallicity, mass, temperature and luminosity calibrations. Uncertainties still remain, however, in the optical spectral region below T<inf>eff</inf> ∼ 3700K, where predicted (V-I) colors are too blue by 0.5 mag for a given magnitude. The possible origins for such a discrepancy, most likely a missing source of opacity in the optical and the onset of grain formation are examined in detail. © 2004 Elsevier Science B.V., Amsterdam. All rights reserved.
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Publisher
EDP Sciences
Journal
Astronomy and Astrophysics
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Archival Collection
PubMed ID
DOI
ISSN
0004-6361
1432-0746
1432-0746