Synthetic Hertzsprung-Russell diagrams of open clusters.

Details Synthetic Hertzsprung-Russell diagrams of open clusters. Synthetic Hertzsprung-Russell diagrams of open clusters.

Aug 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...324..556s&link_type=abstract

Astronomy and Astrophysics, v.324, p.556-565

Astronomy and Astrophysics

Astrophysics

75

Stars: Evolution Of, Stars: Pre-Main Sequence, Stars: Hertzsprung-Russell Diagram, Stars: Fundamental Parameters

Scientific paper

New evolutionary models for pre-main sequence (PMS) stars (0.4Msun_<=M<=5Msun_) of three different metallicities (Z=0.005, Z=0.02, and Z=0.04) have been computed. Improvements have been made in the constitutive physics with the use of new opacity tables at low temperatures and new atmospheric models. We first compare our mass tracks with other recent PMS models and show that important deviations occur below 0.5Msun_, due to different treatments of the electrostatic corrections in cool degenerated matter. We first check the ability of our models to reproduce the ZAMS location and the low-mass end of the isochrones. From the turn-off in the M_V_ versus (B-V) diagram, we estimate ages of 4x10^7^ for α Per cluster and between 8x10^7^ and 10^8^yr for the Pleiades, ages comparable or lower than recent determinations including overshooting. These evolutionary models are used to generate synthetic Hertzsprung-Russell Diagrams (HRD). We show that each of the different parameters, namely the initial mass function (IMF), the star formation rate (SFR) and the binary fraction affect in a specific way the morphology of the derived HRD. We propose to use these synthetic diagrams to constrain some of these quantities in observed open clusters. Applying this procedure to the Pleiades cluster, the observed morphology is best reproduced by invoking a large age dispersion (σ_t_=~3x10^7^yr) and a binary fraction for F-G stars of 40%+/-5%.

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