Stellar evolution models for Z = 0.0001 to 0.03

Details Stellar evolution models for Z = 0.0001 to 0.03 Stellar evolution models for Z = 0.0001 to 0.03

Aug 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mnras.298..525p&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 298, Issue 2, pp. 525-536.

Astronomy and Astrophysics

Astronomy

246

Convection, Stars: Evolution, Hertzsprung-Russell (Hr) Diagram, Stars: Population Ii, Open Clusters And Associations: General, Galaxies: Stellar Content

Scientific paper

We have calculated a grid of empirically well tested evolutionary tracks with masses M between 0.5 and 50Msolar, spaced by approximately 0.1 in log M, and with metallicities Z=0.0001, 0.0003, 0.001, 0.004, 0.01, 0.02 and 0.03. We use a robust and fast evolution code with a self-adaptive non-Lagrangian mesh, which employs the mixing-length theory but treats convective mixing as a diffusion process, solving simultaneously for the structure and the chemical composition. The hydrogen and helium abundances are chosen as functions of the metallicity: X=0.76-3.0ZY=0.24+2.0Z. Two sets of models were computed, one without and one with a certain amount of enhanced mixing or `overshooting'. This amount has been empirically chosen by means of various sensitive tests for overshooting: (1) the luminosity of core helium burning (blue loop) giants of well-known mass, (2) the width of the main sequence as defined by double-lined eclipsing binaries with well-measured masses and radii, and (3) the shape and implied stellar distribution of isochrones of various open clusters. The first two tests have been the subject of previous papers, the third test is discussed in this paper. On the basis of these tests, we recommend the use of the overshooting models for masses above about 1.5Msolar. We describe here the characteristics of the models, the procedure for constructing isochrones for arbitrary age and metallicity from the models, and the performance of these isochrones for several intermediate-age and old open clusters. All original models are available in electronic form and we describe the means by which they may be obtained.

Affiliated with

Also associated with

No associations

Rating

Stellar evolution models for Z = 0.0001 to 0.03 does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Stellar evolution models for Z = 0.0001 to 0.03, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Stellar evolution models for Z = 0.0001 to 0.03 will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1535509