New pre-main-sequence tracks for M less than or equal to 2.5 solar mass as tests of opacities and convection model

Details New pre-main-sequence tracks for M less than or equal to 2.5 solar mass as tests of opacities and convection model New pre-main-sequence tracks for M less than or equal to 2.5 solar mass as tests of opacities and convection model

Jan 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apjs...90..467d&link_type=abstract

Astrophysical Journal Supplement Series, vol. 90, no. 1, p. 467-500

Statistics

Computation

740

Combustion, Computational Astrophysics, Deuterium, Hertzsprung-Russell Diagram, Lithium, Opacity, Pre-Main Sequence Stars, Stellar Convection, Stellar Evolution, Stellar Models, Abundance, Atomic Interactions, Computation, Equations Of State, Equilibrium Methods, Hydrostatics, Numerical Analysis

Scientific paper

We present tabular and graphic results on the computation of pre-main-sequence evolutionary tracks of Population I stellar structures from 2.5 to approximately 0.015 solar mass. Deuterium and lithium burning are followed in detail. The chosen input physics gives M approximately 0.018 solar mass as minimum mass for deuterium burning and M approximately 0.065 solar mass as minimum mass for lithium burning. While we adopt the approximations of hydrostatic equilibrium, no mass accretion and no mass loss, we have taken care to include several updates in the input physics, among them two different sets of the more recent available low-temperature opacities, and we test two different models of overdiabatic convection (the mixing-available low-temperature opacities, and we test two different models of overdiabatic convection (the mixing-length theory (MLT) with the mixing-length scale calibrated on the solar model, and the recent Canuto & Mazzitelli (CM) model). The Hertzsprung-Russell diagram location of tracks turns out to be largely model-dependent, especially for M less than or equal to 0.6 solar mass, and we are able to relate the cause of the large differences (up to 0.04 dex in Teff at 0.3 solar mass) with opacity and with the details of the convection model adopted. Since we are not able to provide 'first principle' physical reasons to choose among models, we consider these tracks as 'tests', in the hope that significant comparisons with observations can exclude some models or provide hints toward a better understanding of convection. Nevertheless, we feel obliged to call the reader's attention to the fact that theoretical Teff's, especially in the red, are intrinsically ill-determined, and no sound observational interpretation critically depending on the Teff's can be presently performed, contrary to the current habit due to an exceedingly 'faithful' use of the MLT.

Affiliated with

Also associated with

No associations

Rating

New pre-main-sequence tracks for M less than or equal to 2.5 solar mass as tests of opacities and convection model 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 New pre-main-sequence tracks for M less than or equal to 2.5 solar mass as tests of opacities and convection model, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and New pre-main-sequence tracks for M less than or equal to 2.5 solar mass as tests of opacities and convection model will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-866390