Statistics – Computation
Scientific paper
May 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26as...69..183h&link_type=abstract
Astronomy and Astrophysics Supplement Series (ISSN 0365-0138), vol. 69, no. 2, May 1987, p. 183-211.
Statistics
Computation
6
B Stars, Computational Astrophysics, Helium, Stellar Evolution, Difference Equations, Equations Of State, Opacity, Saha Equations, Stellar Physics, Stellar Structure
Scientific paper
A description is given of the evolutionary program used for calculating the evolution of helium stars in the mass range 2.0 to 4.0 M_sun; from the helium Zero Age main sequence up to neon ignition (Habets, 1986). The physics involved is summarized with special emphasis on the equation of state. The evolutionary sequences are given in a tabular form. The diffusion equation used to treat convective mixing and the interior structure in the evolved stages are discussed (in appendices). A new three-point difference equation (given in an appendix) is used to overcome numerical instabilities during carbon burning.
No associations
LandOfFree
The evolution of helium stars in the mass range 2.0 to 4.0 solar masses - The evolutionary program 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 The evolution of helium stars in the mass range 2.0 to 4.0 solar masses - The evolutionary program, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The evolution of helium stars in the mass range 2.0 to 4.0 solar masses - The evolutionary program will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-856309