Other
Scientific paper
Aug 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...216...61s&link_type=abstract
Astrophysical Journal, Part 1, vol. 216, Aug. 15, 1977, p. 61-66.
Other
7
Carbon, Helium, Nuclear Fusion, R Coronae Borealis Stars, Stellar Evolution, Stellar Models, Main Sequence Stars, Neutrinos, Opacity, Supergiant Stars, Wolf-Rayet Stars
Scientific paper
The evolution of helium stars in the mass range from 4 to 15 solar masses has been followed from the initial helium main sequence to the end of carbon burning in the core, with the use of Carson's (1976) radiative opacities. As compared with earlier work based on smaller opacities, the main-sequence band in the H-R diagram is now both wider and cooler than before. If neutrino losses are neglected in the stellar models, the phase of carbon burning in the core occurs in the red-supergiant region; otherwise, it occurs, as it does in the earlier models with or without neutrino emission, close to the helium main sequence. Observational data for Wolf-Rayet stars and R Coronae Borealis variables are found to lend some support to the present models.
Chin Chao-Wen
Stothers Richard
No associations
LandOfFree
Evolution of helium stars 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 Evolution of helium stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Evolution of helium stars will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1880238