Computer Science
Scientific paper
Jul 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986ebms.book.....m&link_type=abstract
Unknown
Computer Science
Blue Stars, O Stars, Stellar Evolution, Stellar Models, Diffusion Coefficient, Mixing, Red Shift, Stellar Color, Stellar Rotation, Viscosity, Wolf-Rayet Stars
Scientific paper
The effects of rotationally induced mixing on the evolution of massive stars is examined. Models show that, due to the high radiative viscosity, the diffusion coefficient is sufficiently large to mix most massive stars during their MS lifetime. However, below a critical rotation velocity, diffusive mixing is efficiently prevented by the mu-gradient. A wide bifurcation appears in the evolutionary tracks. Below critical rotation, the evolution is essentially classical with unmodified redwards tracks in the HR diagram. Above critical rotation, the evolutionary tracks go upwards and bluewards, very close to those of fully homogeneous evolution. In this case the model composition is rapidly characterized by He and N enrichments, C and O depletions. The homogeneous models lead to the formation of WR stars before the end of the H-burning phase, which increases the WR lifetime; there is probably no WNE stage in this homogeneous evolutionary scheme. For the classically evolving stars, diffusion may increase the size of the convective core as overshooting does; diffusion may also produce moderate changes of the surface C/N and O/N ratios.
No associations
LandOfFree
Evidence for a bifurcation in massive star evolution 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 Evidence for a bifurcation in massive star evolution, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Evidence for a bifurcation in massive star evolution will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1655047