Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a...102..386g&link_type=abstract
Astronomy and Astrophysics, vol. 102, no. 3, Oct. 1981, p. 386-390. Research supported by the Consiglio Nazionale delle Ricerch
Astronomy and Astrophysics
Astrophysics
5
Gaseous Diffusion, Helium, Horizontal Branch Stars, Stellar Evolution, Stellar Models, Abundance, Globular Clusters, Hydrogen
Scientific paper
The inward diffusion of helium in the atmosphere and subatmosphere of horizontal-branch stars in globular clusters is studied. The process of gravitational diffusion is taken into account, as is the star evolution arising from the burning of helium in the core and hydrogen in an intermediate shell. The models also include an improved procedure for the treatment of the induced semiconvection. The original helium abundance (by mass) was approximately 0.3 in a star model where the mass is 0.53 solar mass; the mass fraction in the helium core was 0.92 at the beginning of the HB evolutionary phase. It is thought that the efficient surface depletion of helium might explain the observed deficiency of helium in blue HB stars. Comparing the evolutionary tracks of models with and without helium diffusion, it is found that some differences may be relevant to the interpretation of the HB morphology with possible implications for the pulsation features.
Giannone Pietro
Rossi Luca
No associations
LandOfFree
Helium diffusion in horizontal-branch-star evolutionary models 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 Helium diffusion in horizontal-branch-star evolutionary models, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Helium diffusion in horizontal-branch-star evolutionary models will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1468153