Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1976
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976apjs...30..551p&link_type=abstract
Astrophysical Journal Supplement Series, vol. 30, Apr. 1976, p. 551-565.
Astronomy and Astrophysics
Astrophysics
63
Abundance, Atmospheric Models, Chemical Composition, Stellar Atmospheres, Stellar Spectra, Variable Stars, Early Stars, Line Shape, Line Spectra, Tables (Data)
Scientific paper
To provide a complete model-atmosphere abundance analysis of the short-period variable star Gamma Pegasi, continuum data for the region from 1384 to 8100 A, equivalent widths of 274 spectral lines between 3090 and 6700 A, and the H-gamma and H-delta line profiles are analyzed and interpreted using the Princeton UV-line-blanketed model atmospheres as well as the hydrogen-line-broadening theory of Vidal et al. (1970). It is found that an interpolated model atmosphere with an effective temperature of 21,500 K and log g of 3.7 predicts the observed continuum energy distribution from 2200 to 7500 A, the observed hydrogen line profiles, and the ionization equilibria of Si III/Si IV and S II/S III. The abundances given by this model are within 0.2 dex of the solar values, except for neon and possibly chlorine. It is noted that significant non-LTE effects in Ne I are responsible for the apparent overabundance of neon, and it is concluded that the Princeton model atmosphere adequately represents Gamma Pegasi.
No associations
LandOfFree
The chemical composition of Gamma Pegasi 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 chemical composition of Gamma Pegasi, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The chemical composition of Gamma Pegasi will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1612335