Fundamental Properties of O and B Stars with Optical Interferometry

We used interferometric observations made with the CHARA Array of 25 B-type stars and 6 O-type stars to obtain precise measurements of angular size, radius, and effective temperature to test stellar atmospheric models for massive stars. Our measured angular diameters range from 1.09 milli-arcseconds...

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Bibliographic Details
Published in:Proceedings of the International Astronomical Union 2022-05, Vol.18 (S361), p.382-386
Main Authors: Gordon, Kathryn D., Gies, Douglas R., Schaefer, Gail H.
Format: Article
Language:English
Subjects:
Arrays
Astronomical models
B stars
Contributed Paper
Diameters
Fluxes
Infrared analysis
Infrared spectra
Infrared spectrophotometers
Infrared stars
Interferometry
Massive stars
O stars
Optical properties
Rotational spectra
Spectrophotometry
Stars & galaxies
Stellar atmospheres
Telescopes
Temperature
Ultraviolet spectra
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Summary:We used interferometric observations made with the CHARA Array of 25 B-type stars and 6 O-type stars to obtain precise measurements of angular size, radius, and effective temperature to test stellar atmospheric models for massive stars. Our measured angular diameters range from 1.09 milli-arcseconds (mas) for β Tau down to 0.11 mas for 10 Lac, the smallest star yet resolved with the CHARA Array. The rotational oblateness of the rapidly rotating star ζ Oph is directly measured for the first time. We collected ultraviolet to infrared spectrophotometry for all sample stars and derived temperatures, angular diameters, and reddening estimates that best fit the spectra. There is generally good agreement between the observed and spectral fit angular diameters for the O and B stars, indicating that the fluxes predicted from model atmospheres are reliable. The derived and model temperatures for the O stars are also in fair agreement, however the sample size is small and several of the O stars results we consider to be preliminary. On the other hand, the temperatures derived from angular diameters and fluxes tend to be larger (by ≈ 4%) for the B stars than those from published results based on analysis of the line spectrum (Gordon et al. 2018, 2019).
ISSN:1743-9213
1743-9221
DOI:10.1017/S1743921322002642