Physical Nature of the Eclipsing δ Scuti Star AO Serpentis

Abstract We present the absolute properties of the eclipsing binary AO Ser with a pulsating component from our BV photometric and high-resolution spectroscopic observations, which were performed between 2017 April and May. The radial velocities (RVs) for both components were measured, and the effect...

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Bibliographic Details
Published in:The Astronomical journal 2020-12, Vol.160 (6), p.247
Main Authors: Park, Jang-Ho, Lee, Jae Woo, Hong, Kyeongsoo, Koo, Jae-Rim, Kim, Chun-Hwey
Format: Article
Language:English
Subjects:
Asteroseismology
Astronomy
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
COMPARATIVE EVALUATIONS
ECLIPSE
Eclipsing binary stars
FREQUENCY ANALYSIS
Fundamental parameters of stars
MASS
Multi-periodic pulsation
Photometry
RADIAL VELOCITY
RESOLUTION
Rotation
SPECTRA
Spectroscopy
STARS
Stellar oscillations
Variable stars
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Summary:Abstract We present the absolute properties of the eclipsing binary AO Ser with a pulsating component from our BV photometric and high-resolution spectroscopic observations, which were performed between 2017 April and May. The radial velocities (RVs) for both components were measured, and the effective temperature and projected rotational velocity of the primary star were determined to be T eff,1  = 8,820 ± 62 K and  = 90 ± 18 km s −1 , respectively, by comparing the observed spectrum with the Kurucz models. The accurate fundamental parameters of AO Ser were determined by a simultaneous analysis of the light and RV curves. The masses and radii of the primary and secondary components are M 1  = 2.55 ± 0.09 M ⊙ and R 1  = 1.64 ± 0.02 R ⊙ and M 2  = 0.49 ± 0.02 M ⊙ and R 2  = 1.38 ± 0.02 R ⊙ , respectively. Multiple frequency analyses for the eclipse-subtracted light residuals were conducted. As a result, we detected two frequencies of f 1  = 21.852 days −1 and f 2  = 23.484 days −1 . The evolutionary position on the HR diagram and the pulsational characteristics indicate that the primary star is a δ Sct pulsator with a radial fundamental mode. On the other hand, the relatively evolved secondary is oversized for its own mass.
ISSN:0004-6256
1538-3881
1538-3881
DOI:10.3847/1538-3881/abbef4