期刊
ASTRONOMICAL JOURNAL
卷 159, 期 5, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.3847/1538-3881/ab7d38
关键词
Asteroseismology; Exoplanet detection methods; Binary stars; Delta Scuti variable stars; B subdwarf stars
资金
- Australian Government Research Training Program (AGRTP)
- University of Sydney Merit Award scholarships
- Australian Government through the Australian Research Council DECRA [DE180101104]
- Simons Foundation
- NASA through the Sagan Fellowship Program
- Australian Research Council [DE180101104] Funding Source: Australian Research Council
Mutual gravitation between a pulsating star and an orbital companion leads to a time-dependent variation in path length for starlight traveling to Earth. These variations can be used for coherently pulsating stars, such as the delta Scuti variables, to constrain the masses and orbits of their companions. Observing these variations for delta Scuti stars has previously relied on subdividing the light curve and measuring the average pulsation phase in equally sized subdivisions, which leads to undersampling near periapsis. We introduce a new approach that simultaneously forward models each sample in the light curve and show that this method improves upon current sensitivity limits-especially in the case of highly eccentric and short-period binaries. We find that this approach is sensitive enough to observe Jupiter mass planets around delta Scuti stars under ideal conditions, and use gravity-mode pulsations in the subdwarf B star KIC 7668647 to detect its companion without radial velocity data. We further provide robust detection limits as a function of the signal-to-noise ratio of the pulsation mode and determine that the minimum detectable light travel time amplitude for a typical Kepler delta Scuti is around 2 s. This new method significantly enhances the application of light travel time variations to detecting short-period binaries with pulsating components, and pulsating A-type exoplanet host stars, especially as a tool for eliminating false positives.
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