A Period Investigation of the Sx Phoenicis Star Dy Pegasi

Li, L.-J.; Qian, S.‐B.

doi:10.1088/0004-6256/139/6/2639

Cited by 11 publications

(2 citation statements)

References 18 publications

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“…The data are not sufficient to prove that the abrupt change of the main period was caused by the third object, and its orbital properties are dependent on the long-term correction of the O−C trend, which need to be confirmed by future observations. To determine the mass of the companion, we use the mass function adopted in previous literature (Fu et al 2008;Li & Qian 2010). The value of mass function of the companion is derived to be 1.65(3) × 10 −4 and it is 17% of that obtained by Fu et al (2008).…”

Section: Period Changesmentioning

confidence: 99%

Pulsations of the SX Phe Star BL Camelopardalis

Zong

Esamdin

et al. 2019

PASP

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We carried out photometric observations of the SX Phe star BL Cam in 2014, 2017 and 2018 using Nanshan 1-m telescope. In addition to the dominated frequency of 25.5790(3) cd −1 and its two harmonics, an independent frequency of 25.247 (2) cd −1 , which is a nonradial mode frequency, was detected from the data in 2014. A total of 123 new times of light maxima were determined from our light curves in the three years, which, together with that published in the literature, were used to analyze the O−C diagram. The change rate of the main period was derived as (1/P)(dP/dt) = -2.39 (8)×10 −8 yr −1 , which is lower than that published in previous literature. A periodical change with a period of 14.01 (9) yr was found in the residuals of the O−C curve fitting. If it was caused by the light-time effect, BL Cam should be a binary system. The mass of the companion was restricted as low as that of a brown dwarf. No evidence of the triple system suggested by previous authors was shown in our analysis.

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Section: Period Changesmentioning

confidence: 99%

Pulsations of the SX Phe Star BL Camelopardalis

Zong

Esamdin

et al. 2019

PASP

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“…P B is the orbital period of the binary system; t is the time of light maximum; T is the time of passage through the periastron. A detailed description can be referenced in Li & Qian (2010).…”

Section: O − C Analysismentioning

confidence: 99%

High amplitudeδScuti star BO Lyn with evidence of a late A-type companion in an elliptical orbit

Qian

Zhang

et al. 2018

Res. Astron. Astrophys.

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We present 145 times of light maximum for high amplitude δ Scuti star BO Lyn based on several sky surveys (CRTS, DASCH, NSVS, OMC and SuperWASP) and our photometric observations. Combining with the data in literature, a total of 179 times of light maximum are used to analyze the O − C diagram of BO Lyn. We find that it can be described by an upward parabolic component and a periodic variation with a period of 34.5 ± 0.1 yr. The latter could be caused by the light travel time effect as a result of an additional companion orbiting in a highly elliptical orbit (e = 0.64 ± 0.03). Our study indicates that the companion’s luminosity cannot be ignored, and it should be a late A-type main-sequence star. The long-term period change of BO Lyn is also detected, and its value, 1.52 ± 0.26 × 10−3 d Myr−1, is consistent with evolutionary models. We suggest that more spectroscopic and photometric observations are needed in the future to confirm the nature of the BO Lyn system.

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Detection of a cool stellar companion to the δ Scuti variable star BP Peg

Wang

Qian

et al. 2014

New Astronomy

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A Period Investigation of the Sx Phoenicis Star Dy Pegasi

Cited by 11 publications

References 18 publications

Pulsations of the SX Phe Star BL Camelopardalis

Pulsations of the SX Phe Star BL Camelopardalis

High amplitudeδScuti star BO Lyn with evidence of a late A-type companion in an elliptical orbit

Detection of a cool stellar companion to the δ Scuti variable star BP Peg

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