Variability Study of the SX Phoenicis Star BL Camelopardalis

Fu, Jian-Ning; Zhang, Chao; Marak, Kanokwan; Boonyarak, Chayan; Khokhuntod, Pongsak; Jiang, Shi-Yang

doi:10.1088/1009-9271/8/2/11

Cited by 15 publications

(23 citation statements)

References 13 publications

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“…d 08) and large visual peak-to-peak amplitudes ( 0. m 1; Fu et al 2008). Precise timeseries photometric observations reveal period changes in these stars, which should reflect theoretically the evolutionary changes in radius.…”

Section: Introductionmentioning

confidence: 82%

Stellar Pulsations and Period Changes in the Sx Phoenicis Star Xx Cygni

Yang

Zha

2012

The Astronomical Journal

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Time-series photometric observations were made for the SX Phoenicis star XX Cyg between 2007 and 2011 at the Xinglong Station of National Astronomical Observatories of China. With the light curves derived from the new observations, we do not detect any secondary maximum in the descending portion of the light curves of XX Cyg, as reported in some previous work. Frequency analysis of the light curves confirms a fundamental frequency f 0 = 7.4148 cycles day −1 and up to 19 harmonics, 11 of which are newly detected. However, no secondary mode of pulsation is detected from the light curves. The O−C diagram, produced from 46 newly determined times of maximum light combined with those derived from the literature, reveals a continuous period increase with the rate of (1/P)(dP/dt) = 1.19(13) × 10 −8 yr −1 . Theoretical rates of period change due to the stellar evolution were calculated with a modeling code. The result shows that the observed rate of period change is fully consistent with period change caused by evolutionary behavior predicted by standard theoretical models.

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Section: Introductionmentioning

confidence: 82%

Stellar Pulsations and Period Changes in the Sx Phoenicis Star Xx Cygni

Yang

Zha

2012

The Astronomical Journal

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“…The most recent paper, that of Zong et al ( 2019) did not find evidence of a triple system as stated by Fu et al (2008). Fauvaud et al ( 2010) performed a triple system analysis of the O−C diagram.…”

Section: Period Determination Conclusionmentioning

confidence: 96%

“…Zong et al (2019) carried out an exhaustive analysis of the O−C residuals. Their origin was based on the work of Fu et al (2008) who suggested that the main period of BL Cam might have undergone an abrupt change. This change was studied by Fauvaud et al (2010) and by Conidis & Delaney (2013) who suggested that the change of the main period might be caused by a third body explained by a cubic curve adjustement shown in their Figure 5, which is presented here in Figure 4.…”

Section: O−c Analysismentioning

confidence: 99%

“…Considering a three body system, Borkovits & Hegedüs (1996) present equation 11 in their paper as a solution which we used, adapting it to a binary system in which BL Cam orbits around another unseen star and the encountered variations in the O−C are provoked by the LTTE. This follows a prescription first employed by Fu et al (2008). Combining them, equation 9 provides the mass function in terms of the orbital parameters.…”

Section: Determination Of Orbital Parameters and Mass Of The Companion Starmentioning

confidence: 99%

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A Study of the Sx Phe Star Bl Cam

Peña

Paredes

Piña

et al. 2021

RMxAA

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We determined the physical parameters of the SX Phe star BL Cam from newly available times of maximum light and other times from the literature, as well as from uvby − β photoelectric photometry. From our analysis we found that this star is a binary system. The mass of the companion star was calculated in term of the mass of the primary star and the orbital angle. For this star we determined a metallicity [Fe/H] of −1.2 ± 0.3.

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“…From May 2013, we observed several binaries and variable stars, including YZ Boo (e.g. Boonyarak et al 2011), XX Cyg (e.g., Yang et al 2012), BL Cam (e.g., Fu et al 2008), AN Lyn (e.g., Zhou et al 2006), EH Lib (e.g., Wilson et al 1993). All observations were made through standard Johnson filters.…”

Section: Observing Of Variable Starsmentioning

confidence: 99%

Time-domain survey of the Galactic anti-center using Nanshan 1m telescope

Yang¹,

Esamdin²,

et al. 2015

Proc. IAU

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Following the LAMOST Spectroscopic Survey and Xuyi's Photometric Survey of the Galactic anti-center (GAC), we plan to conduct a time-domain survey of GAC to study the variable sky using Nanshan 1m telescope. The survey will be conducted during winter (in Nov., Dec., and Jan.). The first goal of the survey is to cover 270 sq.deg. of sky area in three years. The survey intends to detect some strong transient events of stars and find some short time-scale variable stars of different types. In this paper, we introduce the survey and present the preliminary results already carried out.

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Variability Study of the SX Phoenicis Star BL Camelopardalis

Cited by 15 publications

References 13 publications

Stellar Pulsations and Period Changes in the Sx Phoenicis Star Xx Cygni

Stellar Pulsations and Period Changes in the Sx Phoenicis Star Xx Cygni

A Study of the Sx Phe Star Bl Cam

Time-domain survey of the Galactic anti-center using Nanshan 1m telescope

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