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

Yang, Xiaohong; Fu, Jian-Ning; Zha, Q.

doi:10.1088/0004-6256/144/4/92

Cited by 19 publications

(31 citation statements)

References 32 publications

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“…To estimate the age of the system, we plotted theoretically calculated models (Mowlavi et al 2012) for temperature versus luminosity (T -L) ( Figure 7). From this diagram, and from McNamara and Feltz (1980), the age of XX Cyg should be approximately (0.949 ± 0.064) × 10 9 years, It is close to the age predicted by Zhou (2002) and Yang et al (2012), which is (0.9 ± 0.3) × 10 9 years as shown in Table 1. The location of XX Cyg in the H-R diagram is shown in Figure 7.…”

supporting

confidence: 85%

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Analysis of a Short Periodic Pulsator: Sx Phoenicis Star Xx Cyg

Abdel-Sabour

Shokry

Ibrahim

2020

RMxAA

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Photometric observations were made of the SX Phoenicis star XX Cyg between September and October 2019, using the 1.88-m Kottamia reflector telescope in Egypt. We used 340 CCD observations with blue-visible-red (BVR) filters to derive light curves. In addition, we obtained 9540 visual magnitudes for XX Cyg from the literature to prepare an observed-minus-calculated (O-C) diagram. 85 new times of maximum for XX Cyg are presented. We did not detect a bump in the descending portion of the light curve of maximum light for XX Cyg. However, we did detect a secular bump in the phased light curves, which changes with phase in some SuperWASP observations. We found the change in period of XX Cyg to be dP/dt = 15.5 × 10-5 s/yr, with its amplitude decreasing at a rate of 0.7 mmag/year. Stellar parameters of XX Cyg and its position in the instability strip of the Hertzsprung Russell stellar evolution diagram are presented.

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supporting

confidence: 85%

“…ABDEL-SABOUR, SHOKRY, & IBRAHIM 20021.0 (0.5) 2.400 1.700 3.660 1.00 Yang et al (2012) 1.7(0.1) 1.700 0.90(0.30) Figure 7. The parameters are in good agreement with those expected for SX Phe variables in the log M −log L plane.…”

mentioning

confidence: 99%

Analysis of a Short Periodic Pulsator: Sx Phoenicis Star Xx Cyg

Abdel-Sabour

Shokry

Ibrahim

2020

RMxAA

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“…The residuals of YZ Boo after all the 6 significant frequencies fitting is only 0.0087 mag, which indicate the modelled curves fit the light curves well. One should note that we usually do not consider the peaks in the low-frequency domain (typically in the range of 0-3 cycles day −1 ) as the significant signals of the variable star, because it originate in the instrument sensitivity instability and variations of sky transparency in the low-frequency domain (Yang et al 2012).…”

Section: Pulsation Analysismentioning

confidence: 99%

Pulsations of the High-AmplitudeδScuti star YZ Bootis

Yang

Esamdin

et al. 2018

Res. Astron. Astrophys.

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We present a study on the pulsations of the high-amplitude δ Scuti star YZ Boo based on photometric observations in Johnson V and R bands with both the Nanshan 1-m telescope of Xinjiang Astronomical Observatory (XAO) and the Xinglong 85-cm telescope of National Astronomical Observatories, Chinese Academy of Sciences (NAOC). The Fourier analysis of the light curves reveals the fundamental radial mode and its five harmonics, with the fourth and the fifth newly detected. 39 new times of light maximum are determined from the light curves, and combined with those in the literature, we construct the O−C diagram and derive a new ephemeris and the determination of a new value of the updated period 0.104091579(2). Besides, the O − C diagram reveals an increasing period change rate of YZ Boo. Theoretical models are calculated and constrained with the observationally determined parameters of YZ Boo. The mass and age of YZ Boo are hence derived as M = 1.61 ± 0.05 M ⊙ and age = (1.44 ± 0.14) × 10 9 yr, respectively. With both the frequency of the fundamental radial mode and the period change rate, YZ Boo is located at the post-main-sequence stage.

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

Cited by 19 publications

References 32 publications

Analysis of a Short Periodic Pulsator: Sx Phoenicis Star Xx Cyg

Analysis of a Short Periodic Pulsator: Sx Phoenicis Star Xx Cyg

Pulsations of the High-AmplitudeδScuti star YZ Bootis

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

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