High amplitude<i>δ</i>Scuti star BO Lyn with evidence of a late A-type companion in an elliptical orbit

Li, Linjia; Qian, S.‐B.; Zhang, Jia; Zhū, Lìyǐng; Liao, Wuping

doi:10.1088/1674-4527/18/1/11

Cited by 8 publications

(2 citation statements)

References 30 publications

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“…The periodic change can be well fitted by a sinusoidal curve with a period of 11.82 yr and an amplitude of 0.0106 days. The sinusoidal variation may be caused by the orbit motion in a binary system (Lampens et al 2018;Murphy et al 2018), i.e., the light-travel time effect in δ Scuti-type pulsating star, such as BL Cam (Fauvaud et al 2006), AN Lyncis (Li et al 2010), and BO Lyn (Li et al 2018). If it is true, combining the previous absolute parameters of the target and the mass function, the parameters of the companion can be calculated by the following formulae,…”

Section: Discussionmentioning

confidence: 99%

CSS J213934.3-050020: A New Double-mode High-amplitude δ Scuti-type Pulsating Star

Shi

Qian

et al. 2021

PASP

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CSS J213934.3-050020 (hereafter J213934) was originally found as an EW-type eclipsing binary star with a period of 0.225456 days by Catalina Real-time Transient Survey. With the stellar atmospheric parameters from the LAMOST, it is found that the temperature is much higher than those of normal EW-type binaries and does not follow the period–temperature relation of EW-type eclipsing binary stars. To study the physical properties of the variable star, new B and V light curves were obtained by using the 70 cm telescope at the Lijiang station of Yunnan Observatories. It is detected that this variable star is a high-amplitude δ Scuti-type pulsating star rather than an EW-type eclipsing binary. On the log g – T diagram, J213934 lies inside the classical Cepheid instability strip where most δ Scuti stars are located. The results of pulsating frequency analysis show the fundamental frequency f 0 = 6.8195 day−1, the first overtone f 1 = 8.8709 day−1 and 4 harmonics or linear combinations. The mass of J213934 is estimated as 1.83 − 0.21 + 0.27 M ⊙ . The period is revised as 0.11272960 days by using 16 new determined times of light maximum. Meanwhile, it is discovered that its O − C curve shows an upward parabolic variation and a sinusoidal variation. The upward parabolic variation may be a part of a cyclic change or a long-time pulsation period increase caused by its evolution. The sinusoidal variation may be caused by the light-travel-time effect via the presence of a companion star.

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Section: Discussionmentioning

confidence: 99%

CSS J213934.3-050020: A New Double-mode High-amplitude δ Scuti-type Pulsating Star

Shi

Qian

et al. 2021

PASP

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“…We suspected it to be a binary, and therefore vertically displaced in absolute magnitude, as the dominant mode of HADS should fall on the fundamental-mode P-L sequence. Indeed, Li et al (2018) suggested it has an A-type companion in a 35-yr orbit, based on variations in the pulsation phase over the past century.…”

Section: Second Ridge Starsmentioning

confidence: 99%

Revisiting bright delta Scuti stars and their period-luminosity relation with TESS and Gaia DR3

Barac¹,

Bedding²,

Murphy³

et al. 2022

Preprint

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We have used NASA's TESS mission to study catalogued 𝛿 Scuti stars. We examined TESS light curves for 434 stars, including many for which few previous observations exist. We found that 62 are not 𝛿 Scuti pulsators, with most instead showing variability from binarity. For the 372 𝛿 Scuti stars, we provide a catalogue of the period and amplitude of the dominant pulsation mode. Using Gaia DR3 parallaxes, we place the stars in the period-luminosity diagram and confirm previous findings that most stars lie on a ridge that corresponds to pulsation in the fundamental radial mode, and that many others fall on a second ridge that is a factor two shorter in period. This second ridge is seen more clearly than before, thanks to the revised periods and distances. We demonstrate the value of the period-luminosity diagram in distinguishing 𝛿 Scuti stars from short-period RR Lyrae stars, and we find several new examples of high-frequency 𝛿 Scuti stars with regular sequences of overtone modes, including XX Pyx and 29 Cyg. Finally, we revisit the sample of 𝛿 Scuti stars observed by Kepler and show that they follow a tight period-density relation, with a pulsation constant for the fundamental mode of 𝑄 = 0.0315 d.

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Multi-color light curves and orbital period research of eclipsing binary V1073 Cyg

Tian

Zhu

Qian

et al. 2018

Res. Astron. Astrophys.

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New Multi-color B V R c I c photometric observation are presented for W UMa type eclipsing binary V1073 Cyg. The multi-color light curves analysis with the Wilson-Devinney(W-D) procedure acquired the absolute parameters of this system, showing thatV1073Cyg is a shallow contact binary system with fill-out factor f = 0.124(±0.011). We collected all available times of light minima spanning 119 years including CCD data to construct the O-C curve and made detailed O-C analysis. The O-C diagram shows that the period change is complex. There exist a long-term continuous decrease and a cyclic variation. The period is decreasing at a rate ofṖ = −1.04(±0.18) × 10 −10 days · cycle −1 , and with the period decrease, V1073 Cyg will evolve to deep contact stage. The cyclic variation with a period of P 3 = 82.7(±3.6)years and an amplitude of A = 0.028(±0.002)day may be explained by the magnetic activity of one or both components or the light travel time effect (LTTE) caused by a distant third companion with M 3 (i ′ = 90 • ) = 0.511M ⊙ .

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

Cited by 8 publications

References 30 publications

CSS J213934.3-050020: A New Double-mode High-amplitude δ Scuti-type Pulsating Star

CSS J213934.3-050020: A New Double-mode High-amplitude δ Scuti-type Pulsating Star

Revisiting bright delta Scuti stars and their period-luminosity relation with TESS and Gaia DR3

Multi-color light curves and orbital period research of eclipsing binary V1073 Cyg

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