The CCD photometric study of the newly identified RS CVn binary star DV Piscium

Zhang, Liyun; Zhang, Xiliang; Zhu, Zong-Hong

doi:10.1016/j.newast.2009.10.004

Cited by 21 publications

(5 citation statements)

References 17 publications

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“…Most of the R-band flares in cool stars usually have low amplitudes of less than 0.15 mag, accompanied by occasional large amplitudes over 0.2 mag (e.g. Zeilik et al 1982;Kozhevnikova et al 2004Kozhevnikova et al , 2006Nelson & Caton 2007;Vida et al 2009;Zhang et al 2010). The largest R-band flare in the M-type eclipsing binary CU Cnc detected recently by Qian et al (2012) only had an amplitude of 0.52 mag.…”

Section: Transient Eventsmentioning

confidence: 99%

Updated Photometry and Orbital Period Analysis for the Polar Am Herculis on the Upper Edge of the Period Gap

Dai

Qian

2013

ApJ

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Twenty-one new optical light curves, including five curves obtained in 2009 and sixteen curves detected from the AAVSO International Database spanning from 1977 to 2011, demonstrate 16 new primary minimum light times in the high state. Furthermore, seven newly found low-state transient events from 2006 to 2009 were discovered, consisting of five Gaussian-shaped events and two events with an exponential form with decay timescales of <0.005 days; these timescales are one order of magnitude shorter than those of previous X-ray flare events. In the state transition, two special events were detected: a "disrupted event" with an amplitude of ∼ 2 mag and a duration of ∼ 72 minutes and continuing R-band twin events larger than all known R-band flares detected in M-type red dwarfs. All 45 available high-state data points spanning over 35 yr were used to construct an updated O-C diagram of AM Herculis, which clearly shows a significant sinelike variation with a period of 12-15 yr and an amplitude of 6-9 minutes. Using the inspected physical parameters of the donor star, the secular variation in the O-C diagram cannot be interpreted by any decided angular momentum loss mechanism, but can satisfy the condition τṀ 2 ≃ τ KH >> τṘ

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Section: Transient Eventsmentioning

confidence: 99%

Updated Photometry and Orbital Period Analysis for the Polar Am Herculis on the Upper Edge of the Period Gap

Dai

Qian

2013

ApJ

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“…The origin of these short-period CEBs is still an open question. The progenitor of J0344 may be a system similar to DV Psc (Robb et al 1999;Zhang & Zhang 2007;Zhang et al 2010;Pi et al 2014Pi et al , 2019, which is an RS CVn-type binary with a spectral type of K4-5 (Stephenson 1986;Lu et al 2001). Qian et al (2013aQian et al ( ,b, 2014 thought that the existence of an additional stellar component may play an important role for helping to produce these systems.…”

Section: Discussionmentioning

confidence: 99%

1SWASP J034439.97+030425.5: a short-period eclipsing binary system with a close-in stellar companion

Zhang

Qian

Wang

et al. 2020

Res. Astron. Astrophys.

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First multi-wavelength photometric light curves (LCs) of the short-period eclipsing binary (EB) 1SWASP J034439.97+030425.5 (hereafter J0344) are presented and analyzed by using the 2013 version of the Wilson-Devinney (W-D) code. To explain the asymmetric LCs of J0344, a cool star-spot on the less massive component was employed. The photometric solutions suggest that J0344 is a W-subtype shallow contact EB with a contact degree of f = 4.9% ± 3.0% and a mass ratio of q = 2.456 ± 0.013. Moreover, an obvious third light was detected in our analysis. We calculated the average luminosity contribution of the third light to the total light, and that value reaches up to 49.78%. Based on the O − C method, the variations of the orbital period were studied for the first time. Our O − C diagram reveals a secular decrease superimposed on a cyclic oscillation. The orbital period decreases at a rate of dP/dt = −6.07 × 10−7 d yr−1, which can be explained by the mass transfer from the more massive component to the less massive one. Besides, its O − C diagram also shows a cyclic oscillation with an amplitude of 0.0030 d and a period about 7.08 yr, which can be explained by the presence of a third body with a minimum mass of M 3min = 0.15 ± 0.02 M ⊙. The third component may play an important role in the formation and evolution of J0344 by drawing angular momentum from the central system.

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“…136 J210144 +340044 with the largest amplitude in Table 10, the other five brightening events are asymmetric (i.e., the steep rise and moderate fall branches), like the V-band OPTIC flare found during the low state of polar prototype AM Her (Kafka et al 2005). Although most R-band flares in cool stars have low amplitudes of less than 0.15 mag, accompanied by occasional large amplitudes over 0.2 mag (see Vida et al 2009;Zhang et al 2010;Dai et al 2012), the three low-amplitude humps detected in three stars: No. 280 J210207+335644 and No.…”

Section: Brightening Eventsmentioning

confidence: 92%

Full-frame Data Reduction Method: A Data Mining Tool to Detect the Potential Variations in Optical Photometry

戴¹,

Zhou

Cao

2023

Res. Astron. Astrophys.

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A Synchronous Photometry Data Extraction (SPDE) program, performing indiscriminate monitors of all stars appearing at the same field of view of astronomical image, is developed by integrating several Astropy affiliated packages to make full use of time series observed by the traditional small/medium aperture ground-based telescope. The complete full-frame stellar photometry data reductions implemented for the two time series of cataclysmic variables: RX\,J2102.0+3359 and Paloma\,J0524+4244 produce 363 and 641 optimal light curves, respectively. A cross-identification with the SIMBAD finds 23 known stars, of which 16 red giant-/horizontal-branch stars, 2 W\,UMa-type eclipsing variables, 2 program stars, a X-ray source and 2 Asteroid Terrestrial-impact Last Alert System variables. Based on the data productions of the SPDE program, a followup Light Curve Analysis (LCA) program identifies 32 potential variable light curves, of which 18 are from the time series of RX\,J2102.0+3359, and 14 are from that of Paloma\,J0524+4244. They are preliminarily separated into periodical, transient, and peculiar types. By querying for the 58 VizieR online data catalogs, their physical parameters and multi-band brightness spanning from X-ray to radio are compiled for future analysis.

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The CCD photometric study of the newly identified RS CVn binary star DV Piscium

Cited by 21 publications

References 17 publications

Updated Photometry and Orbital Period Analysis for the Polar Am Herculis on the Upper Edge of the Period Gap

Updated Photometry and Orbital Period Analysis for the Polar Am Herculis on the Upper Edge of the Period Gap

1SWASP J034439.97+030425.5: a short-period eclipsing binary system with a close-in stellar companion

Full-frame Data Reduction Method: A Data Mining Tool to Detect the Potential Variations in Optical Photometry

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