Physical parameters and orbital period variation of a newly discovered cataclysmic variable GSC 4560–02157

Han, Z.; Qian, S.‐B.; Voloshina, I. B.; Metlov, V. G.; Zhu, L.-Y.; Li, Linjia

doi:10.1088/1674-4527/16/10/156

Cited by 10 publications

(7 citation statements)

References 21 publications

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“…If we assume that the periodic change in the O − C curve exists, by analysis of equation ( 3) the sinusoidal term reveals a cyclic change with a semi-amplitude of 0.0054 d and a period of 49.92 yr. The periodic variations in W UMa binary stars are usually explained by two ideas: one is the Applegate mechanism (Applegate 1992) via magnetic activity cycles at one component or both, and the second idea is the light travel-time effect (Liao & Qian 2010;Han et al 2016) via the presence of a third body.…”

Section: Discussionmentioning

confidence: 99%

RW Doradus: A solar-type shallow contact binary with a new orbital period investigation

Sarotsakulchai

Qian

Soonthornthum

et al. 2019

Publications of the Astronomical Society of Japan

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New CCD photometric light curves of the short-period (P = 0.285 d) eclipsing binary RW Dor are presented. The observations were performed with the PROMPT-8 robotic telescope at CTIO in Chile between 2015 March and 2017 March. Other eclipse timings were obtained from the 2.15 m JS telescope at CASLEO, San Juan, Argentina in 2011 December. Based on a light curve analysis, it is found that RW Dor is a W-type shallow contact binary with a fill-out factor f ∼ 11% and a high mass ratio q ∼ 1.587 (1/q = 0.63), where the hotter component is the less massive one (M 1 ∼ 0.52 M and M 2 ∼ 0.82 M ). For orbital-period investigation, 15 new eclipse times and those previously published were compiled. O − C analysis with very weak evidence suggests that a long-term decrease in period with a rate of dP/dt = −9.61 × 10 −9 d yr −1 is superimposed on a cyclic variation (A 3 = 0.0054 d and P 3 = 49.9 yr). The long-term decrease can be interpreted as mass transfer from the more massive component to the less massive one, or combined with angular momentum loss via magnetic braking. In addition, the marginal contact phase, high mass ratio (1/q > 0.4), and long-term decrease in period all suggest that RW Dor is a newly formed contact binary via Case A mass transfer, and it will evolve into a deeper normal contact binary. If the cyclic change is correct, the light travel-time effect via the presence of a cool third body will be a more plausible explanation for this.

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Section: Discussionmentioning

confidence: 99%

RW Doradus: A solar-type shallow contact binary with a new orbital period investigation

Sarotsakulchai

Qian

Soonthornthum

et al. 2019

Publications of the Astronomical Society of Japan

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“…Sinusoidal O-C modulations have been identified or proposed in a number of additional AWD systems (e.g. Bond & Freeth 1988;Dai et al 2010;Han et al 2016), but the orbital cycles of these systems are generally either poorly sampled or have not been observed in their entirety. Previous studies have shown that these modulations cannot always be explained by the orbit of a third body (e.g.…”

Section: Third Body In the Z Cha Systemmentioning

confidence: 99%

The eclipsing accreting white dwarf Z chameleontis as seen with TESS

Court

Scaringi

Rappaport

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present results from a study of TESS observations of the eclipsing dwarf nova system Z Cha, covering both an outburst and a superoutburst. We discover that Z Cha undergoes hysteretic loops in eclipse depth -out-of-eclipse flux space in both the outburst and the superoutburst. The direction that these loops are executed in indicates that the disk size increases during an outburst before the mass transfer rate through the disk increases, placing constraints on the physics behind the triggering of outbursts and superoutbursts. By fitting the signature of the superhump period in a flux-phase diagram, we find the rate at which this period decreases in this system during a superoutburst for the first time. We find that the superhumps in this source skip evolutionary stage "A" seen during most dwarf nova superoutbursts, even though this evolutionary stage has been seen during previous superoutbursts of the same object. Finally, O-C values of eclipses in our sample are used to calculate new ephemerides for the system, strengthening the case for a third body in Z Cha and placing new constraints on its orbit.

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“…The most common method for determining the period variations is to analyze the observed-calculated (O − C) diagram. We have used this method several times in the past few years to study a few eclipsing CVs such as Z Cha (Dai et al 2009), OY Car (Han et al 2015), V2051 Oph (Qian et al 2015) and GSC 4560-02157 (Han et al 2016). In this paper, we present new CCD photometric observations of AY Psc and update the orbital ephemeris.…”

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confidence: 99%

Long-term photometric behavior of the eclipsing Z Cam-type dwarf nova AY Psc

Han

Qian

Voloshina

et al. 2017

Res. Astron. Astrophys.

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New eclipse timings of the Z Cam-type dwarf nova AY Psc were measured and the orbital ephemeris was revised. Based on the long-term AAVSO data, moreover, the outburst behaviors were also explored. Our analysis suggests that the normal outbursts are quasiperiodic, with an amplitude of ∼ 2.5(±0.1) mag and a period of ∼ 18.3(±0.7) days. The amplitude vs. recurrence-time relation of AY Psc is discussed, and we concluded that this relation may represents general properties of dwarf nova (DN) outbursts. The observed standstill ends with an outburst, which is inconsistent with the general picture of Z Cam-type stars.This unusual behavior was considered to be related to the mass-transfer outbursts. Moreover, the average luminosity is brighter during standstills than during outburst cycles. The changes in brightness marks the variations inṀ 2 due to the disc of AY Psc is nearly steady state.Ṁ 2 value was limited to the range from 6.35 × 10 −9 to 1.18 × 10 −8 M ⊙ yr −1 . More detailed examination shows that there are a few small outbursts presence during standstills. These events with amplitudes of ∼ 0.5 − 0.9 mag are very similar to the stunted outbursts reported in some NLs. We discussed several possible mechanisms and suggested that the most reasonable mechanism for these stunted outbursts is a changing mass-transfer rate.

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Physical parameters and orbital period variation of a newly discovered cataclysmic variable GSC 4560–02157

Cited by 10 publications

References 21 publications

RW Doradus: A solar-type shallow contact binary with a new orbital period investigation

RW Doradus: A solar-type shallow contact binary with a new orbital period investigation

The eclipsing accreting white dwarf Z chameleontis as seen with TESS

Long-term photometric behavior of the eclipsing Z Cam-type dwarf nova AY Psc

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