Long-Term Decrease and Cyclic Variation in the Orbital Period of the Eclipsing Dwarf Nova V2051 Oph

SB, Qian; ZT, Han; Lajús, E. Fernández; LY, Zhu; Lj, Li; WP, Liao; Zhao, Enmin

doi:10.1088/0067-0049/221/1/17

Cited by 41 publications

(29 citation statements)

References 59 publications

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“…8 shows two phase-folded eclipses showing the differences in eclipse structure at different epochs. We confirm the period changes discussed by Baptista et al (2003) and Qian et al (2015), though we cannot confirm that these changes are cyclical in nature due to the relatively short baseline of our observations. V713 Cep: Originally discovered as variable by inspection of archival photometric plates (Antipin & Kroll 2003), eclipses were soon discovered in this CV (vsnet alert 9516).…”

Section: V2051 Ophcontrasting

confidence: 63%

Hunting for eclipses: high-speed observations of cataclysmic variables

Hardy

McAllister

Dhillon

et al. 2016

Mon. Not. R. Astron. Soc.

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Section: V2051 Ophcontrasting

confidence: 63%

Hunting for eclipses: high-speed observations of cataclysmic variables

Hardy

McAllister

Dhillon

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Recently, the orbital period of cataclysmic variable V2051 Oph with a 0.15 M⊙ secondary was found to be decreasing at a rateṖ orb = −5.93 × 10 −10 day yr −1 , which is about six times that induced by gravitational radiation (Qian et al 2015). As a conclusion, Qian et al (2015) proposed that this source supports the argument that full convective stars are undergoing magnetic braking. Our work also shows that magnetic braking without cut-off may play an important role in forming SAX J1808.4-3658.…”

Section: Discussion and Summarymentioning

confidence: 86%

An evolutionary channel towards the accreting millisecond pulsar SAX J1808.4−3658

Chen

2016

Mon. Not. R. Astron. Soc.

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Recent timing analysis reveals that the orbital period of the first discovered accreting millisecond pulsar SAX J1808.4-3658 is increasing at a rateṖ orb = (3.89 ± 0.15) × 10 −12 s s −1 , which is at least one order of magnitude higher than the value arising from the conservative mass transfer. An ejection of mass loss rate of 10 −9 M ⊙ yr −1 from the donor star at the inner Lagrangian point during the quiescence state could interpret the observed orbital period derivative. However, it is unknown whether this source can offer such a high mass loss rate. In this work, we attempt to investigate an evolutionary channel towards SAX J1808.4-3658. Once the accretion disk becomes thermally and viscously unstable, the spin-down luminosity of the millisecond pulsar and the X-ray luminosity during outbursts are assumed to evaporate the donor star, and the resulting winds carry away the specific orbital angular momentum at the inner Lagrangian point. Our scenario could yield the observed orbital period, the orbital period derivative, the peak X-ray luminosity during outbursts. Low-mass Xray binaries with a 1.0 M ⊙ donor star, and an orbital period in the range of 0.8 -1.5 d, may be the progenitor of SAX J1808.4-3658. Our numerical calculations propose that the current donor star mass is 0.044 M ⊙ , which is in approximately agreement with the minimum mass of the donor star. In addition, our scenario can also account for the formation of black widows or the diamond planet like PSR J1719-1438.

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“…By analyzing the O − C variations, very small mass companions can be detected. This method has been successfully used to detect substellar companions surrounding CVs, e.g., Z Cha ), DP Leo (Qian et al 2010a), QS Vir (Qian et al 2010b), UZ For (Potter et al 2011), V2051 Oph (Qian et al 2015). In this paper, we show the investigation of the eclipse times of LX Ser and the possible giant planet orbiting this system.…”

Section: Introductionmentioning

confidence: 87%

A possible giant planet orbiting the cataclysmic variable LX Ser

Zhou

et al. 2017

Publications of the Astronomical Society of Japan

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LX Ser is a deeply eclipsing cataclysmic variable with an orbital period of 0.d 1584325. Sixty two new eclipse times were determined by our observations and the AAVSO International Data base. Combining all available eclipse times, we analyzed the O − C behavior of LX Ser. We found that the O − C diagram of LX Ser shows a sinusoidal oscillation with a period of 22.8 yr and an amplitude of 0.00035 days. Two mechanisms (i.e., the Applegate mechanism and the light travel time effect) are applied to explain the cyclic modulation. We found that the Applegate mechanism is difficult to explain the cyclic oscillation in the orbital period. Therefore, the cyclic period change is most likely to be caused by the light travel time effect due to the presence of a third body. The mass of the tertiary component was determined to be M 3 ∼ 7.5 M Jup . We supposed that the tertiary companion is plausible a giant planet. The stability of the giant planet was checked, and we found that the multiple system is stable.

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Long-Term Decrease and Cyclic Variation in the Orbital Period of the Eclipsing Dwarf Nova V2051 Oph

Cited by 41 publications

References 59 publications

Hunting for eclipses: high-speed observations of cataclysmic variables

Hunting for eclipses: high-speed observations of cataclysmic variables

An evolutionary channel towards the accreting millisecond pulsar SAX J1808.4−3658

A possible giant planet orbiting the cataclysmic variable LX Ser

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