Possible connection between period change and magnetic activity of the very short‐period binary VZ Piscium

Qian, S. J.; Soonthornthum, B.; Fang, Xiang; Zhu, L.-Y.; He, Jiajia

doi:10.1002/asna.200410251

Cited by 8 publications

(5 citation statements)

References 14 publications

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“…This fell outside the 36 ′′ ×36 ′′ field of view of Rucinski et al (2007). Note that Qian et al (2004) suggest a closer companion to the binary may be causing a variation in the lightcurve with a period of ∼25 years. However, no close companion was identified -16by Rucinski et al (2007), and our companion is too wide to introduce such a short period variation.…”

Section: Hip 115819 (Vz Piscium)mentioning

confidence: 89%

WIDE COOL AND ULTRACOOL COMPANIONS TO NEARBY STARS FROM Pan-STARRS 1

Deacon

Liu

Magnier

et al. 2014

ApJ

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We present the discovery of 57 wide (>5 ) separation, low-mass (stellar and substellar) companions to stars in the solar neighborhood identified from Pan-STARRS 1 (PS1) data and the spectral classification of 31 previously known companions. Our companions represent a selective subsample of promising candidates and span a range in spectral type of K7-L9 with the addition of one DA white dwarf. These were identified primarily from a dedicated common proper motion search around nearby stars, along with a few as serendipitous discoveries from our Pan-STARRS 1 brown dwarf search. Our discoveries include 23 new L dwarf companions and one known L dwarf not previously identified as a companion. The primary stars around which we searched for companions come from a list of bright stars with well-measured parallaxes and large proper motions from the Hipparcos catalog (8583 stars, mostly A-K dwarfs) and fainter stars from other proper motion catalogs (79170 stars, mostly M dwarfs). We examine the likelihood that our companions are chance alignments between unrelated stars and conclude that this is unlikely for the majority of the objects that we have followed-up spectroscopically. We also examine the entire population of ultracool (>M7) dwarf companions and conclude that while some are loosely bound, most are unlikely to be disrupted over the course of ∼10 Gyr. Our search increases the number of ultracool M dwarf companions wider than 300 AU by 88% and increases the number of L dwarf companions in the same separation range by 82%. Finally, we resolve our new L dwarf companion to HIP 6407 into a tight (0. 13, 7.4 AU) L1+T3 binary, making the system a hierarchical triple. Our search for these key benchmarks against which brown dwarf and exoplanet atmosphere models are tested has yielded the largest number of discoveries to date.

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Section: Hip 115819 (Vz Piscium)mentioning

confidence: 89%

WIDE COOL AND ULTRACOOL COMPANIONS TO NEARBY STARS FROM Pan-STARRS 1

Deacon

Liu

Magnier

et al. 2014

ApJ

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“…In binary stars, when at least one of the components has a convective outer envelope, magnetic activity may be expected. In this case, the orbital period of these active systems may indicate cyclic orbital period variations, as discussed for several systems (e.g Qian et al 2004; Zhang…”

Section: Applegate Modelmentioning

confidence: 86%

CN Andromedae: a shallow contact binary with a possible tertiary component

Yıldırım

Aliçavuş

Soydugan

2019

Res. Astron. Astrophys.

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In this study, new photometric observations of shallow contact binary CN Andromedae (CN And) were performed and multi-color (BV R) CCD light curves (LCs) were obtained. Simultaneous analysis of new LCs and published radial velocity (RV) data reveals that the system is an early contact binary in which both components have recently filled their inner Roche lobes. Asymmetric LCs were modeled by a dark spot on the primary component and a hot spot on the secondary component that probably resulted from magnetic activity and mass transfer, respectively. Modeling of LCs and RV data allows us to estimate the following absolute parameters: M1 = 1.40 ± 0.02 M⊙, M2 = 0.55 ± 0.01 M⊙, R1 = 1.45 ± 0.02 R⊙ and R2 = 0.94 ± 0.02 R⊙. A decreasing orbital period with a rate of dP/dt = −1.5 × 10−7 d yr−1 can be seen as evidence that the system is evolving into a contact binary with higher contact degree. Cyclic oscillation of the O – C data was interpreted by the Applegate mechanism and light-time effect due to an unseen component around the close binary system. The hypothetical third component is probably a fully convective red dwarf star with a minimal mass of 0.1 M⊙. CN And is at the early phase of the contact stage of its evolution and is an interesting example for studying the formation and evolution of close binaries.

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“…We listed the residuals of linear fit (O − C) 1 in the seventh column of Table 4 and plotted them in Figure 3. Qian et al (2004) and Ma et al (2018) found that there might be a cyclic variation in the O − C data of VZ Psc. We also fitted the O − C values using the linear function, LITE and magnetic activity cycle.…”

Section: Period Analysis Of Vz Pscmentioning

confidence: 99%

“…The primary and secondary components of VZ Psc were both strongly chromospherically active. Furthermore, the secondary component was more active than the primary component (Qian et al 2004). Ma et al (2018) pointed out that introducing a hot spot on the primary component and adding a third companion produced the best result for their LCs.…”

Section: Introductionmentioning

confidence: 95%

Orbital parameters and period variation studies of the short-period eclipsing binaries FG Sct, VZ Lib and VZ Psc

Yue

Zhang

Han

et al. 2019

Res. Astron. Astrophys.

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We present eight sets of new light curves for binaries FG Sct, VZ Lib and VZ Psc, which are all contact eclipsing binaries with short orbital periods. We carried out our observations from 2016 to 2017 using the 60-cm telescope administered by National Astronomical Observatories, Chinese Academy of Sciences, the Holcomb Observatory at Butler University and the SARA-CT telescope in Chile. We firstly determined the orbital parameters of FG Sct using the O − C method and obtained photometric solutions utilizing the updated W-D program. We also studied its period variation and discovered that its orbital period is decreasing at a rate of 6.39(±0.24) × 10−8 d yr−1, which was likely caused by mass transfer from the primary component to the secondary component or angular momentum interchange between the two components via magnetic interactions. For VZ Lib and VZ Psc, we simultaneously analyzed their BV RI light curves in conjunction with the published radial velocities. In order to obtain the orbital parameters of VZ Lib, we also analyzed its period variation and revised cyclic change, which could be attributed to either the light-time effect due to a tertiary companion or magnetic activity cycle mechanism. We derived the periods of the tertiary component of VZ Lib to be 48.7(±0.1) yr or magnetic cycle to be 46.9(±1.9) yr. Strong emission lines at Ca ii H+K, Hα, Hβ, Hγ and Ca ii IRT were detected in the LAMOST spectra of VZ Psc, which imply chromospheric activities in this binary system.

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Possible connection between period change and magnetic activity of the very short‐period binary VZ Piscium

Cited by 8 publications

References 14 publications

WIDE COOL AND ULTRACOOL COMPANIONS TO NEARBY STARS FROM Pan-STARRS 1

WIDE COOL AND ULTRACOOL COMPANIONS TO NEARBY STARS FROM Pan-STARRS 1

CN Andromedae: a shallow contact binary with a possible tertiary component

Orbital parameters and period variation studies of the short-period eclipsing binaries FG Sct, VZ Lib and VZ Psc

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