Contact Binaries with Additional Components. III. A Search Using Adaptive Optics

Ruciński, S. M.; Pribulla, T.; Kerkwijk, M. H. van

doi:10.1086/523353

Cited by 113 publications

(84 citation statements)

References 25 publications

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“…Note that Qian et al (2004) suggest a closer companion to the binary may be causing a variation in the light curve with a period of ∼25 yr. However, no close companion was identified by Rucinski et al (2007), and our companion is too wide to introduce such a short period variation.…”

Section: Hip 115819 (Vz Piscium)mentioning

confidence: 77%

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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: 77%

“…As angular momentum transfer to additional components can tighten an inner binary and lead to contact, Rucinski et al (2007) observed VZ Piscium as part of an adaptive optics search for companions to contact binaries. We have identified an M8 companion at a separation of 30 .…”

Section: Hip 115819 (Vz Piscium)mentioning

confidence: 99%

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

Deacon

Liu

Magnier

et al. 2014

ApJ

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“…Yang & Liu (2003) considered both mass exchange and mass loss mechanisms that could cause the observed decrease in the period but found that the cyclic variation superimposed on the decreasing trend was quasi-periodic; hence, it could only be attributed to magnetic activity. Pribulla & Rucinski (2006) and Rucinski et al (2007) did not detect the signature of a third body in their studies dedicated to detecting faint third bodies in contact binary systems. In addition, broadening functions constructed for radial velocity analysis by Pribulla et al (2009a) did not show any evidence of a third companion in the system.…”

Section: Rw Commentioning

confidence: 97%

Physical parameters of close binaries QX Andromedae, RW Comae Berenices, MR Delphini, and BD +07° 3142

Djurašević

Yılmaz

Baştürk

et al. 2010

A&A

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Aims. We analyze new multicolor light curves and recently published radial velocity curves for close binaries QX And, RW Com, MR Del, and BD +07 • 3142 to determine the physical parameters of the components. Methods. The light curves are analyzed using a binary star model based on Roche geometry to fit the photometric observations. Spectroscopic parameters, such as the mass ratios and spectral types, were taken from recent spectroscopic studies of the systems in question. Results. Our findings provide consistent and reliable sets of stellar parameters for the four studied binary systems. Of particular interest is the BD +07 • 3142 system, since this is the first analysis of its light curves. We find that it is an overcontact binary of W UMa type and W subtype, and that each component has a large cool spot in the polar region. QX And is an A subtype, and RW Com a W subtype W UMa binary, and in both systems we find a bright spot in the neck region between the components. MR Del is a detached binary with a complex light curve that we could model with two cool spots on the hotter component.

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“…D 'Angelo et al (2006) analyzed 4000 spectra from 75 close binaries for spectroscopic signature of tertiaries and identified 23 triple systems (almost one third). Rucinski et al (2007) presented the results of a search for TC of a group of contact binaries and concluded that the presence of a close component is a very common phenomenon for very close binaries with orbital period , 1 day.…”

Section: Introductionmentioning

confidence: 99%

A Model for Contact Binary EP Andromedae

Manzoori¹

2012

Publ. – Astron. Soc. Aust

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This paper presents the first comprehensive study of the EP And system, a contact binary. In this work the solution of the standard V light curve was obtained using the PHOEBE program (version 0.3c). Absolute parameters of the stellar components were then determined, enabling us to discuss the structure and evolutionary status of the close binary EP And. The times of minima data ('OÀC curve') were analyzed. It was found that a third body with a period of 41.20 yr and mass 0.15 M } is orbiting around the system. Also a modulating period of an 11.72-yr cycle along with a relative period increase of DP P ¼ 1:79 Â 10 À7 were obtained, which were attributed to the magnetic activity cycle and mass transfer with rate Dm m ¼ 9:98 Â 10 À8 yr À1 between the components, respectively.

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Contact Binaries with Additional Components. III. A Search Using Adaptive Optics

Cited by 113 publications

References 25 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

Physical parameters of close binaries QX Andromedae, RW Comae Berenices, MR Delphini, and BD +07° 3142

A Model for Contact Binary EP Andromedae

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