CCD Speckle Observations of Binary Stars With the Wiyn Telescope. Vi. Measures During 2007-2008

Horch, Elliott; Falta, David; Anderson, Lisa M.; DeSousa, Michael D.; Miniter, Craig M.; Ahmed, Tasmia; Altena, W. F. van

doi:10.1088/0004-6256/139/1/205

Cited by 253 publications

(50 citation statements)

References 28 publications

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“…25) at the time of discovery and they are coded as solution Figures 1-4 give the apparent orbits and predicted radial velocity (RV) curves for these HDS binaries. The apparent orbits represented by solid lines are those for which the elements are given in Table 1, whereas the orbits represented by dashed lines are those previously announced in Cvetković (2013) and in Horch et al (2010) The predicted RV curves are based on the orbital elements presented here, the distances following from the Hipparcos parallaxes, and the mass ratios following from the individual masses (Table 2). In these plots the solid lines correspond to the primaries and the dashed lines correspond to the secondaries.…”

Section: Resultsmentioning

confidence: 88%

“…Due to this, which is especially reflected in σ M B (Table 2), and the fact that both components are G stars, the spectral types are estimated with high uncertainty. The composite spectrum given in the SIMBAD database is G5 and the B − V color index (ESA 1997) corresponds to G8, (Horch et al 2010) is shown as a dashed line. Bottom: predicted radial velocities for HDS 3158 (left) and HDS 3315 (right); the solid lines correspond to the primaries, whereas the dashed lines correspond to the secondaries.…”

Section: Individual Systemsmentioning

confidence: 99%

“…The orbits have been previously announced in the IAU Commission 26 Information Circular (Cvetković 2012(Cvetković , 2013. Except for HDS 3158, for which the first orbit was published in Horch et al (2010), for the remaining seven HDS binaries the orbital elements are calculated for the first time.…”

Section: Introductionmentioning

confidence: 99%

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ORBITS FOR EIGHTHIPPARCOSDOUBLE STARS

Cvetković

Pavlović

Ninković

2014

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In this paper, we analyze new orbital elements and the quantities that follow from them for eight binaries: WDS 00101+3825 = HDS 23Da,Db, WDS 00321−1218 = HDS 71, WDS 04287+2613 = HDS 576, WDS 04389−1207 = HDS 599, WDS 16206+4535 = HDS 2309, WDS 17155+1052 = HDS 2440, WDS 22161−0705 = HDS 3158, and WDS 23167+3441 = HDS 3315. For seven of them, the orbital elements are calculated for the first time. Binaries, denoted as HDS, were discovered during the Hipparcos mission, and their first observational epoch is 1991.25, the same as the mean epoch of the Hipparcos catalog. We found all other measurements of these binaries in databases. They were obtained in the last 15 yr using the speckle interferometric technique. All studied pairs are close, and all measured separations are less than 0. 4. The resulting orbital periods fall within 26 and 80 yr. In addition to the orbital elements, we also give (O − C) residuals in θ and ρ, masses, dynamical parallaxes, absolute magnitudes, spectral types, and ephemerides for the next 5 yr.

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Section: Resultsmentioning

confidence: 88%

Section: Individual Systemsmentioning

confidence: 99%

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ORBITS FOR EIGHTHIPPARCOSDOUBLE STARS

Cvetković

Pavlović

Ninković

2014

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“…First we have collected observational data of HD 87646 from the literature (Horch et al 2008, Hartkopf & Mason 2009, Horch et al 2010, Balega et al 2013) and combined them with our AO data to constrain the binary orbit of HD 87646. Our best fitting binary orbital solution (solid line) and the observational data (black dots) are shown in Fig.…”

Section: Dynamical Stability Of Hd 87646mentioning

confidence: 99%

Very Low-Mass Stellar and Substellar Companions to Solar-Like Stars From Marvels. Vi. A Giant Planet and a Brown Dwarf Candidate in a Close Binary System Hd 87646

Wolszczan

et al. 2016

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We report the detections of a giant planet (MARVELS-7b) and a brown dwarf candidate (MARVELS-7c) around the primary star in the close binary system, HD 87646. It is the first close binary system with more than one substellar circum-primary companion discovered to the best of our knowledge. The detection of this giant planet was accomplished using the first multi-object Doppler instrument (KeckET) at the Sloan Digital Sky Survey (SDSS) telescope. Subsequent radial velocity observations using ET at Kitt Peak National Observatory, HRS at HET, the "Classic" spectrograph at the Automatic Spectroscopic Telescope at Fairborn Observatory, and MARVELS from SDSS-III confirmed this giant planet discovery and revealed the existence of a long-period brown dwarf in this binary. HD 87646 is a close binary with a separation of ∼ 22 AU between the two stars, estimated using the Hipparcos catalogue and our newly acquired AO image from PALAO on the 200-inch Hale Telescope at Palomar. The primary star in the binary, HD 87646A, has T eff = 5770± 80K, log g =4.1±0.1 and [Fe/H] = −0.17 ± 0.08. The derived minimum masses of the two substellar companions of HD 87646A are 12.4±0.7 M Jup and 57.0±3.7 M Jup . The periods are 13.481±0.001 days and 674±4 days and the measured eccentricities are 0.05±0.02 and 0.50±0.02 respectively. Our dynamical simulations show the system is stable if the binary orbit has a large semi-major axis and a low eccentricity, which can be verified with future astrometry observations.

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“…These images were obtained in the R (6920 Å) and I (8800 Å) bands. Data reduction and analysis of these images are described in Torres et al (2011), Horch et al (2010), and Howell et al (2011. The reconstructed R-and Iband images reveal no stellar companions brighter than DR 4.5 mag and DĨ 3.5 mag, within the annulus from 0″ .…”

Section: Speckle Imagingmentioning

confidence: 99%

Kepler-432: A Red Giant Interacting With One of Its Two Long-Period Giant Planets

Quinn

White

Latham

et al. 2015

ApJ

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We report the discovery of Kepler-432b, a giant planet ( = 3.9 days), and adaptive optics imaging revealed a nearby (  0. 87), faint companion (Kepler-432B) that is a physically bound M dwarf. The host star exhibits high signal-to-noise ratio asteroseismic oscillations, which enable precise measurements of the stellar mass, radius, and age. Analysis of the rotational splitting of the oscillation modes additionally reveals the stellar spin axis to be nearly edge-on, which suggests that the stellar spin is likely well aligned with the orbit of the transiting planet. Despite its long period, the obliquity of the 52.5 day orbit may have been shaped by star-planet interaction in a manner similar to hot Jupiter systems, and we present observational and theoretical evidence to support this scenario. Finally, as a short-period outlier among giant planets orbiting giant stars, study of Kepler-432b may help explain the distribution of massive planets orbiting giant stars interior to 1 AU.-

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CCD Speckle Observations of Binary Stars With the Wiyn Telescope. Vi. Measures During 2007-2008

Cited by 253 publications

References 28 publications

ORBITS FOR EIGHTHIPPARCOSDOUBLE STARS

ORBITS FOR EIGHTHIPPARCOSDOUBLE STARS

Very Low-Mass Stellar and Substellar Companions to Solar-Like Stars From Marvels. Vi. A Giant Planet and a Brown Dwarf Candidate in a Close Binary System Hd 87646

Kepler-432: A Red Giant Interacting With One of Its Two Long-Period Giant Planets

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