Charge-Coupled Device Speckle Observations of Binary Stars With the Wiyn*
                Telescope. V. Measures During 2001–2006

Horch, Elliott; Altena, W. F. van; Cyr, William M.; Kinsman-Smith, Lori; Srivastava, A. N.; Zhou, Jing

doi:10.1088/0004-6256/136/1/312

Cited by 86 publications

(31 citation statements)

References 21 publications

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“…This binary was then first observed in speckle interferometry by (Horch et al 2008) and many times after that; Table A.5 provides the astrometric observation as well as the magnitude difference between the two components which is Δm V = 0.88 ± 0.05. This difference corresponds to a visual brightness ratio E B /E A = 0.4446 ± 0.0205.…”

Section: From the Literaturementioning

confidence: 99%

A seismic and gravitationally bound double star observed byKepler

Appourchaux

Antia

Ball

et al. 2015

A&A

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Context. Solar-like oscillations have been observed by Kepler and CoRoT in many solar-type stars, thereby providing a way to probe stars using asteroseismology. Aims. The derivation of stellar parameters has usually been done with single stars. The aim of the paper is to derive the stellar parameters of a double-star system (HIP 93511), for which an interferometric orbit has been observed along with asteroseismic measurements. Methods. We used a time series of nearly two years of data for the double star to detect the two oscillation-mode envelopes that appear in the power spectrum. Using a new scaling relation based on luminosity, we derived the radius and mass of each star. We derived the age of each star using two proxies: one based upon the large frequency separation and a new one based upon the small frequency separation. Using stellar modelling, the mode frequencies allowed us to derive the radius, the mass, and the age of each component. In addition, speckle interferometry performed since 2006 has enabled us to recover the orbit of the system and the total mass of the system. Results. From the determination of the orbit, the total mass of the system is 2.34 +0.45 −0.33 M . The total seismic mass using scaling relations is 2.47 ± 0.07 M . The seismic age derived using the new proxy based upon the small frequency separation is 3.5 ± 0.3 Gyr. Based on stellar modelling, the mean common age of the system is 2.7-3.9 Gyr. The mean total seismic mass of the system is 2.34-2.53 M consistent with what we determined independently with the orbit. The stellar models provide the mean radius, mass, and age of the stars as R A = 1.82−1.87 R , M A = 1.25−1.39 M , Age A = 2.6-3.5 Gyr; R B = 1.22−1.25 R , M B = 1.08−1.14 M , Age B = 3.35-4.21 Gyr. The models provide two sets of values for Star A: [1.25-1.27] M and [1.34-1.39] M . We detect a convective core in Star A, while Star B does not have any. For the metallicity of the binary system of Z ≈ 0.02, we set the limit between stars having a convective core in the range [1.14-1.25] M .

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Section: From the Literaturementioning

confidence: 99%

A seismic and gravitationally bound double star observed byKepler

Appourchaux

Antia

Ball

et al. 2015

A&A

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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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“…Photometric results are found in Horch et al (2004Horch et al ( , 2008, and span the time frame of 1997 through 2006. During that interval, two different speckle systems were used, though usually with the same CCD that was used in the Lowell-Tololo observations.…”

Section: Observations and Analysismentioning

confidence: 99%

“…Our group has also done a substantial amount of small-aperture speckle interferometry, mainly in the Southern Hemisphere, from both the 0.76 m telescope at El Leoncito, Argentina (Horch et al 1996(Horch et al , 2006b) and 0.60 m telescopes at Las Campanas and Cerro Tololo, Chile, e.g., Horch et al (2006a) and references therein. We have also contributed a substantial number of measures from the WIYN 3.5 m Telescope, the most recent group of which is detailed in Horch et al (2008).…”

Section: Introductionmentioning

confidence: 99%

“…For example, magnitude difference measures of subarcsecond binaries obtained with the RIT-Yale Tip-Tilt Speckle Imager (RYTSI) at the WIYN 3.5 m Telescope have an average precision of 0.10 mag per two-minute observation (Horch et al 2008). RYTSI uses a large-format CCD detector as the image capture device, as detailed in Meyer et al (2006).…”

Section: Introductionmentioning

confidence: 99%

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A Photometric Analysis of Seventeen Binary Stars Using Speckle Imaging

Davidson

Baptista

Horch

et al. 2009

The Astronomical Journal

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199

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Magnitude differences obtained from speckle imaging are used in combination with other data in the literature to place the components of binary star systems on the H-R diagram. Isochrones are compared with the positions obtained, and a best-fit isochrone is determined for each system, yielding both masses of the components as well as an age range consistent with the system parameters. Seventeen systems are studied, 12 of which were observed with the 0.6 m Lowell-Tololo Telescope at Cerro Tololo Inter-American Observatory and six of which were observed with the WIYN 3.5 m Telescope (The WIYN Observatory is a joint facility of the University of Wisconsin-Madison, Indiana University, Yale University, and the National Optical Astronomy Observatories) at Kitt Peak. One system was observed from both sites. In comparing photometric masses to mass information from orbit determinations, we find that the photometric masses agree very well with the dynamical masses, and are generally more precise. For three systems, no dynamical masses exist at present, and therefore the photometrically determined values are the first mass estimates derived for these components.

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Charge-Coupled Device Speckle Observations of Binary Stars With the Wiyn* Telescope. V. Measures During 2001–2006

Cited by 86 publications

References 21 publications

A seismic and gravitationally bound double star observed byKepler

A seismic and gravitationally bound double star observed byKepler

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

A Photometric Analysis of Seventeen Binary Stars Using Speckle Imaging

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