Interferometric measurements of binary stars

Wickes, W. C.

doi:10.1086/111790

Cited by 11 publications

(6 citation statements)

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“…McCarthy (149) has used the advantages of infrared speckle interferometry to increase the relative brightness of the secondary to about 5% of that of the primary, causing a visibility modulation of about 10%. These results confirm the previous marginal resolutions at visible wavelengths (100,225,228) and provide mass determinations with uncertainties of ± 25%. The orbit is still known with too little precision to contribute new data to the question of the primordial helium abundance.…”

Section: Hr 321 ()L Cas)supporting

confidence: 90%

“…This approach offers the significant improvements over visual interfe rometry of being impersonal and yielding magnitude dif fe rences. The instrument was applied to a small number of field visual binaries (including the first direct resolution of the systems rx Del A and the Population II star J.l Cas) and several Hyades binaries (225,226), but its use was discontinued after this promising beginning. A modified version of the Wickes-Dicke interferometer has been developed by Tokovinin (203), who calls the device a "phase-grating stellar interferometer."…”

Section: Interferometric Measurements Of Binary Starsmentioning

confidence: 99%

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High Angular Resolution Measurements of Stellar Properties

McAlister¹

1985

Annu. Rev. Astron. Astrophys.

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Section: Hr 321 ()L Cas)supporting

confidence: 90%

Section: Interferometric Measurements Of Binary Starsmentioning

confidence: 99%

High Angular Resolution Measurements of Stellar Properties

McAlister¹

1985

Annu. Rev. Astron. Astrophys.

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“…In all cases splines were used to interpolate between the table values. In addition to the ∆R and ∆I data obtained from this run at SOR, ∆V measurements were located in the literature (Baize 1950, Dombrowski 1990, Muller 1949, Wickes 1975, Worley 1969, most provided by the Catalog of Photometric Magnitude Differences (maintained at the USNO).…”

Section: Discussionmentioning

confidence: 99%

Differential Binary Star Photometry Using the Adaptive Optics System at Starfire Optical Range

Brummelaar¹,

Mason²,

Bagnuolo³

et al. 1996

The Astronomical Journal

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As part of an NSF effort to make the Starfire Optical Range 1.5-m telescope, equipped with laser guide star and adaptive optics, available to the astronomical community, several nights in May and October of 1995 were awarded to the CHARA group in order to perform differential photometry on close binary stars. Images were acquired in two near-IR pass bands of over twenty pairs and reduced by fitting both the point spread function (PSF) and the positions and intensities of the stars. The ∆m values were calibrated using ten stars for which combined I and R photometric data were available in the literature.Color indices have been calculated for the individual components of these stars, allowing for the determination of spectral classifications of both components in seven of the systems.

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“…the astrometric orbit should give the total mass of the system, as well as the optical magnitude difference of 5.5 mag. The resolution was confirmed in another interferometric observation a year later (Wickes 1975), but orbital motion had reduced the separation to only 0. ′′ 23.…”

mentioning

confidence: 77%

Hubble Space Telescope Astrometry of the Metal-Poor Visual Binary $μ$ Cassiopeiae: Dynamical Masses, Helium Content, and Age

Bond,

Schaefer,

Gilliland

et al. 2020

Preprint

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µ Cassiopeiae is a nearby, high-velocity, metal-poor ([Fe/H] = −0.81) visual binary. We have used highresolution imaging with the Hubble Space Telescope (HST), obtained over nearly two decades, to determine the period (21.568 yr) and precise orbital elements. Combining these with published ground-and space-based astrometry, we determined dynamical masses for both components of µ Cas: 0.7440 ± 0.0122 M ⊙ for the G5 V primary, and 0.1728 ± 0.0035 M ⊙ for its faint dM companion. We detect no significant perturbations in the HST astrometry due to a third body in the system. The primary aim of our program was to determine, with the aid of stellar models, the helium content and age of the metal-deficient primary star, µ Cas A. Although we now have a precise mass, there remain uncertainties about other parameters, including its effective temperature. Moreover, a re-examination of archival interferometric observations leads to a suspicion that the angular diameter was overestimated by a few percent. In the absolute magnitude versus color plane, µ Cas A lies slightly cooler and more luminous than the main sequence of the globular cluster 47 Tucanae; this may imply that the star has a lower helium content, and/or is older, and/or has a higher metallicity, than the cluster. Our best estimates for the helium content and age of µ Cas A are Y = 0.255 ± 0.014 and 12.7 ± 2.7 Gyr-making µ Cas possibly the oldest star in the sky visible to the naked eye. Improved measurements of the absolute parallax of the system, the effective temperature of µ Cas A, and its angular diameter would provide tighter constraints.

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Interferometric measurements of binary stars

Cited by 11 publications

References 0 publications

High Angular Resolution Measurements of Stellar Properties

High Angular Resolution Measurements of Stellar Properties

Differential Binary Star Photometry Using the Adaptive Optics System at Starfire Optical Range

Hubble Space Telescope Astrometry of the Metal-Poor Visual Binary $μ$ Cassiopeiae: Dynamical Masses, Helium Content, and Age

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