Achromatic double-star interferometry.

Wickes, W. C.; Dicke, R. H.

doi:10.1086/111697

Cited by 15 publications

(7 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%

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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%

“…A photoelectric modernization of the Anderson-Finsen version of the Michelson interferometer was devised and demonstrated by Wickes & Dicke (227,228). This approach offers the significant improvements over visual interfe rometry of being impersonal and yielding magnitude dif fe rences.…”

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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“…Torres et al (2002) argue that abundance estimates for a binary are affected by the presence of the secondary in both photometric and spectroscopic measurement techniques. However, Wickes & Dicke (1974) measured the system's Ám ¼ 5:5 AE 0:7 at k ¼ 0:55 m, limiting the secondary's influence of these estimates to no more than $0.05 dex, basically undetectable. Second, the abundance analysis by Thévenin & Idiart (1999) provides substantial evidence that it is imperative to use non-LTE (NLTE) treatment when measuring stars with subsolar abundances.…”

Section: Stellar Modelsmentioning

confidence: 99%

Angular Diameters of the G Subdwarf μ Cassiopeiae A and the K Dwarfs σ Draconis and HR 511 from Interferometric Measurements with the CHARA Array

Boyajian

McAlister

Baines

et al. 2008

Astrophysical Journal

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Using the longest baselines of the CHARA Array, we have measured the angular diameter of the G5 V subdwarf Cas A, the first such determination for a halo population star. We compare this result to new diameters for the higher metallicity K0 V stars, Dra and HR 511, and find that the metal-poor star, Cas A, has an effective temperature (T eA ¼ 5297 AE 32 K), radius (R ¼ 0:791 AE 0:008 R ), and absolute luminosity (L ¼ 0:442 AE 0:014 L ) comparable to those of the other two stars with later spectral types. We show that stellar models show a discrepancy in the predicted temperature and radius for Cas A, and we discuss these results and how they provide a key to understanding the fundamental relationships for stars with low metallicity.

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“…Since Wagman (1961) discovered the binarity of µ Cas from the variable proper motion, a series of astrometric observations of the parallax and orbital parameters has been continued. In earlier studies, the position angle and the separation of the system were measured by double-aperture interferometry (Wickes & Dicke 1974;Wickes 1975) and by narrow-band photography (Feibelman 1976). Through compilation of several decades of photometry, this nearby (∼ 7.5 pc) binary system is found to have a priod of P ∼ 22 years (Wagman et al 1963;Lippincott & Wyckoff 1964;Lippincott 1981;Russell & Gatewood 1984).…”

Section: Fundamental Parametersmentioning

confidence: 99%

Evolutionary Status and Internal Structure of Μ Cassiopeiae

Bach¹

2015

Journal of The Korean Astronomical Society

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We investigate physical properties of the nearby (∼ 7.5 pc) astrometric binary µ Cas in the context of standard evolutionary theory. Based on the spectroscopically determined relative abundances ([α/Fe] +0.4 dex, [Fe/H] ∼ −0.7 dex), all physical inputs such as opacities and equation of state are consistently generated. By combining recent spectroscopic analyses with the astrometric observations from the HIPPARCOS parallaxes and the CHARA array, the evolutionary model grids have been constructed. Through the statistical evaluation of the χ 2 -minimization among alternative models, we find a reliable evolutionary solution (M A , M B , t age ) = (0.74 M ⊙ , 0.19 M ⊙ , 11 Gyr) which excellently satisfies observational constraints. In particular, we find that the helium abundance of µ Cas is comparable with the primordial helium contents (Y p ∼ 0.245). On the basis of the well-defined stellar parameters of the primary star, the internal structure and the p-mode frequencies have been estimated. From our seismic computation, µ Cas is expected to have a first order spacing ∆ν ∼ 169 µHz. The ultimate goal of this study is to describe physical processes inside a low-mass star through a complete modelling from the spectroscopic observation to the evolutionary computation.

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Achromatic double-star interferometry.

Cited by 15 publications

References 0 publications

High Angular Resolution Measurements of Stellar Properties

High Angular Resolution Measurements of Stellar Properties

Angular Diameters of the G Subdwarf μ Cassiopeiae A and the K Dwarfs σ Draconis and HR 511 from Interferometric Measurements with the CHARA Array

Evolutionary Status and Internal Structure of Μ Cassiopeiae

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