The two variables in the triple system HR 6469 = V819 Her: One eclipsing, one spotted

Hamme, W. Van; Hall, D. S.; Hargrove, Adam W.; Henry, Gregory W.; Wasson, R.; Barkslade, W. S.; Chang, Suyon; Fried, Robert; Green, C. L.; Lines, H. C.; Lines, R. D.; Nielsen, P.; Powell, H. D.; Reisenweber, R. C.; Rogers, C. W.; Shervais, Stephen; Tatum, Randy

doi:10.1086/116962

Cited by 9 publications

(7 citation statements)

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“…This very interesting system was the subject of three papers published at the same time (Wasson et al;Van Hamme et al;Scarfe et al 1994) in the same journal.…”

Section: General Casesmentioning

confidence: 95%

“…The evolved G5 star is referred to as the primary and has a period of variability of about 83 days in V, while the secondary is taken as the brighter star of the close eclipsing pair, whose period is 2.23 days (Van Hamme 1994). The duplicity of the second component could not be seen by Hipparcos, and the double variability phenomenon (eclipse + spotted variable) entails reasonably small change of the magnitude (< 0.09 mag), so the set of Hipparcos observations may be considered as photometrically homogeneous, at least for the purpose of this study.…”

Section: General Casesmentioning

confidence: 99%

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Mass determination of astrometric binaries with Hipparcos

Märtin

Mignard

Hartkopf

et al. 1998

Astron. Astrophys. Suppl. Ser.

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Abstract. This paper is the third of a series devoted to the determination of stellar masses from Hipparcos data. This is a continuation of Martin et al. (1997), who introduced the theory and assessed the performance of the method from simulated data, and of a second paper with the first results for 46 systems, (Martin & Mignard 1998). The orbit file maintained by the CHARA group and new publications of orbital elements made the processing of 70 additional candidate systems possible, including 28 of the 145 systems already tested in the previous work. Significant results were obtained on 22 systems, with relative accuracy better than 25% for the masses of 17 binaries. New estimates are also given for 6 systems previously investigated, thanks to reliable values of the magnitude difference from the Hipparcos catalogue (ESA 1997). New orbital elements are proposed for HIP 12623 (12 Persei) from speckle/spectroscopic measurements. Results are discussed for each system, alongside the mass-luminosity relation based on Hipparcos magnitudes and distances.

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“…This very interesting system was the subject of three papers published at the same time (Wasson et al;Van Hamme et al;Scarfe et al 1994) in the same journal.…”

Section: General Casesmentioning

confidence: 95%

Section: General Casesmentioning

confidence: 99%

Mass determination of astrometric binaries with Hipparcos

Märtin

Mignard

Hartkopf

et al. 1998

Astron. Astrophys. Suppl. Ser.

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“…Using the published sizes and temperatures for Ba and Bb from van Hamme et al (1994), it is found that the magnitude of the astrometric shift in CL position during eclipse compared to what it would be outside of eclipse can be greater than 100 µas. Because this shift is larger than PHASES astrometric measurement precisions, six measurements taken during eclipse are omitted from the data tables and the fits.…”

Section: Phases Observations During Ba-bb Eclipsesmentioning

confidence: 99%

“…The close pair (Ba and Bb) is in an edge-on orbit and exhibits shallow eclipses. A combination of radial velocity, speckle interferometry, eclipse timing and light-curve fitting has made it possible to accurately determine most of the interesting system parameters, including masses, radii and distance (Scarfe et al 1994;van Hamme et al 1994;Wasson et al 1994) with accuracies of a few percent. However, until now it has not been possible to determine the mutual inclination of the orbits.…”

Section: Introductionmentioning

confidence: 99%

PHASES differential astrometry and the mutual inclination of the V819 Herculis triple star system

Muterspaugh

Lane

Konacki

et al. 2006

A&A

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V819Herculis is a well-studied triple star system consisting of a "wide" pair with 5.5 year period, one component of which is a 2.2-day period eclipsing single-line spectroscopic binary. Differential astrometry measurements from the Palomar High-precision Astrometric Search for Exoplanet Systems (PHASES) are presented and used to determine a relative inclination between the short-and long-period orbits of 23.6 ± 4.9 degrees. This represents only the sixth unambiguous determination of the mutual inclination of orbits in a hierarchical triple system. This result is combined with those for the other five systems for analysis of the observed distribution of mutual inclinations in nearby triple systems. It is found that this distribution is different than that which one would expect from random orientations with statistical significance at the 94% level; implications for studying the spatial distribution of angular momentum in star forming regions is discussed.

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“…The star HIP 84949 = V819 Her is a complex triple system. The inner binary is eclipsing of Algol type with a period of 2.23 d. The outer companion of G8IV-III type is an active spotty star rotating with a period of about 86 d (van Hamme et al 1994). It can hardly be a coincidence that our best NDAC solution produced a period of 89 d. In a binary system with a variable component, the photocenter moves along the line connecting the components synchronously with the light curve, the effect known as Variability Imposed Movers (VIM).…”

Section: Unconstrained Solutions For Stochastic Starsmentioning

confidence: 99%

Unconstrained Astrometric Orbits for Hipparcos Stars with Stochastic Solutions

Goldin

Макаров

2006

ASTROPHYS J SUPPL S

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A considerable number of astrometric binaries whose positions on the sky do not obey the standard model of mean position, parallax and linear proper motion, were observed by the Hipparcos satellite. Some of them remain non-discovered, and their observational data have not been properly processed with the more adequate astrometric model that includes nonlinear orbital motion. We develop an automated algorithm based on "genetic optimization", to solve the orbital fitting problem in the most difficult setup, when no prior information about the orbital elements is available (from, e.g., spectroscopic data or radial velocity monitoring). We also offer a technique to accurately compute the probability that an orbital fit is bogus, that is, that an orbital solution is obtained for a single star, and to estimate the probability distributions for the fitting orbital parameters. We test this method on Hipparcos stars with known orbital solutions in the catalog, and further apply it to 1561 stars with stochastic solutions, which may be unresolved binaries. At a confidence level of 99%, orbital fits are obtained for 65 stars, most of which have not been known as binary. It is found that reliable astrometric fits can be obtained even if the period is somewhat longer than the time span of the Hipparcos mission, i.e., if the orbit is not closed. A few of the new probable binaries with A-type primaries with periods 444-2015 d are chemically peculiar stars, including Ap and λ Boo type. The anomalous spectra of these stars are explained as admixture of the light from the unresolved, sufficiently bright and massive companions. We estimate the apparent orbits of four stars which have been identified as members of the ≈ 300 Myr-old UMa kinematic group. Another four new nearby binaries may include low-mass M-type or brow dwarf companions. Follow-up spectroscopic observations in conjunction with 25 +32−13

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The two variables in the triple system HR 6469 = V819 Her: One eclipsing, one spotted

Cited by 9 publications

References 0 publications

Mass determination of astrometric binaries with Hipparcos

Mass determination of astrometric binaries with Hipparcos

PHASES differential astrometry and the mutual inclination of the V819 Herculis triple star system

Unconstrained Astrometric Orbits for Hipparcos Stars with Stochastic Solutions

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