Orbits of Five Visual Double Stars

Docobo, J. A.; Ling, J. F.

doi:10.1086/313166

Cited by 14 publications

(4 citation statements)

References 19 publications

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“…-This system has a grade 3 orbit 3 ( Docobo & Ling 1999). Astrometry computed from the orbital elements at the time of our observations, 2001.0985, gives a separation of 0.29 00 with a position angle of 244 .…”

Section: Known Binariesmentioning

confidence: 75%

Adaptive Optics Photometry and Astrometry of Binary Stars

et al. 2005

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We carried out a search for companions to B stars using the adaptive optics system of the Advanced Electro-Optical System 3.6 m telescope. We observed 70 B stars in the I band, finding 16 companions, 10 of which are newly discovered companions. For each system with a detected companion we give its measured astrometry and differential magnitude. We then put the observation in context of the system's known multiplicity and provide a somewhat crude estimate of its spectral type based on the single differential magnitude measurement. The separations range from 0.2 00 to 7.31 00 , and the differential magnitudes range from 1:41 AE 0:01 to 10:1 AE 0:5. Finally, we present a list of the null detections and discuss the implications of null detections of selected stars.

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Section: Known Binariesmentioning

confidence: 75%

Adaptive Optics Photometry and Astrometry of Binary Stars

et al. 2005

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“…HD 37711 (WDS 05413+1632, BU 1007 ).-This system has a grade 3 orbit 3 ( Docobo & Ling 1999). Astrometry computed from the orbital elements at the time of our observations, 2001.0985, gives a separation of 0.29 00 with a position angle of 244 .…”

Section: Known Binariesmentioning

confidence: 82%

Adaptive Optics Photometry and Astrometry of Binary Stars. II. A Multiplicity Survey of B Stars

2007

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We carried out a search for companions to B stars using the adaptive optics system of the Advanced ElectroOptical System 3.6 m telescope. We observed 70 B stars in the I band, finding 16 companions, 10 of which are newly discovered companions. For each system with a detected companion we give its measured astrometry and differential magnitude. We then put the observation in context of the system's known multiplicity and provide a somewhat crude estimate of its spectral type based on the single differential magnitude measurement. The separations range from 0.2 00 to 7.31 00 , and the differential magnitudes range from 1:41 AE 0:01 to 10:1 AE 0:5. Finally, we present a list of the null detections and discuss the implications of null detections of selected stars.

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“…HD 37711 (126 Tau, HIP 26777) is a B-type star with a known visual companion. Docobo & Ling (1999) found a period of 115 yr for the highly eccentric orbit. Using speckle data compiled from WDS, Malkov et al (2012) confirmed this orbital period for the B8V+B7V system, with a high eccentricity of 0.87.…”

Section: Hd 37711mentioning

confidence: 98%

ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI

Gardner

Monnier

Fekel

et al. 2022

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We started a survey with CHARA/MIRC-X and VLTI/GRAVITY to search for low-mass companions orbiting individual components of intermediate-mass binary systems. With the incredible precision of these instruments, we can detect astrometric “wobbles” from companions down to a few tens of microarcseconds. This allows us to detect any previously unseen triple systems in our list of binaries. We present the orbits of 12 companions around early F- to B-type binaries, 9 of which are new detections and 3 of which are first astrometric detections of known radial velocity (RV) companions. The masses of these newly detected components range from 0.45 to 1.3 M ⊙. Our orbits constrain these systems to a high astrometric precision, with median residuals to the orbital fit of 20–50 μas in most cases. For seven of these systems we include newly obtained RV data, which help us to identify the system configuration and to solve for masses of individual components in some cases. Although additional RV measurements are needed to break degeneracy in the mutual inclination, we find that the majority of these inner triples are not well aligned with the wide binary orbit. This hints that higher-mass triples are more misaligned compared to solar and lower-mass triples, though a thorough study of survey biases is needed. We show that the ARMADA survey is extremely successful at uncovering previously unseen companions in binaries. This method will be used in upcoming papers to constrain companion demographics in intermediate-mass binary systems down to the planetary-mass regime.

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Orbits of Five Visual Double Stars

Abstract: This paper revises and discusses the orbits and other parameters of the double stars WDS

Cited by 14 publications

References 19 publications

Adaptive Optics Photometry and Astrometry of Binary Stars

Adaptive Optics Photometry and Astrometry of Binary Stars

Adaptive Optics Photometry and Astrometry of Binary Stars. II. A Multiplicity Survey of B Stars

ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI

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