Orbits of new Hipparcos binaries. I

Балега, И. И.; Balega, Yu. Yu.; Hofmann, Karl H.; Pluzhnik, Eugene; Schertl, D.; Shkhagosheva, Z. U.; Weigelt, G.

doi:10.1051/0004-6361:20041190

Cited by 42 publications

(43 citation statements)

References 19 publications

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“…Using the 2004 observations and the newest 2006 measurements, we can derive orbital parameters for two more Hipparcos binaries: HIP 109281 and HIP 116259. The method of orbit computation is described in our previous paper (Balega et al, 2005). New relative orbits of the systems are plotted in fig.…”

Section: Observations and Resultsmentioning

confidence: 99%

Speckle interferometry of nearby multiple stars. IV. Measurements in 2004 and new orbits

et al. 2007

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Abstract. The results of speckle interferometric observations of 104 binary and 6 triple stars performed at the BTA 6 m telescope in 2004 October are presented. Nearby low-mass stars are mostly observed for the program, among which 59 there are new binaries recently discovered by the Hipparcos astrometric satellite. Concurrently with the diffraction-limited position measurements we obtained 154 brightness ratio measurements of binary and multiple star components in different bands of the visible spectrum. New, first-resolved binaries are the symbiotic star CH Cyg with a weak companion at 0.043 ′′ separation and the pair of red dwarfs, GJ 913 = HIP 118212. In addition, we derived the orbital parameters for two interferometric systems: the CN-giant pair HD 210211 = HIP 109281 (P=10.7 yr) and the G2V-K2V binary GJ 9830 = HIP 116259 (P=15.7 yr).

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Section: Observations and Resultsmentioning

confidence: 99%

Speckle interferometry of nearby multiple stars. IV. Measurements in 2004 and new orbits

et al. 2007

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“…Mason et al (1993) presented a few other measurements but also noted that it was undetected 8 times. It was also undetected by Balega et al (1994). McAlister et al (1989) said that the peaks of the autocorrelation are weak and indicative of a large dynamic range, which would only be detected under ideal seeing conditions.…”

Section: Newly Discovered Companionsmentioning

confidence: 99%

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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“…A1918b : Aitken (1918); Abt2006: Abt & Willmarth (2006); AST1999: Franz et al (1999); AST2001: Benedict et al (2001); B1960c: van den Bos (1960); Bag2005: Balega et al (2005); Baz1980b: Baize (1980); Chg1972: Chang (1972); CIA2010: Farrington et al (2010); Cou1960b: Couteau (1960; Doc1985c: Docobo & Costa (1985); Doc2008d: Docobo et al (2008); Doc2010d: Docobo & Ling (2010); Dom1978: Dommanget (1978; Dru1995: Drummond et al (1995); Duq1991b: Duquennoy et al (1991 Egg1956: Eggen (1956; Egn2008: Eggenberger et al (2008); Fek1983: Fekel & Tomkin (1983 FMR2008b: Rica Romero (2008 Frv1999: Forveille et al (1999; Gri1975: Griffin & Emerson (1975); Gri1998: Griffin (1998) Acknowledgements. We dedicate this paper to the memory of J. Dommanget, who initiated this study and could unfortunately not see it accomplished.…”

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Are the orbital poles of binary stars in the solar neighbourhood anisotropically distributed?

Agati

Bonneau

Jorissen

et al. 2015

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We test whether or not the orbital poles of the systems in the solar neighbourhood are isotropically distributed on the celestial sphere. The problem is plagued by the ambiguity on the position of the ascending node. Of the 95 systems closer than 18 pc from the Sun with an orbit in the 6th Catalogue of Orbits of Visual Binaries, the pole ambiguity could be resolved for 51 systems using radial velocity collected in the literature and CORAVEL database or acquired with the HERMES/Mercator spectrograph. For several systems, we can correct the erroneous nodes in the 6th Catalogue of Orbits and obtain new combined spectroscopic/astrometric orbits for seven systems [WDS 01083+5455Aa,Ab; 01418+4237AB; 02278+0426AB (SB2); 09006+4147AB (SB2); 16413+3136AB; 17121+4540AB; 18070+3034AB]. We used of spherical statistics to test for possible anisotropy. After ordering the binary systems by increasing distance from the Sun, we computed the false-alarm probability for subsamples of increasing sizes, from N = 1 up to the full sample of 51 systems. Rayleigh-Watson and Beran tests deliver a false-alarm probability of 0.5% for the 20 systems closer than 8.1 pc. To evaluate the robustness of this conclusion, we used a jackknife approach, for which we repeated this procedure after removing one system at a time from the full sample. The false-alarm probability was then found to vary between 1.5% and 0.1%, depending on which system is removed. The reality of the deviation from isotropy can thus not be assessed with certainty at this stage, because only so few systems are available, despite our efforts to increase the sample. However, when considering the full sample of 51 systems, the concentration of poles toward the Galactic position l = 46.0• , b = 37• , as observed in the 8.1 pc sphere, totally vanishes (the Rayleigh-Watson false-alarm probability then rises to 18%).

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Orbits of new Hipparcos binaries. I

Cited by 42 publications

References 19 publications

Speckle interferometry of nearby multiple stars. IV. Measurements in 2004 and new orbits

Speckle interferometry of nearby multiple stars. IV. Measurements in 2004 and new orbits

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

Are the orbital poles of binary stars in the solar neighbourhood anisotropically distributed?

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