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Statistics of spectroscopic sub-systems in visual multiple stars
A large sample of visual multiples of spectral types F5-M has beensurveyed for the presence of spectroscopic sub-systems. Some 4200 radialvelocities of 574 components were measured in 1994-2000 with thecorrelation radial velocity meter. A total of 46 new spectroscopicorbits were computed for this sample. Physical relations are establishedfor most of the visual systems and several optical components areidentified as well. The period distribution of sub-systems has a maximumat periods from 2 to 7 days, likely explained by a combination of tidaldissipation with triple-star dynamics. The fraction of spectroscopicsub-systems among the dwarf components of close visual binaries withknown orbits is similar to that of field dwarfs, from 11% to 18% percomponent. Sub-systems are more frequent among the components of widevisual binaries and among wide tertiary components to the known visualor spectroscopic binaries - 20% and 30%, respectively. In triple systemswith both outer (visual) and inner (spectroscopic) orbits known, we findan anti-correlation between the periods of inner sub-systems and theeccentricities of outer orbits which must be related to dynamicalstability constraints. Tables 1, 2, and 6 are only available inelectronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/382/118
| Kinematics of Hipparcos Visual Binaries. II. Stars with Ground-Based Orbital Solutions
This paper continues kinematical investigations of the Hipparcos visualbinaries with known orbits. A sample, consisting of 804 binary systemswith orbital elements determined from ground-based observations, isselected. The mean relative error of their parallaxes is about 12% andthe mean relative error of proper motions is about 4%. However, even 41%of the sample stars lack radial velocity measurements. The computedGalactic velocity components and other kinematical parameters are usedto divide the stars with known radial velocities into kinematical agegroups. The majority (92%) of binaries from the sample are thin diskstars, 7.6% have thick disk kinematics and only two binaries have halokinematics. Among them, the long-period variable Mira Ceti has a verydiscordant {Hipparcos} and ground-based parallax values. From the wholesample, 60 stars are ascribed to the thick disk and halo population.There is an urgent need to increase the number of the identified halobinaries with known orbits and substantially improve the situation withradial velocity data for stars with known orbits.
| Mesures d'etoiles doubles faites a Nice (5eme serie. Double star measurements made at Nice
We present the last observations from two lists: General program and MLRpairs, made with the 50~cm refractor of Nice Observatory.
| Orbits of sixteen visual binaries
Orbital elements, dynamic parallaxes, total masses, ephemerides, normalplaces, and residuals for 16 visual binary systems are computed frommicrometer observations and previously published data. The systemsinclude A1910, A1014, Hu 555, Beta 1047, A1034, A2146, A1951, A2776, Hu644, Sigma 1781, Omicron Sigma 278, Hu 1168, Omicron Sigma 327, OmicronSigma 406, Omicron Sigma 527, and Kpr 112.
| Micrometer observations of double stars.8.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1975ApJS...29..315H&db_key=AST
| The masses of stars above the main sequence.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1969AJ.....74..689S&db_key=AST
| Mikrometermessungen von Doppelsternen. VI.
Not Available
| Mesures d'etoiles doubles faites AU 38cm de l'Observatoire de Paris.
Not Available
| Mesures d'étoiles doubles faites au rĝfraceur de 38 cm de l'Observatoire de Nice
Not Available
| Mesures d'étoiles doubles faites à l'Observatoire de Paris
Not Available
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| Takýmyýldýz: | Buyuk Ayi |
| Sað Açýklýk: | 11h05m34.67s |
| Yükselim: | +54°48'28.8" |
| Görünürdeki Parlaklýk: | 8.325 |
| Uzaklýk: | 137.363 parsek |
| özdevim Sað Açýklýk: | 15.9 |
| özdevim Yükselim: | 10.6 |
| B-T magnitude: | 9.026 |
| V-T magnitude: | 8.383 |
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