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Pulkovo compilation of radial velocities for 35495 stars in a common system.
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| Abundance difference between components of wide binaries. II. The southern sample
Aims.We present high-precision iron abundance differences for 33 widebinaries with similar components. They were observed with the FEROSspectrograph at ESO, looking for abundance anomalies due to theingestion of metal rich material of a planetary origin. Methods:.An optimized data analysis technique and the high quality of thespectra allowed us to achieve an error of about 0.02 dex for pairs withsmall temperaure differences. Results: . We found one case (HIP64030 = HD 113984) with a large (0.27 dex) abundance difference. Theprimary of this binary appears to be a blue straggler, and the abundancedifference might be due to the peculiar evolution of the star. A fewother pairs show small abundance differences (≤0.09 dex). In a fewcases these differences suggest the ingestion of a small amount of metalrich material, but in others they are likely spurious, because of thelarge temperature difference, high level of magnetic activity, ordifferent evolutionary phases between the components. Some cases ofabundance differences involving pairs with warm (Teff ≥6000 K) primaries might be due to the diffusion of heavy elements;dedicated theoretical models for the stellar parameters of the targetswould be welcome. Conclusions: . This study confirms ourpreliminary result based on analysis of 23 pairs (Desidera et al. 2004)that the occurrence of large alterations in stellar abundances caused bythe ingestion of metal rich, rocky material is not a common event. Forat least 65% of the pairs with components warmer than 5500 K, the limitson the amount of rocky material accreted by the program stars arecomparable to the estimates of rocky material accreted by the Sun duringits main-sequence lifetime.
| Spectroscopic characterization of a sample of southern visual binaries
Aims.We present the spectroscopic characterization of 56 pairs of visualbinaries with similar components, based on high resolution spectraacquired with FEROS at ESO La Silla. Methods: .For all stars, wemeasured radial and rotational velocities and CaII H&K emission. Results: .Five previously unknown double lined spectroscopic binarieswere found. Six other pairs show velocity differences that are notcompatible with the orbital motion of the wide pair, indicating thepresence of further companion(s) in the system. The fraction of visualbinaries that contain additional spectroscopic components is27±10%, compatible with other literature estimates. The ages ofthe components of the pairs derived from chromospheric activitytypically show apparent differences of about 0.2 dex. A few pairs show arather large difference in activity level, but in most cases this isconsistent with the variability of chromospheric emission observed forthe Sun along its magnetic cycle.
| The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of 14 000 F and G dwarfs
We present and discuss new determinations of metallicity, rotation, age,kinematics, and Galactic orbits for a complete, magnitude-limited, andkinematically unbiased sample of 16 682 nearby F and G dwarf stars. Our63 000 new, accurate radial-velocity observations for nearly 13 500stars allow identification of most of the binary stars in the sampleand, together with published uvbyβ photometry, Hipparcosparallaxes, Tycho-2 proper motions, and a few earlier radial velocities,complete the kinematic information for 14 139 stars. These high-qualityvelocity data are supplemented by effective temperatures andmetallicities newly derived from recent and/or revised calibrations. Theremaining stars either lack Hipparcos data or have fast rotation. Amajor effort has been devoted to the determination of new isochrone agesfor all stars for which this is possible. Particular attention has beengiven to a realistic treatment of statistical biases and errorestimates, as standard techniques tend to underestimate these effectsand introduce spurious features in the age distributions. Our ages agreewell with those by Edvardsson et al. (\cite{edv93}), despite severalastrophysical and computational improvements since then. We demonstrate,however, how strong observational and theoretical biases cause thedistribution of the observed ages to be very different from that of thetrue age distribution of the sample. Among the many basic relations ofthe Galactic disk that can be reinvestigated from the data presentedhere, we revisit the metallicity distribution of the G dwarfs and theage-metallicity, age-velocity, and metallicity-velocity relations of theSolar neighbourhood. Our first results confirm the lack of metal-poor Gdwarfs relative to closed-box model predictions (the ``G dwarfproblem''), the existence of radial metallicity gradients in the disk,the small change in mean metallicity of the thin disk since itsformation and the substantial scatter in metallicity at all ages, andthe continuing kinematic heating of the thin disk with an efficiencyconsistent with that expected for a combination of spiral arms and giantmolecular clouds. Distinct features in the distribution of the Vcomponent of the space motion are extended in age and metallicity,corresponding to the effects of stochastic spiral waves rather thanclassical moving groups, and may complicate the identification ofthick-disk stars from kinematic criteria. More advanced analyses of thisrich material will require careful simulations of the selection criteriafor the sample and the distribution of observational errors.Based on observations made with the Danish 1.5-m telescope at ESO, LaSilla, Chile, and with the Swiss 1-m telescope at Observatoire deHaute-Provence, France.Complete Tables 1 and 2 are only available in electronic form at the CDSvia anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/418/989
| Improved Astrometry and Photometry for the Luyten Catalog. II. Faint Stars and the Revised Catalog
We complete construction of a catalog containing improved astrometry andnew optical/infrared photometry for the vast majority of NLTT starslying in the overlap of regions covered by POSS I and by the secondincremental Two Micron All Sky Survey (2MASS) release, approximately 44%of the sky. The epoch 2000 positions are typically accurate to 130 mas,the proper motions to 5.5 mas yr-1, and the V-J colors to0.25 mag. Relative proper motions of binary components are measured to 3mas yr-1. The false-identification rate is ~1% for11<~V<~18 and substantially less at brighter magnitudes. Theseimprovements permit the construction of a reduced proper-motion diagramthat, for the first time, allows one to classify NLTT stars intomain-sequence (MS) stars, subdwarfs (SDs), and white dwarfs (WDs). We inturn use this diagram to analyze the properties of both our catalog andthe NLTT catalog on which it is based. In sharp contrast to popularbelief, we find that NLTT incompleteness in the plane is almostcompletely concentrated in MS stars, and that SDs and WDs are detectedalmost uniformly over the sky δ>-33deg. Our catalogwill therefore provide a powerful tool to probe these populationsstatistically, as well as to reliably identify individual SDs and WDs.
| A second list of wide visual binaries
Not Available
| A second list of wide visual binaries
Not Available
| Photographic measurements of double stars
In this paper the relative distances and position angles of thecomponents of 170 mostly southern visual double stars are presented. Theresults are obtained using photographic plates taken with the 60 cmdouble refractor of the Bosscha Observatory, Lembang, Indonesia.
| Long period double stars.
Abstract image available at:http://adsabs.harvard.edu/abs/1974A&A....33...15B
| Double stars of equal components.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1972A&A....18..341S&db_key=AST
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Pozíciós és asztrometriai adatok
| Csillagkép: | Mérleg |
| Rektaszcenzió: | 15h03m35.81s |
| Deklináció: | -27°50'27.6" |
| Vizuális fényesség: | 8.422 |
| Távolság: | 47.326 parszek |
| RA sajátmozgás: | 155.6 |
| Dec sajátmozgás: | -141.1 |
| B-T magnitude: | 9.166 |
| V-T magnitude: | 8.484 |
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