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Properties of planets in binary systems. The role of binary separation
Aims.The statistical properties of planets in binaries wereinvestigated. Any difference to planets orbiting single stars can shedlight on the formation and evolution of planetary systems. As planetswere found around components of binaries with very different separationand mass ratio, it is particularly important to study thecharacteristics of planets as a function of the effective gravitationalinfluence of the companion. Methods: .A compilation of planets inbinary systems was made; a search for companions orbiting stars recentlyshown to host planets was performed, resulting in the addition of twofurther binary planet hosts (HD 20782 and HD 109749). The probableoriginal properties of the three binary planet hosts with white dwarfscompanions were also investigated. Using this updated sample of planetsin binaries we performed a statistical analysis of the distributions ofplanet mass, period, and eccentricity, fraction of multiplanet systems,and stellar metallicity for planets orbiting components of tight andwide binaries and single stars. Results: .The only highlysignificant difference revealed by our analysis concerns the massdistribution of short-period planets. Massive planets in short periodorbits are found in most cases around the components of rather tightbinaries. The properties of exoplanets orbiting the components of widebinaries are compatible with those of planets orbiting single stars,except for a possible greater abundance of high-eccentricity planets.The previously suggested lack of massive planets with P>100 days inbinaries is not confirmed. Conclusions: .We conclude that thepresence of a stellar companion with separation smaller than 100-300 AUis able to modify the formation and/or migration and/or the dynamicalevolution history of giant planets while wide companions play a morelimited role.Table 1 and Appendices A-C are only available in electronic form athttp://www.aanda.org
| 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.
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| Takýmyýldýz: | Su Yilani |
| Sað Açýklýk: | 12h32m37.02s |
| Yükselim: | -26°27'28.4" |
| Görünürdeki Parlaklýk: | 9.43 |
| özdevim Sað Açýklýk: | -190.2 |
| özdevim Yükselim: | 48.6 |
| B-T magnitude: | 10.296 |
| V-T magnitude: | 9.502 |
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