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Effective temperature scale and bolometric corrections from 2MASS photometry
We present a method to determine effective temperatures, angularsemi-diameters and bolometric corrections for population I and II FGKtype stars based on V and 2MASS IR photometry. Accurate calibration isaccomplished by using a sample of solar analogues, whose averagetemperature is assumed to be equal to the solar effective temperature of5777 K. By taking into account all possible sources of error we estimateassociated uncertainties to better than 1% in effective temperature andin the range 1.0-2.5% in angular semi-diameter for unreddened stars.Comparison of our new temperatures with other determinations extractedfrom the literature indicates, in general, remarkably good agreement.These results suggest that the effective temperaure scale of FGK starsis currently established with an accuracy better than 0.5%-1%. Theapplication of the method to a sample of 10 999 dwarfs in the Hipparcoscatalogue allows us to define temperature and bolometric correction (Kband) calibrations as a function of (V-K), [m/H] and log g. Bolometriccorrections in the V and K bands as a function of T_eff, [m/H] and log gare also given. We provide effective temperatures, angularsemi-diameters, radii and bolometric corrections in the V and K bandsfor the 10 999 FGK stars in our sample with the correspondinguncertainties.
| 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.
| The ages of the globular clusters M 71 and 47 Tuc from Strömgren uvby photometry. Evidence for high ages
New uvby CCD photometry for the fairly metal-rich globular clusters M 71(NGC 6838) and 47 Tuc (NGC 104) is presented. We derive the clusterdistances using a sample of field subdwarfs with metallicitiesdetermined from uvby photometry and accurate parallaxes from theHipparcos mission. The biases associated with the main-sequence fittingtechnique are discussed and only that due to metallicity is found to besignificant, corresponding to a -0.05 mag change in distance modulus.Our main results are that: 1) The distance moduli of 47 Tuc and M 71 aresomewhat shorter than that derived by Reid (\cite{Rei98}, AJ 115, 204).For M 71 and 47 Tuc we find (metallicity corrected) (m-M)V =13.71+/- 0.04+/- 0.1 and (m-M)V = 13.33+/- 0.04+/- 0.1, foradopted reddenings of E(B-V) = 0.28 and E(B-V) = 0.04 respectively(first errorbar denotes random errors and the second systematic errors).The main source of difference with Reid is the selection of subdwarfswith this study having more intrinsically faint field subdwarfs; 2)These values lead to ages of nearly 12 Gyr when using the isochrones ofVandenBerg et al. (\cite{Vane00}, ApJ, 532, 430); this estimate does notinclude the effects of He diffusion. 3) A differential comparison of thecluster colour-magnitude diagrams show that the age difference betweenthe two is very small - less than one billion years. 4) The observedscatter in the c1 index (due to star-to-star nitrogenvariations) among main-sequence stars does not allow us to use the[(v-y)0, c0] diagram for a distance-independentage determination. Based on observations made with the Nordic OpticalTelescope, operated on the island of La Palma jointly by Denmark,Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio delRoque de los Muchachos of the Instituto de Astrofisica de Canarias.Based on observations obtained with the Danish 1.5 m telescope at theEuropean Southern Observatory, La Silla, Chile.
| Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics
The Catalogue, available at the Centre de Données Stellaires deStrasbourg, consists of 13 573 records concerning the results obtainedfrom different methods for 7778 stars, reported in the literature. Thefollowing data are listed for each star: identifications, apparentmagnitude, spectral type, apparent diameter in arcsec, absolute radiusin solar units, method of determination, reference, remarks. Commentsand statistics obtained from CADARS are given. The Catalogue isavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcar?J/A+A/367/521
| Kinematics and Metallicity of Stars in the Solar Region
Several samples of nearby stars with the most accurate astrometric andphotometric parameters are searched for clues to their evolutionaryhistory. The main samples are (1) the main-sequence stars with b - ybetween 0.29 and 0.59 mag (F3 to K1) in the Yale parallax catalog, (2) agroup of high-velocity subgiants studied spectroscopically by Ryan &Lambert, and (3) high-velocity main-sequence stars in the extensiveinvestigation by Norris, Bessel, & Pickles. The major conclusionsare as follows: (1) The oldest stars (halo), t >= 10-12 Gyr, haveV-velocities (in the direction of Galactic rotation and referred to theSun) in the range from about -50 to -800 km s^-1 and have aheavy-element abundance [Fe/H] of less than about -0.8 dex. The agerange of these objects depends on our knowledge of globular clusterages, but if age is correlated with V-velocity, the youngest may be M22and M28 (V ~ -50 km s^-1) and the oldest NGC 3201 (V ~ -500 km s^-1) andassorted field stars. (2) The old disk population covers the large agerange from about 2 Gyr (Hyades, NGC 752) to 10 or 12 Gyr (Arcturusgroup, 47 Tuc), but the lag (V) velocity is restricted to less thanabout 120 km s^-1 and [Fe/H] >= -0.8 or -0.9 dex. The [Fe/H] ~ -0.8dex division between halo and old disk, near t ~ 10-12 Gyr, is marked bya change in the character of the CN index (C_m) and of the blanketingparameter K of the DDO photometry. (3) The young disk population, t <2 Gyr, is confined exclusively to a well-defined area of the (U, V)velocity plane. The age separating young and old disk stars is also thatseparating giant evolution of the Hyades (near main-sequence luminosity)and M67 (degenerate helium cores and a large luminosity rise) kinds. Thetwo disk populations are also separated by such indexes as the g-indexof Geveva photometry. There appears to be no obvious need to invokeexogeneous influences to understand the motion and heavy-elementabundance distributions of the best-observed stars near the Sun.Individual stars of special interest include the parallax star HD 55575,which may be an equal-component binary, and the high-velocity star HD220127, with a well-determined space velocity near 1000 km s^-1.
| The catalogue of nearby stars metallicities.
Not Available
| Vitesses radiales. Catalogue WEB: Wilson Evans Batten. Subtittle: Radial velocities: The Wilson-Evans-Batten catalogue.
We give a common version of the two catalogues of Mean Radial Velocitiesby Wilson (1963) and Evans (1978) to which we have added the catalogueof spectroscopic binary systems (Batten et al. 1989). For each star,when possible, we give: 1) an acronym to enter SIMBAD (Set ofIdentifications Measurements and Bibliography for Astronomical Data) ofthe CDS (Centre de Donnees Astronomiques de Strasbourg). 2) the numberHIC of the HIPPARCOS catalogue (Turon 1992). 3) the CCDM number(Catalogue des Composantes des etoiles Doubles et Multiples) byDommanget & Nys (1994). For the cluster stars, a precise study hasbeen done, on the identificator numbers. Numerous remarks point out theproblems we have had to deal with.
| New six-color intermediate-band photometry and photometric solutions for U Cephei
We describe new six-color intermediate-band photometric observations ofU Cephei, obtained during an interval of consistently low mass-transferactivity. We use the new Wilson eclipsing binary computer program toobtain several photometric solutions, which incorporate the rapidrotation of the hot star. Residual trends for solutions using allobservations show the absorbing effect of the stream between phases 0.7and 0.96. A second set of solutions, omitting data in this phase range,leads to more satisfactory results. Our photometric mass ratio issomewhat smaller than the spectroscopic values found by both Batten(1974) and Tomkin (1981). Differences between our solutions and those ofRafert and Markworth (1991) are probably due to residual contaminationof light curves by circumstellar matter.
| What is RX Cephei?
Not Available
| Magnetic structure in cool stars. XVII - Minimum radiative losses from the outer atmosphere
The emissions in several chromospheric and transition region lines andin coronal soft X-rays are analyzed for a sample of cool stars. Thenature of the lower-limit flux densities is explored, and evidence isgiven for the possibility of a basal, nonmagnetic heating mechanismbeing responsible for these emission fluxes up to, and perhapsincluding, the upper transition region. It is argued that the excessflux density, derived by subtraction of the basal flux density from theobserved stellar flux, is the proper measure of magnetic activity. Thelevel of the basal flux density as a function of color is determined tobe 2 x 10 exp 6 erg/sq cm/s for F-type stars and 2 x 10 exp 5 erg/sqcm/s for K-type stars.
| CA II H and K measurements made at Mount Wilson Observatory, 1966-1983
Summaries are presented of the photoelectric measurements of stellar CaII H and K line intensity made at Mount Wilson Observatory during theyears 1966-1983. These results are derived from 65,263 individualobservations of 1296 stars. For each star, for each observing season,the maximum, minimum, mean, and variation of the instrumental H and Kindex 'S' are given, as well as a measurement of the accuracy ofobservation. A total of 3110 seasonal summaries are reported. Factorswhich affect the ability to detect stellar activity variations andaccurately measure their amplitudes, such as the accuracy of the H and Kmeasurements and scattered light contamination, are discussed. Relationsare given which facilitate intercomparison of 'S' values with residualintensities derived from ordinary spectrophotometry, and for convertingmeasurements to absolute fluxes.
| Chromospheric activity in evolved stars - The rotation-activity connection and the binary-single dichotomy
A tabulation of measured values of the Ca II H and K (S) index aretransformed to the original Mount Wilson definition of the index. Thetabulation includes main-sequence, evolved, single, and tidally coupled(RS CVn) binary stars. The (S) indices are analyzed against Wilson's(1976) I(HK) intensity estimates, showing that Wilson's estimates areonly a two-state indicator. Ca II H and K fluxes are computed andcalibrated with published values of rotation periods. It is found thatthe single and binary stars are consistent with a single relationshipbetween rotation and Ca II excess emission flux.
| The chromospheric age dependence of the birthrate, composition, motions, and rotation of late F and G dwarfs within 25 parsecs of the sun
The chromospheric ages of 115 late F and G dwarfs within 25 parsecs ofthe sun are calculated. Rotational velocities are plotted againstchromospheric age to reveal the rotational spin-down trajectories ofsolar-type stars of various masses. Also, plots of metal abundance andpeculiar velocity versus chromospheric age are used to determine trendswith age.
| Einstein Observatory survey of X-ray emission from solar-type stars - The late F and G dwarf stars
Results of a volume-limited X-ray survey of stars of luminosity classesIV and V in the spectral range F7-G9 observed with the EinsteinObservatory are presented. Using survival analysis techniques, thestellar X-ray luminosity function in the 0.15-4.0 keV energy band forboth single and multiple sources. It is shown that the difference inX-ray luminosity between these two classes of sources is consistent withthe superposition of individual components in multiple-componentsystems, whose X-ray properties are similar to those of thesingle-component sources. The X-ray emission of the stars in our sampleis well correlated with their chromospheric CA II H-K line emission andwith their projected equatorial rotational velocity. Comparison of theX-ray luminosity function constructed for the sample of the dG stars ofthe local population with the corresponding functions derived elsewherefor the Hyades, the Pleiades, and the Orion Ic open cluster confirmsthat the level of X-ray emission decreases with stellar age.
| An unbiased X-ray sampling of stars within 25 parsecs of the sun
A search of all of the Einstein Laboratory IPC and HRI fields foruntargeted stars in the Woolley, et al., Catalogue of the nearby starsis reported. Optical data and IPC coordinates, flux densityFx, and luminosity Lx, or upper limits, aretabulated for 126 single or blended systems, and HRI results for a fewof them. IPC luminosity functions are derived for the systems, for 193individual stars in the systems (with Lx shared equally amongblended components), and for 63 individual M dwarfs. These stars haverelatively large X-ray flux densities that are free of interstellarextinction, because they are nearby, but they are otherwise unbiasedwith respect to the X-ray properties that are found in a defined smallspace around the sun.
| Predicted infrared brightness of stars within 25 parsecs of the sun
Procedures are given for transforming selected optical data intoinfrared flux densities or irradiances. The results provide R, T(eff)blackbody approximations for about 2000 of the stars in Woolley et al.'sCatalog of Stars (1970) within 25 pc of the sun, and additional whitedwarfs, with infrared flux densities predicted for them at ninewavelengths from 2.2 to 101 microns including the Infrared AstronomySatellite bands.
| The recent behavior of the period of U Cephei
Four primary eclipses were observed in 1975 and 1976 and times ofminimum were obtained from them. Twenty other recent times of minimumbased on photoelectric observations, published and unpublished, arecollected and analyzed. One can expect systematic error of about plus orminus 0.003 d due to asymmetry in many of these light curves. In theinterval 1963.7 through 1971.2 individual photoelectric times of minimumfit a parabola with an rms scatter of only plus or minus 0.0015 d. Latertimes fall progressively below this parabola, 0.06 d below as of Fall1976, and with an rms scatter of plus or minus 0.0025 d fit a straightline which intersects the parabola in early 1972. The sudden perioddecrease implicit in this interpretation, delta P/P of about -3 x 10 tothe 5th, is similar to the other nine experienced by U Cep since 1880.
| Catalog of Indidual Radial Velocities, 0h-12h, Measured by Astronomers of the Mount Wilson Observatory
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1970ApJS...19..387A&db_key=AST
| A photometric study of U Cephei.
Not Available
| Variable stars of short period.
Not Available
| Light curves of variables stars determined photometrically.
Not Available
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| Сазвежђа: | Цефеј |
| Ректацензија: | 01h03m38.78s |
| Deклинација: | +82°06'02.7" |
| Apparent магнитуда: | 8.427 |
| Даљина: | 44.326 parsecs |
| Proper motion RA: | -175.1 |
| Proper motion Dec: | -63.1 |
| B-T magnitude: | 9.15 |
| V-T magnitude: | 8.487 |
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