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A Methodology for the Description of Multiple Stellar Systems with Spectroscopic Subcomponents
We propose a methodology for analyzing triple stellar systems thatinclude a visual double star wherein one of the components is a single-or double-lined spectroscopic binary. By using this methodology, we cancalculate the most probable values of the spectroscopic binary'sinclination, the angular separation between its components, and itsstellar masses, and we can even estimate the spectral types. For a few WUMa-type eclipsing binaries, stellar radii are also determined.Moreover, we present new formulae for calculating stellar massesdepending on spectral type. In this way we have studied 61 triplesystems, five of them W UMa-type eclipsing binaries with low-masssubcomponents. In addition, we study nine quadruple systems, applyingthe same methodology and considering them twice as a triple system. Withthe aim of having more accurate orbital elements, we have takenadvantage of the occasion to calculate and improve orbits. In this waywe have used a new speckle measurement to improve the orbital elementsfor the binary Hu 506 AB. Also, new visual orbits are calculated for thebinaries BAG 10 Aa and LAB 6 Aa. Finally, we give a list of fivespectroscopic binaries with more than 0.1" for the maximum angularseparation; these should be easily observable as visual binaries bymeans of interferometric techniques.
| Tertiary companions to close spectroscopic binaries
We have surveyed a sample of 165 solar-type spectroscopic binaries (SB)with periods from 1 to 30 days for higher-order multiplicity. Asubsample of 62 targets were observed with the NACO adaptive opticssystem and 13 new physical tertiary companions were detected. Anadditional 12 new wide companions (5 still tentative) were found usingthe 2MASS all-sky survey. The binaries belong to 161 stellar systems; ofthese 64 are triple, 11 quadruple and 7 quintuple. After correction forincompleteness, the fraction of SBs with additional companions is foundto be 63% ± 5%. We find that this fraction is a strong functionof the SB period P, reaching 96% for P<3d and dropping to34% for P>12^d. Period distributions of SBs with and withouttertiaries are significantly different, but their mass ratiodistributions are identical. The statistical data on the multiplicity ofclose SBs presented in this paper indicates that the periods and massratios of SBs were established very early, but the periods of SB systemswith triples were further shortened by angular momentum exchange withcompanions.
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| SB9: The ninth catalogue of spectroscopic binary orbits
The Ninth Catalogue of Spectroscopic Binary Orbits(http://sb9.astro.ulb.ac.be) continues the series of compilations ofspectroscopic orbits carried out over the past 35 years by Batten andcollaborators. As of 2004 May 1st, the new Catalogue holds orbits for2386 systems. Some essential differences between this catalogue and itspredecessors are outlined and three straightforward applications arepresented: (1) completeness assessment: period distribution of SB1s andSB2s; (2) shortest periods across the H-R diagram; (3)period-eccentricity relation.
| 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
| Speckle Interferometry at the US Naval Observatory. VIII.
The results of 2044 speckle interferometric observations of doublestars, made with the 26 inch (66 cm) refractor of the US NavalObservatory, are presented. Each speckle interferometric observation ofa system represents a combination of over a thousand short-exposureimages. These observations are averaged into 1399 mean positions andrange in separation from 0.16" to 14.97", with a mean separation of2.51". This is the eighth in a series of papers presenting measuresobtained with this system and covers the period 2001 March 18 through2001 December 30.
| 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.
| Binary star speckle measurements at Calar Alto. I.
We present the first results of our speckle interferometric measurementsof binary stars made with the ICCD speckle camera using the 1.52-mtelescope of the Observatorio Astronomico Nacional at Calar Alto (Spain)in September, 1999. The data contain 123 observations of 83 systems. Themeasured angular separations range from 0farcs153 to 6farcs727 . We haveused there new speckle measurements to improve the orbital elements forthe binaries COU 247 and BU 524 AB.
| Dynamical Stability of Triple Stars
The dynamical stability of 38 observed hierarchical triple stars withknown orbital elements of the internal and external binary subsystemsand component masses is considered. Four different criteria of dynamicalstability are used. The observed stability parameters and their criticalvalues are calculated by taking into account errors in the orbitalelements and component masses. Most triple systems are stable. Accordingto some criteria, several triple stars (ADS440, xi Tau, lambda Tau,ADS3358, VV Ori, ADS10157, HZ Her, Gliese 795, ADS15971, and ADS16138)may be dynamically unstable. This result is probably associated withunreliability of the empirical stability criteria and/or with errors inthe observed quantities.
| Two-colour photometry for 9473 components of close Hipparcos double and multiple stars
Using observations obtained with the Tycho instrument of the ESAHipparcos satellite, a two-colour photometry is produced for componentsof more than 7 000 Hipparcos double and multiple stars with angularseparations 0.1 to 2.5 arcsec. We publish 9473 components of 5173systems with separations above 0.3 arcsec. The majority of them did nothave Tycho photometry in the Hipparcos catalogue. The magnitudes arederived in the Tycho B_T and V_T passbands, similar to the Johnsonpassbands. Photometrically resolved components of the binaries withstatistically significant trigonometric parallaxes can be put on an HRdiagram, the majority of them for the first time. Based on observationsmade with the ESA Hipparcos satellite.
| Photometric Separation of Stellar Properties Using SDSS Filters
Using synthetic photometry of Kurucz model spectra, we explore thecolors of stars as a function of temperature, metallicity, and surfacegravity with Sloan Digital Sky Survey (SDSS) filters, u'g'r'i'z'. Thesynthetic colors show qualitative agreement with the few publishedobservations in these filters. We find that the locus of synthetic starsis basically two-dimensional for 4500 < T < 8000 K, whichprecludes simultaneous color separation of the three basic stellarcharacteristics we consider. Colors including u' contain the mostinformation about normal stellar properties; measurements in this filterare also important for selecting white dwarfs. We identify two differentsubsets of the locus in which the loci separate by either metallicity orsurface gravity. For 0.5 < g' - r' < 0.8 (corresponding roughly toG stars), the locus separates by metallicity; for photometric error of afew percent, we estimate metallicity to within ~0.5 dex in this range.In the range -0.15 < g' - r' < 0.00 (corresponding roughly to Astars), the locus shows separation by surface gravity. In both cases, weshow that it is advantageous to use more than two colors whendetermining stellar properties by color. Strategic observations in SDSSfilters are required to resolve the source of a ~5% discrepancy betweensynthetic colors of Gunn-Stryker stars, Kurucz models, and externaldeterminations of the metallicities and surface gravities. The syntheticstar colors can be used to investigate the properties of any normal starand to construct analytic expressions for the photometric prediction ofstellar properties in special cases.
| Observations of Double Stars. XVIII.
Micrometer observations of 1350 pairs in 1995-1997 are listed.
| Micrometer measurements of visual double stars made at the Cote d'Azur Observatory.
Not Available
| MSC - a catalogue of physical multiple stars
The MSC catalogue contains data on 612 physical multiple stars ofmultiplicity 3 to 7 which are hierarchical with few exceptions. Orbitalperiods, angular separations and mass ratios are estimated for eachsub-system. Orbital elements are given when available. The catalogue canbe accessed through CDS (Strasbourg). Half of the systems are within 100pc from the Sun. The comparison of the periods of close and widesub-systems reveals that there is no preferred period ratio and allpossible combinations of periods are found. The distribution of thelogarithms of short periods is bimodal, probably due to observationalselection. In 82\% of triple stars the close sub-system is related tothe primary of a wide pair. However, the analysis of mass ratiodistribution gives some support to the idea that component masses areindependently selected from the Salpeter mass function. Orbits of wideand close sub-systems are not always coplanar, although thecorresponding orbital angular momentum vectors do show a weak tendencyof alignment. Some observational programs based on the MSC aresuggested. Tables 2 and 3 are only available in electronic form at theCDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| 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.
| Orbital coplanarity in solar-type binary systems: Implications for planetary system formation and detection
The equatorial inclinations of solar-type stars within visual binarysystems are computed by combining v sin i measurements with rotationalperiod information, or with expected rotational velocities based uponthe age of the star in question. These inclinations are then comparedwith the orbital inclinations of the systems to test the alignmentbetween the equatorial and orbital planes, and how the tendency for oragainst coplanarity varies as a function of parameters such as spectraltype, separation, eccentricity, etc. The results are extended toplanetary systems in order to determine the appropriateness of basingplanetary search strategies upon a parent star's equatorial inclination,and to address issues in planetary system formation and evolution,including the stability of planetary orbits within binary systems.During the course of this project new or improved v sin i measurementsare made for over 30 solar-type stars within binary systems, and (forthe purposes of the study) tentative orbits are computed for thirteenlong-period systems. The results suggest that approximate coplanaritybetween the equatorial and orbital planes exists solar-type binarysystems with separations less than 30-40 AU. The coplanarity tendency,as well as this 'critical separation,' is not significantly affected bymost of the other parameters studied. The one significant exceptionoccurs with hierarchical multiple systems, where noncoplanarity mayexist at relatively small separations. If it is assumed that planetarydistances in our solar system are typical, the results suggest there isno reason to expect planets to orbit in planes significantly differentfrom that of the parent star's equator, in turn suggesting thatplanetary formation models and search strategies dependent upon thisassumption are valid from this standpoint. The results also suggest thatnoncoplanarity between the components of a binary system is not asignificant issue in addressing the stability of planetary orbits withinthe system.
| Double Star Measurements Made at Nice
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1993A&AS..102..643M&db_key=AST
| Relative Orientation of Angular Momenta in Multiple Stellar Systems
Not Available
| Theoretical colours and isochrones for some Hubble Space Telescope colour systems. II
A grid of synthetic surface brightness magnitudes for 14 bandpasses ofthe Hubble Space Telescope Faint Object Camera is presented, as well asa grid of UBV, uvby, and Faint Object Camera surface brightnessmagnitudes derived from the Gunn-Stryker spectrophotometric atlas. Thesynthetic colors are used to examine the transformations between theground-based Johnson UBV and Stromgren uvby systems and the Faint ObjectCamera UBV and uvby. Two new four-color systems, similar to theStromgren system, are proposed for the determination of abundance,temperature, and surface gravity. The synthetic colors are also used tocalculate color-magnitude isochrones from the list of theoretical tracksprovided by VandenBerg and Bell (1990). It is shown that by using theappropriate filters it is possible to minimize the dependence of thiscolor difference on metallicity. The effects of interstellar reddeningon various Faint Object Camera colors are analyzed as well as theobservational requirements for obtaining data of a given signal-to-noisefor each of the 14 bandpasses.
| Measurements of binaries made with the 152-cm telescope at Calar Alto
A total of 143 micrometer measurements are presented for 58 double starsobserved with the 152-cm telescope of the National AstronomicalObservatory at Calar Alto. This is the first published list ofobservations of this kind made with this telescope.
| The mass and luminosity of cool dwarf stars
An empircal mass-luminosity relation is derived for main-sequence starsin the range where log m is between -0.6 and +0.1. The sample used inthe computations is a combination of the visual double stars consideredby Cester et al. (1983) and the spectroscopic binaries studied byDuquennoy and Mayor (1988). Linear and second-order fits were applied tothese measures with rms errors of + or - 0.3 in magnitude and + or -0.025 in the logarithm of stellar mass. An example is presented in whichthe relation is applied to the luminosity function of nearby stars.
| Energy Distribution in the Stellar Spectra of Different Spectral Types and Luminosities - Part Five - Normal Stars
Not Available
| The absolute spectrophotometric study of binary stars around Gamma CAS in the UV and visible ranges
Results of absolute spectrophotometric measurements of 15 binary starsof the classes F, G, and K in the 2300-4800 A wavelength interval arepresented. The absolute energy distributions of the stars studied in theUV and visible range were compared with Kurucz's (1979) theoreticalmodels. Spectral and luminosity classes of the system components areestimated by constructing the combined spectra.
| Micrometer observations of double stars and new pairs. XIII
From a program of double star observations which emphasizes orbital,neglected, and newly discovered pairs, results obtained from October1984 to January 1987 are presented. A total of 3030 visual and 550photographic measures are listed. The positions in WDS format andDurchmusterung numbers are shown for 117 pairs for which firstobservations appear in this paper. Magnitudes are estimated for some ofthe objects.
| A study of multiple stellar systems with CORAVEL.
A spectrographic survey of visual binaries undertaken with the CORAVELspectrometer permitted detection or confirmation of unknownspectroscopic subsystems, sometimes with small amplitude radial velocityvariations. A new computer program has been developed to analyze theblended dips of such systems, giving correct determinations of theindividual radial velocities for separations down to 2 km/s. Four visualbinaries for which a spectroscopic subsystem has been discovered (HD7331, HD 214608) or confirmed (HD 196795, HD 219018) are studied.Orbital elements of the last three show small ratios of visual tospectroscopic period and small amplitude of radial velocity variation.Individual masses are derived and included in satisfactory modelscombining photometry, spectral types, parallaxes, and rotation
| Stellar spectrophotometric atlas, wavelengths from 3130 to 10800 A
Over the course of the past 10 years, a large body of homogeneousspectrophotometric data on relatively bright stars has been gathered toserve as a library with which to synthesize galaxy spectra in populationstudies. As the data might be generally useful, they are presented inthree tables. One hundred seventy-five (175) stars were selected, mostfrom the Navy photometric catalog. Covered are complete ranges ofspectral type and luminosity class. Normalized spectral energydistributions of these stars in pictorial form are provided along withtables of calculated colors, scan line and continuum indices, and someinformation on the relation of the scan colors to real photometricsystems.
| Correction of the dynamical elements of the orbits of eleven visual binaries.
Not Available
| MK classification for visual binary components
MK classifications are presented for both components of 208 visualbinaries, most of which appear in the Third Catalogue of Orbits ofVisual Binary Stars (Finsen and Worley 1970) and which have onlycomposite MK spectral types and visual-magnitude differences. Comparisonbetween the results obtained and the several individually observed orpreviously inferred component types suggest that an accuracy of plus orminus 2 to 3 spectral subtypes may be expected for both unevolved pairsand evolved pairs; an accuracy of plus or minus 0.5 to 1.0 luminosityclasses is expected for evolved pairs.
| 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
| Micrometric measures of visual double stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1975PASP...87..253H&db_key=AST
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| קבוצת-כוכבים: | קאסיופיאה |
| התרוממות ימנית: | 01h14m45.82s |
| סירוב: | +60°56'20.2" |
| גודל גלוי: | 7.311 |
| מרחק: | 87.873 פארסק |
| תנועה נכונה: | 64 |
| תנועה נכונה: | -43.5 |
| B-T magnitude: | 7.862 |
| V-T magnitude: | 7.357 |
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