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A Spectroscopic Search for λ Bootis and Other Peculiar A-Type Stars in Intermediate-Age Open Clusters
As part of our continuing search for peculiar A-type stars, especiallyλ Bootis stars, in open clusters of all ages, we have obtainedclassification spectra of 130 late B, A, and early F-type stars in 12intermediate-age open clusters, including NGC 1039, 2281, 2548, 6633,7039, 7063, 7092, and 7209, IC 4665, IC 4756, Stock 2, and Praesepe. Thespectra were obtained with resolutions of 1.8 and 3.6 Å on the 0.8m telescope of Appalachian State University and were classified on theMK system. Numerous classical Ap and Am stars were found among the 130,including two new Ap stars in NGC 7092. In addition, three emission-linestars and two candidate λ Bootis stars were found. Neither ofthese λ Bootis candidates turned out to be members of theirrespective clusters. Combined with 184 stars previously classified in 10other intermediate-age open clusters, also devoid of λ Bootisstars, a statistically significant null result is obtained. We discussthe implications of this null result for our understanding of theλ Bootis mechanism.
| 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
| Absolute proper motions of open clusters. I. Observational data
Mean proper motions and parallaxes of 205 open clusters were determinedfrom their member stars found in the Hipparcos Catalogue. 360 clusterswere searched for possible members, excluding nearby clusters withdistances D < 200 pc. Members were selected using ground basedinformation (photometry, radial velocity, proper motion, distance fromthe cluster centre) and information provided by Hipparcos (propermotion, parallax). Altogether 630 certain and 100 possible members werefound. A comparison of the Hipparcos parallaxes with photometricdistances of open clusters shows good agreement. The Hipparcos dataconfirm or reject the membership of several Cepheids in the studiedclusters. Tables 1 and 2 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
| Radial velocities. Measurements of 2800 B2-F5 stars for HIPPARCOS
Radial velocities have been determined for a sample of 2930 B2-F5 stars,95% observed by the Hipparcos satellite in the north hemisphere and 80%without reliable radial velocity up to now. Observations were obtainedat the Observatoire de Haute Provence with a dispersion of 80Ä,mm(-1) with the aim of studying stellar and galactic dynamics.Radial velocities have been measured by correlation with templates ofthe same spectral class. The mean obtained precision is 3.0 km s(-1)with three observations. A new MK spectral classification is estimatedfor all stars. Based on observations made at the Haute ProvenceObservatory, France and on data from The Hipparcos Catalogue, ESA.Tables 4, 5 and 6 are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr or viahttp://cdsweb.u-strasbg.fr/Abstract.htm
| Open clusters with Hipparcos. I. Mean astrometric parameters
New memberships, mean parallaxes and proper motions of all 9 openclusters closer than 300 pc (except the Hyades) and 9rich clusters between 300 and 500 pc have been computed using Hipparcosdata. Precisions, ranging from 0.2 to 0.5 mas for parallaxes and 0.1 to0.5 mas/yr for proper motions, are of great interest for calibratingphotometric parallaxes as well as for kinematical studies. Carefulinvestigations of possible biases have been performed and no evidence ofsignificant systematic errors on the mean cluster parallaxes has beenfound. The distances and proper motions of 32 more distant clusters,which may be used statistically, are also indicated. Based onobservations made with the ESA Hipparcos astrometry satellite
| The HR-diagram from HIPPARCOS data. Absolute magnitudes and kinematics of BP - AP stars
The HR-diagram of about 1000 Bp - Ap stars in the solar neighbourhoodhas been constructed using astrometric data from Hipparcos satellite aswell as photometric and radial velocity data. The LM method\cite{luri95,luri96} allows the use of proper motion and radial velocitydata in addition to the trigonometric parallaxes to obtain luminositycalibrations and improved distances estimates. Six types of Bp - Apstars have been examined: He-rich, He-weak, HgMn, Si, Si+ and SrCrEu.Most Bp - Ap stars lie on the main sequence occupying the whole width ofit (about 2 mag), just like normal stars in the same range of spectraltypes. Their kinematic behaviour is typical of thin disk stars youngerthan about 1 Gyr. A few stars found to be high above the galactic planeor to have a high velocity are briefly discussed. Based on data from theESA Hipparcos astrometry satellite and photometric data collected in theGeneva system at ESO, La Silla (Chile) and at Jungfraujoch andGornergrat Observatories (Switzerland). Tables 3 and 4 are onlyavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Spectrophotometry of 237 Stars in 7 Open Clusters
Spectrophotometry is presented for 237 stars in 7 nearby open clusters:Hyades, Pleiades, Alpha Persei, Praesepe, Coma Berenices, IC 4665, andM39. The observations were taken by Lee McDonald and David Bursteinusing the Wampler single-channel scanner on the Crossley 0.9m telescopeat Lick Observatory from July 1973 through December 1974. Sixteenbandpasses spanning the spectral range 3500 Angstroms to 7780 Angstromswere observed for each star, with bandwidths 32Angstroms, 48 Angstromsor 64 Angstroms. Data are standardized to the Hayes-Latham system tomutual accuracy of 0.016 mag per passband. The accuracy of thespectrophotometry is assessed in three ways on a star-by-star basis.First, comparisons are made with previously published spectrophotometryfor 19 stars observed in common. Second, (B-V) colors and uvby colorsare compared for 236 stars and 221 stars, respectively. Finally,comparsions are made for 200 main sequence stars to the spectralsynthesis models of Kurucz, fixing log g = 4.0 and [Fe/H] = 0.0, andonly varying effective temperature. The accuracy of tests using uvbycolors and the Kurucz models are shown to track each other closely,yielding an accuracy estimate (1 sigma ) of 0.01 mag for the 13 colorsformed from bandpasses longward of the Balmer jump, and 0.02 mag for the3 colors formed from the three bandpasses below the Balmer jump. Incontrast, larger scatter is found relative to the previously publishedspectrophotometry of Bohm-Vitense & Johnson (16 stars in common) andGunn & Stryker (3 stars). We also show that the scatter in the fitsof the spectrophotometric colors and the uvby filter colors is areasonable way to identify the observations of which specific stars areaccurate to 1 sigma , 2 sigma , .... As such, the residuals from boththe filter color fits and the Kurucz model fits are tabulated for eachstar where it was possible to make a comparison, so users of these datacan choose stars according to the accuracy of the data that isappropriate to their needs. The very good agreement between the modelsand these data verifies the accuracy of these data, and also verifiesthe usefulness of the Kurucz models to define spectrophotometry forstars in this temperature range (>5000 K). These data define accuratespectrophotometry of bright, open cluster stars that can be used as asecondary flux calibration for CCD-based spectrophotometric surveys.
| Catalogue of proper motions, UBV-photometry and spectral classification in the region of NGC 7092 (M39)
Not Available
| Absolute proper motions of the open clusters M 39 and TR 37
The absolute proper motions of five BD stars in the region of the opencluster M 39 and of 20 BD stars in the region of the open cluster Tr 37are determined with an accuracy of 0.26 arcsec/100 yr. Measurements ofthe proper motions of the open clusters M 39 and Tr 37 are reported.
| Liste des étoiles Ap et Am dans les amas ouverts (édition révisée)
Not Available
| Infrared photometry of upper main sequence stars in M39
Infrared photometry of 19 Main sequence stars in the open cluster M39 ispresented. Infrared-infrared and optical-infrared color-color andcolor-magnitude diagrams are presented and compared with mean intrinsiccolor for Population I stars. An interstellar reddening of E(B - V) =0.01 is obtained by analysis of the color-color diagrams. Comparisonwith a set of theoretical isochrones leads to an age estimate for thecluster between 240 and 480 million years.
| Catalogue of Hydrogen Line Spectral Profiles of 236 B-Stars A-Stars and F-Stars
Not Available
| Liste des étoiles Ap et Am dans les amas ouverts (Edition révisée)
Not Available
| The catalogue of equivalent line widths in the spectra of A- and F-stars.
Not Available
| Catalog of AP and AM stars in open clusters
The previous results of Raab (1922), Markarian (1951), and Collinder(1931) have been used to catalog Ap and Am stars that are in the fieldof open clusters. Tabular data are presented for the clusterdesignation, the HD or HDE number, the right ascension (1900), thedeclination (1900), and the magnitude. Also listed are the spectraltypes and, for certain stars, the probability of cluster membership.
| Chemically peculiar stars in open clusters. I - The catalog
The largest existing compilation is presented of Ap and Am open clusterstars. The catalog contains information on 381 chemically peculiar (CP)stars of the upper main sequence in 79 open clusters. The catalog iscomposed of the following tables: (1) the main body, which lists CP (orsuspected CP) stars which are kinematical (or suspected kinematical)members of open clusters; (2) the list of CP (or suspected CP) starssometimes numbered among cluster members but which are actuallykinematical nonmembers; (3) the list of stars sometimes designated as'peculiar' but, in fact, probably not CP; (4) references for numberingsystems of cluster stars; (5) references for membership; and (6)references for spectral and/or peculiarity types.
| Quantitative Spectral Peculiarity Indices of Cp-Stars of the Upper Main Sequence
Not Available
| Statistical Investigation of Chemically Peculiar Stars - Part Four - Luminosity of Different Type Stars
Not Available
| Galactic cluster star radial velocities obtained with a focal reducer field spectrograph. I - The clusters IC 1805, NGC 2287, NGC 2548, IC 4665, NGC 6633, NGC 6940 and NGC 7092
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1985A&AS...62..301G&db_key=AST
| Velocities of rotation of chemically peculiar stars
An analysis of the velocities of rotation of 77 peculiar stars, membersof open clusters and associations in the age range log t = 6.4-8.7, wasmade based on observations with the OZSP spectrograph of the 6-mtelescope. It was concluded that there is no loss of angular momentum bypeculiar stars in the process of gravitational contraction as theyapproach the zero-age main sequence and in the stage of evolution withinthe main sequence. A statistically significant difference was obtainedin the velocities of rotation of peculiar stars in different zones ofthe Scorpio-Centaurus association: Stars of the core (t = 4 million yr)rotate faster on the average than stars in the outer zones of theassociation (t = 12 million yr).
| A photometric study of the open cluster M39
Photoelectric UBV magnitudes of 50 stars in the field of M39 have beenobtained for most of which previous photoelectric data were notavailable. These include 36 new members given by Platais (1984). Thereddening for the cluster has been found to be 0.03 mag. A distance of300 pc has been estimated for the cluster. The age of the cluster liesbetween 200 million and 400 million yr.
| Peculiar stars in the open clusters alpha Per, M 39, Coma Berenices.
Not Available
| Evidence of decay of the magnetic fields of AP stars
Data obtained in the Geneva photometric system (Rufener, 1981) andappropriate calibrations of this system in terms of surface magneticfield and gravity are used to provide, on the basis of 708 field andcluster Ap stars, observational evidence that these stars undergo decayof their magnetic field on an evolutionary timescale. Justifications aregiven for the application of a photometric gravity calibration topeculiar stars. The dependence of the photometrically estimated surfacemagnetic field on gravity is found to differ markedly from availabletheoretical calculations. HgMn stars are found to show the same trend,strengthening the impression that they might be slightly magnetic.He-weak stars do not.
| New candidate members of the open cluster NGC 7092 (M39)
Proper-motion and UBV data on 7931 stars in the 110-arcmin-diameterfield of the open cluster NGC 7092 from the catalog of Platais (1983)are analyzed, and the results are presented in tables and a graph. Atotal of 38 stars previously identified as cluster candidates areconfirmed, and 43 new candidates are presented. Of the members andcandidates, 38 have B magnitude 6-11 mag; 34 have 11.0-14.8 mag; and 9have 14.8-16.7 mag.
| Stellar content of young open clusters. III - The 'sn' stars
Twelve out of 16 stars in the sample of 17 cluster stars belonging tothe recently recognized class of 'sn' stars have V sin i values lowerthan 50 km/sec. It is ascertained that this represents true lowrotation, and does not result from an inclination effect, therebyexcluding both the pole-on hypothesis and the shell-like nature of thesharp lines as probable explanations. Either the 'sn' stars are thenormal state of slowly rotating stars, or they are peculiar. If thelatter, then normal rotating stars cannot exist for more than 50 millionyears before developing any peculiarity.
| The Sirius group as a moving supercluster
Without use of trigonometric parallaxes, the distances of some 50 brightstars have been determined on the basis of their well-determined propermotions and membership in a supercluster that includes Sirius. Theastrometric parallaxes are in excellent agreement with those obtainedfrom photometric parameters and, for the stars within 40 pc of the sun,they are also in agreement with trigonometric determinations. Thesupercluster stars are near 2.4 x 10 to the 8th yr old with (Fe/H) near-0.1. The resulting color-luminosity array confirms the expectedmain-sequence displacement for stars with a metal abundance only abouttwo thirds that of the Hyades supercluster members. The superclustercontains the UMa cluster and M39 (NGC 7092) but the former, at least,has only attracted attention because of the concentration of a fewbright (Dipper) supercluster members in Ursa Major.
| Photometric properties of AP stars in the Geneva system
An examination of the properties in some photometric diagrams of morethan 600 Ap stars measured in the Geneva photometric system confirm thatthe Balmer discontinuity is smaller than for normal stars, along withthe link between a proposed peculiarity parameter and both rotationalvelocity and effective magnetic field. It is shown that the peculiarityparameter is sensitive to interstellar reddening, and it is foundthrough examination of the standard deviations for visual magnitudesthat cool CP 2 stars without Eu peculiarity have the greatestamplitudes. Rapid rotators have a mild peculiarity, while positivecorrelation exists for Si and SrCr stars.
| The rotational velocities of magnetic AP stars
New and existing observations of the rotational velocities of Si-type Apstars in clusters are combined to demonstrate that magnetic stars loseangular momentum after they reach the main sequence. Measurements offield stars provide additional support for this hypothesis. Mechanismsfor magnetic braking are discussed, and it is shown that an interactionof the stellar magnetic field with the interstellar medium can accountfor the observed rate of loss of angular momentum. For Ap stars of later(non-Si) spectral type, it is likely that substantial additionalmagnetic braking takes place during the pre-main-sequence phase ofevolution.
| Polarization measurements of 313 nearby stars
The linear polarization of 313 low galactic latitude stars has beenmeasured. With few exceptions all program stars have a spectral typelater than B9 and are within 600 parsec of the sun. 181 stars aresituated at the southern sky and 132 at the northern sky.
| The occurrence of abnormal stars in open clusters
The age dependence of the frequencies of various types of abnormal starsin open clusters and associations is discussed. Spectra acquired atdispersions of 39 A/mm and 129 A/mm were used to determine the spectraltypes and luminosity classes of 661 stars in 14 open clusters andassociations. The frequencies of Ap(Si), Ap(Hg,Mn) and Ap(Sr,Cr) starsare found to increase with age to a level about that of field stars,while the rotational velocities of Ap(Si) and Ap(Hg,Mn) stars decreasewith time. Be stars in clusters exhibit a relatively constant frequency,roughly equal to that of Be field stars. The frequencies of stars withpronounced shell spectra are observed to remain constant with age, whilestars with unusually broad hydrogen lines (Vb stars) occur only in theyoungest clusters. The frequency of Am stars in clusters is notsignificantly different from that of field stars, and does not seem todepend on age, although rotational velocity is seen to decrease. It isconcluded that Ap or Am stars develop from stars of various rotationalspeeds, with a subsequent decrease in rotational velocity.
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| Csillagkép: | Hattyú |
| Rektaszcenzió: | 21h31m42.38s |
| Deklináció: | +48°35'04.6" |
| Vizuális fényesség: | 6.824 |
| Távolság: | 289.017 parszek |
| RA sajátmozgás: | -9.2 |
| Dec sajátmozgás: | -20.1 |
| B-T magnitude: | 6.786 |
| V-T magnitude: | 6.821 |
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