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Searching for links between magnetic fields and stellar evolution. I. A survey of magnetic fields in open cluster A- and B-type stars with FORS1
Context: .About 5% of upper main sequence stars are permeated by astrong magnetic field, the origin of which is still matter of debate. Aims: . With this work we provide observational material to studyhow magnetic fields change with the evolution of stars on the mainsequence, and to constrain theory explaining the presence of magneticfields in A and B-type stars. Methods: . Using FORS1 inspectropolarimetric mode at the ESO VLT, we have carried out a survey ofmagnetic fields in early-type stars belonging to open clusters andassociations of various ages. Results: . We have measured themagnetic field of 235 early-type stars with a typical uncertainty of 100 G. In our sample, 97 stars are Ap or Bp stars. For thesetargets, the median error bar of our field measurements was 80 G.A field has been detected in about 41 of these stars, 37 of which werenot previously known as magnetic stars. For the 138 normal A and B-typestars, the median error bar was 136 G, and no field was detected in anyof them.
| Statistics of the Instability Strip of β Cephei Stars
We present a study of the β Cephei instability strip based on asample of 49 stars of this type. After deriving their effectivetemperatures and luminosities from their observed (B-V), (U-B) colorsand parallaxes we find their positions in the HR diagram to be mostlyconfined to the main sequence, and their masses to lie between 7Mȯ and 30 Mȯ. Their distribution on theHR diagram matches well with our previous theoretical instability stripwhich has an upper bound in the luminosity and rather tight boundariesin the effective temperature.
| A CCD Search for Variable Stars of Spectral Type B in the Northern Hemisphere Open Clusters. V. NGC 2169
We present results of a search for variable stars in the field of theyoung open cluster NGC 2169. The General Catalogue of Variable Stars(GCVS, http://www.sai.msu.su/groups/cluster/gcvs/) lists four variablestars in the field we observed, viz., two beta Cep stars, V 916 and V917Ori, an alpha^2CVn variable, V 1356Ori, and an RRc variable, V1154Ori. We find V 916 and V 1154Ori to be constant in light. We confirmthe variability of V 917Ori, but not the period given in GCVS. For thechemically peculiar A0 V Si star V 1356Ori we definitely establish theperiod of 1.565 d, thus settling the uncertainty persisting in theliterature since the star was discovered to be variable. In addition, wefind two other stars to be variable in light. Both show irregularvariations.For V 917Ori, one of the two GCVS beta Cep variables, we determine aperiod of 0.267 d (frequency 3.7477d^-1). However, prewhitening withthis period leaves a significant amount of the star's light-variationunaccounted for. Since the star shows emission at Hα, wehypothesize that the unaccounted for variation is caused by an erratic,Be-type activity. As to the periodic term, we consider three hypotheses:(1) beta Cep-type pulsation, (2) rotational modulation of the lambda Eritype, and (3) ellipsoidal variation due to distorted primary componentin a close binary system. After deriving the star's effectivetemperature from Stromgren indices and the luminosity from the distancemodulus of the cluster, we show that while the third hypothesis isuntenable, the first two should be retained. However, neither isentirely satisfactory.For a number of stars we provide the V magnitudes. For 14 brighteststars in our field we also obtain the photometric alpha-index, a measureof the Hα equivalent width. From the alpha index, we detect mildemission at Hα in two stars, V 917Ori and NGC 2169-8.
| 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
| Uvby-beta photometry of open clusters. IV. NGC 1444, NGC 1662, NGC 2129, NGC 2169 and NGC 7209.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1994RMxAA..28..139P&db_key=AST
| An IUE survey of interstellar H I LY alpha absorption. 1: Column densities
We measure Galactic interstellar neutral hydrogen column densities byanalyzing archival interstellar Ly alpha absorption line data toward 554B2 and hotter stars observed at high resolution with the IUE satellite.This study more than doubles the number of lines of sight with measuresof N(H I) based on Ly alpha. We have included the scattered lightbackground correction algorithm of Bianchi and Bohlin in our datareduction. We use the correlation between the Balmer discontinuity(c1) index and the stellar Ly alpha absorption in order toassess the effects of stellar Ly alpha contamination. Approximately 40%of the B stars with measured (c1) index, exhibit seriousstellar Ly alpha contamination. One table contains the derived values ofthe interstellar N(H I) for 393 stars with at most small amounts ofstellar contamination. Another lists the observed values of total N(H I)for 161 stars with suspected stellar Ly alpha contamination and/oruncertain stellar parameters.
| Photoelectric Search for Peculiar Stars in Open Clusters - Part Fourteen - NGC1901 NGC2169 NGC2343 CR:132 NGC2423 and NGC2447
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1993A&AS..102....1M&db_key=AST
| Ubvy + H-beta photometry of the young open clusters NGC 1502 and NGC 2169
This study presents results of a ubvy + H-beta photometric investigationof 22 and 14 stars, in the fields of NGC 1502 and NGC 2169,respectively, including new H-beta measurements for the 22 stars in NGC1502. A comparison with the findings of Perry et al. (1978) and Reimannand Pfau (1987) is discussed, with particular attention to the presenceof systematic errors present in the sequences of instrumental andstandard values. The membership of the observed stars is discussed onthe basis of the available photometric and radial velocity data.
| More radial-velocity measurements in young open clusters
Further high resolution radial-velocity measurements are reported in 23young open clusters using the Kitt Peak CCD coude spectrograph on the0.9-m feed telescope. The radial velocities for the cluster stars arederived with the technique of cross correlation. The internal precisionof the velocity measurements is typically 2 km/s for early type stars.From these new data and previously published velocities, the observedstars in two clusters, NGC 663 and NGC 2287, were found to show arelatively small dispersion in the measured mean velocities. Furtherobservations of stars in young clusters will be useful in helping toestablish an early-type-star-velocity standard system.
| Radial-velocity measurements in 20 young open clusters
The further results of a program to determine the radial velocities ofyoung open clusters are presented. Using the KPNO coude spectrographcoupled with the 1-m feed and 2.1-m telescopes, radial velocities havebeen measured for nearly one hundred stars, most of which are ofspectral type B and A, in 20 young clusters. The combination ofinstruments and the use of cross-correlation techniques show that radialvelocities of B and A type stars as faint as 10th magnitude can bedetermined with an internal precision of less than about 2 km/s. Asexpected, the uncertainties in the velocity determination for the youngclusters are dominated by spectroscopic binary stars in these clusters.A third of the stars in the sample are found to be spectroscopicbinaries, but with a large variation in the frequency of binaries fromcluster to cluster. Because the time coverage is still limited, thisshould be considered a lower limit to the binary frequency. Clustervelocities are determined after eliminating binaries and known nonmemberstars. The new velocities are compared with a model galactic rotationcurve, as well as with previous velocity determinations.
| Galactic interstellar abundance surveys with IUE. II - The equivalent widths and column densities
This paper continues a survey of interstellar densities, abundances, andcloud structure in the Galaxy, using the International UltravioletExplorer (IUE) satellite. Equivalent widths of 18 ultraviolet resonancetransitions are presented and column densities for Si II, Mn II, Fe II,S II, and Zn II toward 261 early-type stars are derived. Theseequivalent widths and column densities agree within the stated errors ofearlier Copernicus, BUSS, or IUE surveys of Mn II, Fe II, S II, and ZnII for 45 stars in common. The column densities are derived fromsingle-component curves of growth with a common b-value based on that ofFe II and Si II.
| IUE-IRAS studies of the infrared cirrus
The 60 and 100 micron cirrus emission around 256 lines of sight in theIRAS all-sky survey was measured, and the flux averages were used tostudy the distribution, variations, and correlations of the IRASinfrared cirrus fluxes with various interstellar parameters. It wasfound that the 60 and 100 micron fluxes correlate with the depletion ofSi and show a trend with the depletion of Fe for 51 lines of sighttoward the Galactic halo. No correlation was found with the abundancesof Si, Mn, Fe, S, or Zn or with abundance ratios for the full sample of256 stars. An abundance ratio of about 3 x 10 to the 7th by numberrelative to H was derived from 60 and 100 micron flux ratios and the Hcolumn along the line of sight; this ratio appears to decrease by afactor of 10 into the halo.
| Galactic interstellar abundance surveys with IUE. III - Silicon, manganese, iron, sulfur, and zinc
This paper continues a survey of intestellar densities, abundances, andcloud structure in the Galaxy using the IUE satellite. A statisticaldata set of 223 O3-B2.5 stars is constructed, including 53 stars in theGalactic halo. It is found that S II lines in B stars, of luminosityclasses IV and V, have possible contamination from stellar S II,particular for stars with v sin i less than 200 km/s. The meanlogarithmic depletions are -1.00, -1.19. -0.63, and -0.23 (Si, Mn,Fe,S,Zn). Depletions of Si, Mn, and Fe correlate with the mean hydrogendensity n-bar along the line of sight, with a turnover for n-bar greaterthan 1/cm. Sulfur depletions correlate with n-bar along the line ofsight. The slight Zn depletion correlation also appears to bestatistically insignificant. No correlation of depletion is found withthe physical density derived from H2 rotational states in 21 lines ofsight. Depletion variations in the disk are consistent with a Galacticabundance gradient or with enhanced mean depletions in the anticenterregion.
| Trapezium-type wide systems
On the basis of the Smithsonian Observatory Catalogues 15 Trapezium-typesystems are found. Photometric distances are determined for theTrapezium components. A conclusion is drawn on physical relations of thecomponents in the systems. The fact of existence of Trapezium-type largestellar systems confirms the existence of Trapezia with positive totalenergy.
| Equatorial coordinates of double and multiple star components measured on GPO astrographic plates
Equatorial coordinates are given for some of the multiple starcomponents having incomplete or inconsistent information in the IndexCatalog of Visual Double Stars. Two photographic plates were taken foreach system with incomplete or inconsistent information using the GPOastrograph. The plate measurement and reduction techniques used aredescribed.
| Galactic interstellar abundance surveys with IUE. I - Neutral hydrogen
A survey is initiated of interstellar densities, abundances, and cloudstructure in the Galaxy, using the International Ultraviolet Explorer.From high-resolution (0.1-A) spectra, interstellar column densities arederived toward 244 early-type stars by fitting the damping wings of theLy-alpha absorption line. Published B-V photometry is used to deriveE(B-V) color excesses, stellar distances r, and the mean hydrogendensities, n-bar = N(H I)/r. The data set includes stars out to r = 8.5kpc and E(B-V) = 0.86, with 68 stars in the galactic halo (absolute bgreater than 20 deg). The statistical sample consists of 205 stars oftype O3-B2.5 within 5 kpc (53 stars in the halo). The column densities,log N(H I), range from less than 19.44 per square centimeter for alphaVir to 21.81 for HD 37061. A statistical analysis of the E(B-V)distribution suggests variations in the line-of-sight cloud density andthe mean reddening per cloud.
| A photometric and spectroscopic study of the open cluster NGC 2169.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1978PASP...90...73P&db_key=AST
| Spectral Types in the Open cluster NGC 2169
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1977PASP...89..646A&db_key=AST
| Studies of early-type variable stars. I - The ellipsoidal and Beta Cephei variable HD 149881 /V 600 Her/
Fifty years of spectroscopic data are used to determine an orbit for theellipsoidal variable HD 149881 (V 600 Her). It is shown that this staris actually a spectroscopic binary with a period of 5.20 days andvelocity variations characteristic of Beta Cephei variables. The lightcurve and orbital data are combined to derive the orbital and physicalparameters of the system. For an assumed primary mass of 15 solarmasses, the following parameters are obtained: an orbital inclination of35 deg, a surface gravity of log g = 3.26, a primary radius of 15 solarradii, a secondary mass of two solar masses, a bolometric magnitude (forthe whole system) of -8.1, an absolute visual magnitude of -5.4, and aspectral type (for the primary) of B0.5 III. The evolutionary state ofBeta Cephei stars is reviewed, noting that such stars are probably nearthe end of hydrogen exhaustion.
| Four-color and H beta photometry of beta CEP stars and their locationin the Hertzsprung-Russel diagram.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1975A&A....41..367S&db_key=AST
| The spectral classification of the beta CEP stars and their location in the theoretical Hertzprung-Russell diagram.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1973A&A....22..229L&db_key=AST
| Atmospheric Abundances in the Beta Cephei Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1971ApJ...169..343W&db_key=AST
| 57th Name-List of Variable Stars
Not Available
| Distance Moduli of Open Clusters.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1965ApJS...12..215H&db_key=AST
| Polarization Measurements of the Open Clusters NGC 2169 and 7243
Not Available
| Stellar Spectra in Milky way Regions. VIII. a Region in Orion.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1959ApJS....4...23M&db_key=AST
| The Galactic Cluster NGC 2169.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1956ApJ...123...59C&db_key=AST
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Pozíciós és asztrometriai adatok
| Csillagkép: | Orion |
| Rektaszcenzió: | 06h08m18.11s |
| Deklináció: | +13°58'17.5" |
| Vizuális fényesség: | 8.096 |
| Távolság: | 598.802 parszek |
| RA sajátmozgás: | -2.2 |
| Dec sajátmozgás: | -1.3 |
| B-T magnitude: | 8.086 |
| V-T magnitude: | 8.096 |
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