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Rotational Velocities of B Stars
We measured the projected rotational velocities of 1092 northern B starslisted in the Bright Star Catalogue (BSC) and calibrated them againstthe 1975 Slettebak et al. system. We found that the published values ofB dwarfs in the BSC average 27% higher than those standards. Only 0.3%of the stars have rotational velocities in excess of two-thirds of thebreakup velocities, and the mean velocity is only 25% of breakup,implying that impending breakup is not a significant factor in reducingrotational velocities. For the B8-B9.5 III-V stars the bimodaldistribution in V can be explained by a set of slowly rotating Ap starsand a set of rapidly rotating normal stars. For the B0-B5 III-V starsthat include very few peculiar stars, the distributions in V are notbimodal. Are the low rotational velocities of B stars due to theoccurrence of frequent low-mass companions, planets, or disks? Therotational velocities of giants originating from late B dwarfs areconsistent with their conservation of angular momentum in shells.However, we are puzzled by why the giants that originate from the earlyB dwarfs, despite having 3 times greater radii, have nearly the samerotational velocities. We find that all B-type primaries in binarieswith periods less than 2.4 days have synchronized rotational and orbitalmotions; those with periods between 2.4 and 5.0 days are rotating withina factor 2 of synchronization or are ``nearly synchronized.'' Thecorresponding period ranges for A-type stars are 4.9 and 10.5 days, ortwice as large. We found that the rotational velocities of the primariesare synchronized earlier than their orbits are circularized. The maximumorbital period for circularized B binaries is 1.5 days and for Abinaries is 2.5 days. For stars of various ages from 107.5 to1010.2 yr the maximum circularized periods are a smoothexponential function of age.
| Sixth Catalogue of Fundamental Stars (FK6). Part III. Additional fundamental stars with direct solutions
The FK6 is a suitable combination of the results of the HIPPARCOSastrometry satellite with ground-based data, measured over a longinterval of time and summarized mainly in the FK5. Part III of the FK6(abbreviated FK6(III)) contains additional fundamental stars with directsolutions. Such direct solutions are appropriate for single stars or forobjects which can be treated like single stars. Part III of the FK6contains in total 3272 stars. Their ground-based data stem from thebright extension of the FK5 (735 stars), from the catalogue of remainingSup stars (RSup, 732 stars), and from the faint extension of the FK5(1805 stars). From the 3272 stars in Part III, we have selected 1928objects as "astrometrically excellent stars", since their instantaneousproper motions and their mean (time-averaged) ones do not differsignificantly. Hence most of the astrometrically excellent stars arewell-behaving "single-star candidates" with good astrometric data. Thesestars are most suited for high-precision astrometry. On the other hand,354 of the stars in Part III are Δμ binaries in the sense ofWielen et al. (1999). Many of them are newly discovered probablebinaries with no other hitherto known indication of binarity. The FK6gives, besides the classical "single-star mode" solutions (SI mode),other solutions which take into account the fact that hidden astrometricbinaries among "apparently single-stars" introduce sizable "cosmicerrors" into the quasi-instantaneously measured HIPPARCOS proper motionsand positions. The FK6 gives, in addition to the SI mode, the "long-termprediction (LTP) mode" and the "short-term prediction (STP) mode". TheseLTP and STP modes are on average the most precise solutions forapparently single stars, depending on the epoch difference with respectto the HIPPARCOS epoch of about 1991. The typical mean error of anFK6(III) proper motion in the single-star mode is 0.59 mas/year. This isa factor of 1.34 better than the typical HIPPARCOS errors for thesestars of 0.79 mas/year. In the long-term prediction mode, in whichcosmic errors are taken into account, the FK6(III) proper motions have atypical mean error of 0.93 mas/year, which is by a factor of about 2better than the corresponding error for the HIPPARCOS values of 1.83mas/year (cosmic errors included).
| 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
| An extensive Delta a-photometric survey of southern B and A type bright stars
Photoelectric photometry of 803 southern BS objects in the Deltaa-system as detection tool for magnetic chemically peculiar (=CP2) starshas been carried out and compared to published spectral types. Thestatistical yield of such objects detected by both techniques ispractically the same. We show that there are several factors whichcontaminate the search for these stars, but this contamination is onlyof the order of 10% in both techniques. We find a smooth transition fromnormal to peculiar stars. Our sample exhibits the largest fraction ofCP2 stars at their bluest colour interval, i.e. 10% of all stars in thecolour range -0.19 <= B-V < -0.10 or -0.10 <= b-y < -0.05.No peculiar stars based on the Delta a-criterion were found at bluercolours. Towards the red side the fraction of CP2 stars drops to about3% for positive values of B-V or b-y with red limits roughlycorresponding to normal stars of spectral type A5. The photometricbehaviour of other peculiar stars: Am, HgMn, delta Del, lambda Boo, Heabnormal stars, as well as Be/shell stars and supergiants shows someslight, but definite deviations from normal stars. Spectroscopic andvisual binaries are not distinguished from normal stars in their Delta abehaviour. The results of this work justify larger statistical work(e.g. in open clusters) employing more time-saving photometric methods(CCD). \newpage Based on observations obtained at the European SouthernObservatory, La Silla, Chile. This research has made use of the Simbaddatabase, operated at CDS, Strasbourg, France. Table 2 is only availablein electronic form via anonymous ftp 130.79.128.5 orhttp://cdsweb.u-strasbg.fr/Abstract.html
| On the nature of the Be phenomenon. I. The case of omega Canis Majoris
The main purpose of this paper is to demonstrate the extreme complexityof the observed variations of Be stars on the example of a well-observedbright Be star omega CMa. A detailed analysis of all published radialvelocities and a representative set of photometric and spectralobservations of this star led to the following firm conclusions:\begin{itemize} At least three and possibly four different time scalesof variability of omega CMa, ranging from 1\D37 to more than 40 years,could be identified. The correct mean period of the RV and line-profilechanges is 1\D371906, not 1\D3667 as derived earlier. The brightness ofthe object and the strength of the Balmer emission vary in an apparentcycle of several thousands of days. The long-term brightness andemission-line changes can be understood as consequences of the formationand gradual dispersal of a gaseous envelope which is flattened and seenmore face-on than equator-on. During each episode, the envelope growsfrom an optically thick pseudophotosphere to a more extended andoptically thin envelope. Existence of much smaller episodes of lightbrightening which can have the same cause (though on a more limitedscale) has clearly been demonstrated. The amplitude of the 1\D37 RVcurve varies on a time scale somewhere between 10 and 300 d. Thefollowing conclusions are less certain and represent possiblealternatives to be tested by future, systematic and homogeneousobservations: \begin{itemize} Some evidence is presented that theamplitude of the 1\D372 RV variations, local mean RV and brightness ofthe object, prewhitened for the long-term changes, all vary on a timescale of about 35 d, possibly with a period of 34\D675. The O-Cdeviations of the local epochs of RV maxima from a linear ephemeris forthe 1\D372 period seem to be undergoing a slow and probably cyclicvariation in time, being shortest at times when the star is brightestand when a new Be envelope begins to grow. However, the same O-Cdeviations can also be reconciled with the 34\D675 period. Whatever thetrue timescale of the O-C deviations is, their behaviour can also besimulated as an interference of several periods, the second mostsignificant period being close to 1\D35. Several reasons are given whythe explanation in terms of one variable period appears more probable.With the help of both, real and artificial data it is demonstrated thatthe slow variation of the 1\D3719 period -- if unrecognized -- may bemisinterpreted for a multiperiodic variation with several close periodsbetween 1\D3 and 1\D45. This constitutes a methodological warning forthe period analyses of data on some \bn, Be and ``slowly pulsating" Bstars. The cause(s) of the variations with the 1\D37 (and 1\D345)period(s) and/or the 35 d cycle remain unexplained. It is obvious,however, that these three periods are not mutually independent. The34\D675 period may be either a real physical period or a beat periodbetween the 1\D372 and 1\D345 periods. In the former case, omega CMacould be a 34\D7 binary in an eccentric orbit and the periods twicelonger than the two periods near 1\D4 would represent the sidereal andsynodic rotational periods of the Be primary. Finally, some speculationsare offered in terms of a hierarchical multiple system of three or evenfour stars.
| The discovery of a new massive O-type close binary: tau CMa (HD 57061), based on HIPPARCOS and Walraven photometry
We present an interpretation of Hipparcos Hp and Walraven VBLUWphotometry of the brightest star in the open cluster NGC 2362 (althoughnot necessarily associated with this cluster), HD 57061 (30tau CMa, HR2782, HIP 35415). In this multiple system the central component consistof a visual double star, two O-type stars separated by 0\farcs 151,which is also known to be a 154\fd 9 period single lined spectroscopicbinary. It is now shown that this system also contains a massive closebinary with a period of 1\fd 282122, most probably as the main componentof the spectroscopic binary. This system therefore contains both thelongest period spectroscopic binary and the shortest period eclipsingbinary known for O-type stars. The shape of the light curve ischaracteristic for heavily distorted double star components. An estimatehas been made for various physical parameters of the system. The systemseems to be typical for some binary interaction results obtained inN-body simulations for open clusters. Improved ephemeris are providedfor two similar stars that were observed around the same time as HD57061: HD 57060 and HD 167971. Based on observations made with the ESAHipparcos satellite, and on observations collected at the EuropeanSouthern Observatory, La Silla, Chile
| The ROSAT all-sky survey catalogue of optically bright OB-type stars.
For the detailed statistical analysis of the X-ray emission of hot starswe selected all stars of spectral type O and B listed in the Yale BrightStar Catalogue and searched for them in the ROSAT All-Sky Survey. Inthis paper we describe the selection and preparation of the data andpresent a compilation of the derived X-ray data for a complete sample ofbright OB stars.
| Derivation of the Galactic rotation curve using space velocities
We present rotation curves of the Galaxy based on the space-velocitiesof 197 OB stars and 144 classical cepheids, respectively, which rangeover a galactocentric distance interval of about 6 to 12kpc. Nosignificant differences between these rotation curves and rotationcurves based solely on radial velocities assuming circular rotation arefound. We derive an angular velocity of the LSR of{OMEGA}_0_=5.5+/-0.4mas/a (OB stars) and {OMEGA}_0_=5.4+/-0.5mas/a(cepheids), which is in agreement with the IAU 1985 value of{OMEGA}_0_=5.5mas/a. If we correct for probable rotations of the FK5system, the corresponding angular velocities are {OMEGA}_0_=6.0mas/a (OBstars) and {OMEGA}_0_=6.2mas/a (cepheids). These values agree betterwith the value of {OMEGA}_0_=6.4mas/a derived from the VLA measurementof the proper motion of SgrA^*^.
| 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.
| SANTIAGO 91, a right ascension catalogue of 3387 stars (equinox J2000).
The positions in right ascension of 3387 stars belonging to the Santiago67 Catalogue, observed with the Repsold Meridian Circle at Cerro Calan,National Astronomical Observatory, during the period 1989 to 1994, aregiven. The average mean square error of a position, for the wholeCatalogue, is +/-0.009 s. The mean epoch of the catalogue is 1991.84.
| Long-term photometry of Be stars. I. Fading events and variations on time scales of years.
Stroemgren differential uvby photometry of 7 Be stars was analyzed. Thedata were taken during 1983-1991 by the Long-Term Photometry ofVariables team at La Silla. Two low v.sin(i) stars (27 CMa and 28 CMa)showed fading events-that is, sudden fading of a few weeks duration-thatwere preceded by quasi-periodic oscillations (QPO) on time scalesT~10-20 days and amplitudes up to 0.2mag. In both cases the colorvariations indicated occurrence of dust ejections. QPO were observedalso in 48 Lib and in ɛ Cap, but these were not related to anyfading event. Long-term photometric variations up to 0.6mag amplitudewere seen for all stars. In most cases, these variations were larger inthe u band, the stars being bluest when brightest. The Be stars seems tofollow a fixed track in the c1-(b-y) color plane. The b-y color is notvery sensitive to changes in brightness, whereas the c1 color isstrongly correlated with the u magnitude. Moreover, the largest c1changes, compared with u changes, occurred in high v sin i Be stars withshell characteristics. Additional variations on time scales of days werealways present; these were larger in the u band. HR 3237 shows peculiarphotometric variations, being the exception to the behaviour abovedescribed. The amplitudes of short-term and long-term variations of 13Be stars are correlated; the tightest correlation was found in the yband. We discuss long-term photometric variations and quasi-periodicoscillations as due to enhanced mass loss episodes preceded by globalone-armed thin-disk oscillations, which could be excited by some type ofphotospheric activity.
| Longterm Photometry of Variables at ESO - Part Two - the Second Data Catalogue 1986-1990
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1993A&AS..102...79S&db_key=AST
| Fifth fundamental catalogue. Part 2: The FK5 extension - new fundamental stars
The mean positions and proper motions for 3117 new fundamental starsessentially in the magnitude range about 4.5 to 9.5 are given in thisFK5 extension. Mean apparent visual magnitude is 7.2 and is on average2.5 magnitudes fainter then the basic FK5 which has a mean magnitude of4.7. (The basic FK5 gives the mean positions and proper motions for theclassical 1535 fundamental stars). The following are discussed: theobservational material, reduction of observations, star selection, andthe system for the FK5 extension. An explanation and description of thecatalog are given. The catalog of 3117 fundamental stars for the equinoxand epoch J2000.0 and B1950.0 is presented. The parallaxes and radialvelocities for 22 extension stars with large forecasting effects aregiven. Catalogs used in the compilation of the FK5 fundamental catalogare listed.
| Long-term photometry of variables at ESO. I - The first data catalogue (1982-1986)
This paper presents the catalog of photometric data in the Stromgrensystem obtained during the first four years (October 1982 - September1986) of the Long-Term Photometry of Variables (LTPV) program at ESO.The data are available in computer-readable form.
| Walraven photometry of nearby southern OB associations
Homogeneous Walraven (VBLUW) photometry is presented for 5260 stars inthe regions of five nearby southern OB associations: Scorpio Centaurus(Sco OB2), Orion OB1, Canis Major OB1, Monoceros OB1, and Scutum OB2.Derived V and (B - V) in the Johnson system are included.
| Light variations of massive stars (Alpha Cygni variables). IX
High-precision VBLUW photometry of 22 highly luminous OBA-type stars, 13of which are Alpha Cygni variables and two of which are variable only incolor, is presented. It is suggested that sigma (V-B) increases fasterthan sigma (B-L) with later spectral types due to the absence ofstochastic metal line strength variations in the V band. It is assumedthat short-time-scale stellar spot activity is present, or thattemperature and density waves move through the atmospheres with the sametime scales, producing these line strength variations independent of thecontinuum variations. The possibility of differentiating stars which lieclose to each other in the HR diagram but have different evolutionaryhistories (and thus different metal abundances) with the aid of themaximum light amplitude/sigma (V-B) diagram is considered.
| An investigation of the micro variations of highly luminous OBA type stars (Alpha Cygni variables). VII - The two interacting O type eclipsing binaries UW CMa = HD 57060 and HD 167971
Photometric VBLUW observations of two interacting O type binaries, UWCMa and HD 167971, were obtained with the 90-cm Dutch ESO telescope atLa Silla. For UW CMa, evidence is found for the existence of plasmastreams, and the light amplitude of the optical microvariations,probably originating mainly from the O8.5I component, is about twice aslarge as for nondistorted stars of the same temperature. Themicrovariations superimposed on the light curve of HD 167971 probablyoriginate on the more distant component of the triple system and are ofnormal size.
| Instrumental effects and the Stroemgren photometric system
The extent to which the use of different photometers can affect resultson stellar color indices was investigated by simultaneously observing asample of widely different stars with several uvby photometric systemsavailable at the ESO, La Silla, Chile. In one instance, the ESO 50-cmtelescope and the four-channel photometer at the Danish 50-cm telescopewere used simultaneously. The reductions were performed separately oneach data set, using a linear color transformation procedure. Theresults agree with theoretical investigations which showed thatsubstantial errors can arise from the nonconformity of passbands. It isemphasized that it is necessary to use separate color transformationsfor various stellar types and classes and for different interstellarreddenings.
| An investigation of the micro-variations of highly luminous OBA type stars. I
Photometric observations of eight OBA stars of absolute bolometricmagnitude brighter than -7 mag, obtained during the Walraven five-colorsimultaneous VBLUW photometer with a 16-arcsec aperture on the 90-cmDutch Light Collector at ESO since 1980 are reported. The data-reductionprocedures are explained; the stability of the comparison stars ischaracterized; and the data are presented in tables and graphs.Brightness variations of 0.01-0.1 mag on time scales of days or weeksare observed in all eight objects, the mean error of the nightlyaverages being about + or - 0.002 mag, and a secular decrease of 0.012mag over about 2 yr is found for HD 37022. The larger variations seen inthe B-U color indices of some of the stars are attributed toshort-period (days or less) variations in temperature and/or densitynear the stellar surfaces.
| The local system of early type stars - Spatial extent and kinematics
Published uvby and H-beta photometric data and proper motions arecompiled and analyzed to characterize the structure and kinematics ofthe bright early-type O-A0 stars in the solar vicinity, with a focus onthe Gould belt. The selection and calibration techniques are explained,and the data are presented in extensive tables and graphs and discussedin detail. The Gould belt stars of age less than 20 Myr are shown togive belt inclination 19 deg to the Galactic plane and node-lineorientation in the direction of Galactic rotation, while the symmetricaldistribution about the Galactic plane and kinematic properties (purecircular differential rotation) of the belt stars over 60 Myr oldresemble those of fainter nonbelt stars of all ages. The unresolveddiscrepancy between the expansion observed in the youngest nearby starsand the predictions of simple models of expansion from a point isattributed to the inhomogeneous distribution of interstellar matter.
| Be stars in binaries
The known companions to 80 Be stars and 355 B stars listed in the BrightStar Catalogue in the range B1-B7 III-V and north of delta = -30 deg areconsidered. The known near-absence of Be binaries with periods less than1/10 yr is confirmed. For longer periods up to the limit of 10,000 AU ofthis survey, the Be and B stars do not differ in binary frequencies.This result implies that during pre-main-sequence contraction, the tidalbraking in binaries wider than 0.5 AU was inadequate to prevent theformation of stars with nearly the break-up rotational velocities. Thefraction of Be and B stars that have companions is higher in clustersand associations (38 percent) than among field stars (25 percent),confirming that escapees from clusters tend to be single stars. There issome evidence that the companions of Be stars that occur in the sameluminosity range tend also to be Be stars; that result was expectedbecause in visual binaries there is a known tendency for rapidlyrotating primaries to have rapidly rotating secondaries.
| Radial velocities of bright southern stars. I - 139 B-type HR and FK stars
Radial velocity determinations for 139 southern B stars in the BrightStar, FK4, and FK4 Supplement catalogues and for 53 bright southernlate-type stars are presented, based on coudespectrograms taken with theESO 1.5 m telescope at La Silla. The programs, observations,measurements, and reductions are described. Among the data presented arethe visual magnitude, spectral class, mean error, E/T variabilityparameter, velocity of interstellar lines, and rotation class.
| The region of NGC 2287 and CR 121
Intermediate band and H-beta observations of 135 stars in the regions ofthe clusters NGC 2287 and Cr 121 are discussed, and a luminositycalibration of photometric parameters for late G- to early K-type brightgiants and supergiants is introduced. Results indicate that NGC 2287 isat a distance of 740 pc, very little reddened, 100-million years old,and contains three or four G8-K2 bright giants and supergiants and ablue straggler. Cr 121 is 1.17 kpc distant, very little reddened, 1.5million years old and an extension of CMa OB1. Cr 121 contains a nearerconcentration of stars at the same distance as NGC 2287, and theassociation appears to be the same age as CMa OB1, although presequencestars may exist. Intermingling of stars in CMa OB2 and NGC 2287 is alsoconsidered possible, and a test of the calibration of two methods ofluminosity determination of early A-type stars using photometricparameters shows them to be entirely consistent.
| Space velocities and ages of nearby early-type stars
Photometric distances and space velocities have been calculated for 458B0-A0 stars with apparent magnitudes not exceeding 6.5. UsingStromgren's ubvy-beta photometry the effective temperature and theposition in bolometric magnitude over the zero-age main sequence of thestars were derived. These quantities were used to obtain age and massfor 423 of the stars by interpolation in the models of stellar evolutionfor the chemical composition (X Z) = (0.7, 0.03). A relation forderiving interstellar reddening for normal stars in the intermediategroup is given.
| Spectral classification from the ultraviolet line features of S2/68 spectra. II - Late B-type stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1977A&AS...30...71C&db_key=AST
| Five-channel photometry of cepheids and supergiants in the southern Milky Way.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1976A&AS...24..413P&db_key=AST
| Line strengths for southern OB stars-II. Observations with moderate dispersion
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1969MNRAS.144...31B&db_key=AST
| Radial velocities of southern OB stars and supergiants
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1969MNRAS.143....1B&db_key=AST
| Observations of the Infrared Object, VY Canis Majoris
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1969ApJ...158..619H&db_key=AST
| Collinder 121: a Young Southern Open Cluster Similar to H and χ Persei
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1967ApJ...149..107F&db_key=AST
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Osservazione e dati astrometrici
| Costellazione: | Cane Maggiore |
| Ascensione retta: | 07h25m25.30s |
| Declinazione: | -25°13'04.0" |
| Magnitudine apparente: | 5.78 |
| Distanza: | 990.099 parsec |
| Moto proprio RA: | -7.1 |
| Moto proprio Dec: | 0.2 |
| B-T magnitude: | 5.646 |
| V-T magnitude: | 5.764 |
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