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Statistical Constraints for Astrometric Binaries with Nonlinear Motion
Useful constraints on the orbits and mass ratios of astrometric binariesin the Hipparcos catalog are derived from the measured proper motiondifferences of Hipparcos and Tycho-2 (Δμ), accelerations ofproper motions (μ˙), and second derivatives of proper motions(μ̈). It is shown how, in some cases, statistical bounds can beestimated for the masses of the secondary components. Two catalogs ofastrometric binaries are generated, one of binaries with significantproper motion differences and the other of binaries with significantaccelerations of their proper motions. Mathematical relations betweenthe astrometric observables Δμ, μ˙, and μ̈ andthe orbital elements are derived in the appendices. We find a remarkabledifference between the distribution of spectral types of stars withlarge accelerations but small proper motion differences and that ofstars with large proper motion differences but insignificantaccelerations. The spectral type distribution for the former sample ofbinaries is the same as the general distribution of all stars in theHipparcos catalog, whereas the latter sample is clearly dominated bysolar-type stars, with an obvious dearth of blue stars. We point outthat the latter set includes mostly binaries with long periods (longerthan about 6 yr).
| B Star Rotational Velocities in h and χ Persei: A Probe of Initial Conditions during the Star Formation Epoch?
Projected rotational velocities (vsini) have been measured for 216 B0-B9stars in the rich, dense h and χ Persei double cluster and comparedwith the distribution of rotational velocities for a sample of fieldstars having comparable ages (t~12-15 Myr) and masses (M~4-15Msolar). For stars that are relatively little evolved fromtheir initial locations on the zero-age main sequence (ZAMS) (those withmasses M~4-5 Msolar), the mean vsini measured for the h andχ Per sample is slightly more than 2 times larger than the meandetermined for field stars of comparable mass, and the cluster and fieldvsini distributions differ with a high degree of significance. Forsomewhat more evolved stars with masses in the range 5-9Msolar, the mean vsini in h and χ Per is 1.5 times thatof the field; the vsini distributions differ as well, but with a lowerdegree of statistical significance. For stars that have evolvedsignificantly from the ZAMS and are approaching the hydrogen exhaustionphase (those with masses in the range 9-15 Msolar), thecluster and field star means and distributions are only slightlydifferent. We argue that both the higher rotation rates and the patternof rotation speeds as a function of mass that differentiatemain-sequence B stars in h and χ Per from their field analogs werelikely imprinted during the star formation process rather than a resultof angular momentum evolution over the 12-15 Myr cluster lifetime. Wespeculate that these differences may reflect the effects of the higheraccretion rates that theory suggests are characteristic of regions thatgive birth to dense clusters, namely, (1) higher initial rotationspeeds; (2) higher initial radii along the stellar birth line, resultingin greater spin-up between the birth line and the ZAMS; and (3) a morepronounced maximum in the birth line radius-mass relationship thatresults in differentially greater spin-up for stars that become mid- tolate-B stars on the ZAMS.
| New periodic variables from the Hipparcos epoch photometry
Two selection statistics are used to extract new candidate periodicvariables from the epoch photometry of the Hipparcos catalogue. Theprimary selection criterion is a signal-to-noise ratio. The dependenceof this statistic on the number of observations is calibrated usingabout 30000 randomly permuted Hipparcos data sets. A significance levelof 0.1 per cent is used to extract a first batch of candidate variables.The second criterion requires that the optimal frequency be unaffectedif the data are de-trended by low-order polynomials. We find 2675 newcandidate periodic variables, of which the majority (2082) are from theHipparcos`unsolved' variables. Potential problems with theinterpretation of the data (e.g. aliasing) are discussed.
| 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.
| Velocity Distribution of Stars in the Pup-CMa Association
The distribution of proper motions of stars in the Pup-CMa associationis presented. The stars' velocities are approximately parallel to eachother, which indicates that the stars are close together in space. Themutual distribution of stars and molecular clouds in the association isinterpreted as proof that the stars emerged from a single giganticprimordial molecular cloud (or several large clouds), destroyed byradiation and/or stellar wind coming from those stars. It is assumedthat part of that cloud is being dissipated, while part is being brokeninto several small clouds, which we are observing at present.
| New OB-Association in Pup - CMA
Not Available
| Asteroseismology of the beta Cephei stars. II. 12 (DD) Lacertae
Five pulsation modes are simultaneously excited in this well-known betaCephei star. Three of them, including the one with the largest light andradial-velocity amplitudes, form a triplet. The triplet is equidistantin frequency to within the errors of measurement, that is, 0.0003 d(-1). Explaining why the triplet should be so nearly equidistant turns outto be a real challenge to the theory. We investigate the following threeoptions: (1) rotational splitting, (2) an oblique magnetic pulsator, and(3) nonlinear phase lock. Unfortunately, apart from the frequencies, thedata are meager. Photometric indices yield the effective temperature andsurface gravity of rather low accuracy. In addition, the existingdeterminations of the spherical harmonic degree of even the strongestobserved mode are discrepant. Consequently, the model parameters are notwell constrained. We show that of the three above-mentioned options, theoblique pulsator model is unlikely because it would require excessivelystrong dipolar field or a special field geometry. The rotationalsplitting is a possibility, but only for an l = 2, p_0 mode in a modelwith specific values of the effective temperature and surface gravity.Finally, we note that the nonlinear phase lock may be the solution.However, verifying this depends on the progress of nonlinearcalculations.
| 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
| The 73rd Name-List of Variable Stars
Not Available
| The Distribution of Dust Clouds in the Interstellar Medium
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996ApJ...457..764D&db_key=AST
| 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.
| V539 Arae: first accurate dimensions of a slowly pulsating B star.
Analysis of high precision uvby light curves (Clausen et al. 1995b) ofthe detached, double-lined eclipsing binary V539 Ara has uncovered, thatits secondary component belongs to the group of slowly pulsating B (orSPB) stars (Waelkens 1991). The B4V star is situated in the instabilitydomain of the HR diagram predicted for Z=0.02 (Dziembowski et al. 1993),whereas the B3V primary, which appears stable, lies just at its border.Low amplitude oscillations with periods of 1.36, 1.78 and possibly 1.08days have been identified. The components of V539 Ara are located in thelower half of the main sequence band. New absolute dimensions have beenestablished: (M,R,logg,logT_eff_,logL) values are (6.24+/-0.07,4.50+/-0.08, 3.93+/-0.02, 4.26+/-0.01, 3.29+/- 0.05) and (5.31+/-0.06,3.42+/-0.08, 4.23+/-0.01, 2.95+/-0.06) for primary and secondary,respectively. V539 Ara is consequently among our best sources foraccurate parameters of mid-B stars. Stellar evolutionary models (Claret& Gimenez 1992a) based on OPAL opacities and including moderateovershooting fit the components very well for an assumed composition of(Y,Z)=(0.28,0.02); a common age of 4.5x10^7^yr is predicted. Models ofsignificantly lower/higher metal abundance represent the observationsless satisfactorily. The orbit of V539 Ara is slightly eccentric(e=0.053+/-0.001), and apsidal motion with a period of U=150+/-15yr hasbeen detected. Relativistic effects are negligible, and thecorresponding mean density concentration coefficientlogk_2_=-2.32+/-0.07 confirms the theoretical prediction of the Claret& Gimenez (1992a, 1993) models. For a yet unknown reason it is,however, not possible to describe all available times of minima through"normal" apsidal motion (Gimenez & Bastero 1995); more observationsare needed. The combination of well established SPB oscillations andaccurate dimensions is unique. V539 Ara appears to offer a highly neededpossibility to study the structure of convective cores and theirboundaries for intermediate mass stars. Dedicated (rotationallydeformed) models are needed, as well as further photometric observationsfor a more detailed frequency study of V539 Ara. Several other wellstudied binaries are located in or near the predicted SPB domain.Results from a critical review of their properties, a confrontation withOPAL based models, and a search for yet overlooked SPB oscillations willbe published separately (Clausen 1995).
| 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.
| The South African Astronomical Observatory.
Not Available
| The extraordinary early-type eclipsing binary HR 2680
Photometric observations of the HR 2680 (B5V) star using Stromgren-b andStromgren-uvby filters carried out in 1990 and 1991 are reported. It isfound that this star is a single-line spectroscopic binary showingpartial or annular eclipses with a period of 8.1 d. A light variationwith an amplitude of 0.03 mag can be seen outside eclipse which can beinterpreted as two oscillations, with approximate periods of about 1.19and 1.28 d, but the periods are not constant. It is suggested that thestar is a member of the 53 Per class of line-profile variables. Theextraordinary variability of HR 2680 outside eclipse makes this starunique. It is suggested that the star could be used as a test bed forstellar dynamics and nonradial pulsations.
| The 71st Name-List of Variable Stars
Not Available
| 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.
| Empirical temperature calibrations for early-type stars
Three temperature calibrations of suitable photometric quantities havebeen derived for O and B stars. A sample of 120 stars with reliableT(eff.) determinations has been used for establishing each calibration.The different calibrations have been critically discussed and compared.Temperature determinations for 1009 program stars have been obtainedwith an accuracy of the order of 10 percent.
| 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.
| The interstellar 2200 A band - A catalogue of equivalent widths
Not Available
| MK Spectral Types for Bright Southern OB Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1969ApJ...157..313H&db_key=AST
| Catalogue d'etoiles O et B.
Not Available
| Radial velocities of 200 southern B stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1965MNRAS.130..281B&db_key=AST
| Spectral types and luminosities of B, A and F southern stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1957MNRAS.117..449D&db_key=AST
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Pozíciós és asztrometriai adatok
| Csillagkép: | Nagy Kutya |
| Rektaszcenzió: | 07h06m00.60s |
| Deklináció: | -30°39'20.0" |
| Vizuális fényesség: | 6.34 |
| Távolság: | 254.453 parszek |
| RA sajátmozgás: | -11.6 |
| Dec sajátmozgás: | 4 |
| B-T magnitude: | 6.155 |
| V-T magnitude: | 6.303 |
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