Evolution of interacting binaries with a B type primary at birth
We revisited the analytical expression for the mass ratio distributionfor non-evolved binaries with a B type primary. Selection effectsgoverning the observations were taken into account in order to comparetheory with observations. Theory was optimized so as to fit best withthe observed q-distribution of SB1s and SB2s. The accuracy of thistheoretical mass ratio distribution function is severely hindered by theuncertainties on the observations. We present a library of evolutionarycomputations for binaries with a B type primary at birth. Some liberalcomputations including loss of mass and angular momentum during binaryevolution are added to an extensive grid of conservative calculations.Our computations are compared statistically to the observeddistributions of orbital periods and mass ratios of Algols. ConservativeRoche Lobe Over Flow (RLOF) reproduces the observed distribution oforbital periods but fails to explain the observed mass ratios in therange q in [0.4-1]. In order to obtain a better fit the binaries have tolose a significant amount of matter, without losing much angularmomentum.
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New Estimates of the Solar-Neighborhood Massive Star Birthrate and the Galactic Supernova Rate
The birthrate of stars of masses >=10 Msolar is estimatedfrom a sample of just over 400 O3-B2 dwarfs within 1.5 kpc of the Sunand the result extrapolated to estimate the Galactic supernova ratecontributed by such stars. The solar-neighborhood Galactic-plane massivestar birthrate is estimated at ~176 stars kpc-3Myr-1. On the basis of a model in which the Galactic stellardensity distribution comprises a ``disk+central hole'' like that of thedust infrared emission (as proposed by Drimmel and Spergel), theGalactic supernova rate is estimated at probably not less than ~1 normore than ~2 per century and the number of O3-B2 dwarfs within the solarcircle at ~200,000.
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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.
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Catalog of Galactic OB Stars
An all-sky catalog of Galactic OB stars has been created by extendingthe Case-Hamburg Galactic plane luminous-stars surveys to include 5500additional objects drawn from the literature. This work brings the totalnumber of known or reasonably suspected OB stars to over 16,000.Companion databases of UBVβ photometry and MK classifications forthese objects include nearly 30,000 and 20,000 entries, respectively.
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The relation between far-UV and visible extinctions
For directions of sufficient reddening (/E(B-V)>~0.25), there is asimple relation between the slope of the extinction curve in the far-UVand /E(B-V). Regardless of direction, the far-UV extinction curve isproportional to 1/λn e-2E(B-V)/λ(/λ in μm, /n=4), in accordance with the idea that reddenedstars spectra are contaminated by scattered light (Zagury, 2001b). Thisrelation is not compatible with the standard theory of extinction whichstates that far-UV and visible extinctions are due to different classesof particle. In that model the two (far-UV and visible) extinctions varythus independently according to the proportion of each type of particle.In preceding papers I have shown that the standard theory cannot explainUV observations of nebulae, and is contradicted by the UV spectra ofstars with very low reddening: for how long shall the standard theory beconsidered as the interpretation of the extinction curve?
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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.
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UBV beta Database for Case-Hamburg Northern and Southern Luminous Stars
A database of photoelectric UBV beta photometry for stars listed in theCase-Hamburg northern and southern Milky Way luminous stars surveys hasbeen compiled from the original research literature. Consisting of over16,000 observations of some 7300 stars from over 500 sources, thisdatabase constitutes the most complete compilation of such photometryavailable for intrinsically luminous stars around the Galactic plane.Over 5000 stars listed in the Case-Hamburg surveys still lackfundamental photometric data.
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UBVRI-CCD photometry of Cepheus OB3 association.
Johnson CCD photometry was performed in the two subgroups of theassociation Cepheus OB3, for selected fields each containing at leastone star with previous UBV photoelectric photometry. Photometry forabout 1000 stars down to visual magnitude 21 is provided, although thecompleteness tests show that the sample is complete down to V=19mag.Individual errors were assigned to the magnitude and colours for eachstar. Colour-colour and colour-magnitude diagrams are shown. Astrometricpositions of the stars are also given. Description of the reductionprocedure is fully detailed.
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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.
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Environment Dependence of Interstellar Extinction Curves
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1993A&A...274..439J&db_key=AST
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Hα Interferometric Optical and Near Infrared Photometric Studies of Star Forming Regions - Part One - the Cepheus-B / SH:2-155 / CEPHEUS-OB3 Association Complex
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1993A&A...273..619M&db_key=AST
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A photometric analysis of the Cepheus OB3 region
Results are presented on Stromgren-Crawford uvby-beta photometry carriedout at Calar Alto (Spain) for 45 stars in the Cepheus OB3 regioncovering an apparent area of 6 deg x 6 deg. The relationship of thesestars with the association is examined. Three of these stars (BD +62 deg2114, BD +62 deg 2152, and BD +62 deg 2156) are identified as members ofthis association, while two more (BD +64 deg 1714 and BD +64 deg 1717)are classified as possible members. It is noted that intrinsic colorsand absolute magnitudes of member stars are consistent with thehypothesis of Blaauw (1964) and Garmany (1973) of the existence of twosubgroups with different evolutionary phases.
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An Einstein Observatory SAO-based catalog of B-type stars
About 4000 X-ray images obtained with the Einstein Observatory are usedto measure the 0.16-4.0 keV emission from 1545 B-type SAO stars fallingin the about 10 percent of the sky surveyed with the IPC. Seventy-fourdetected X-ray sources with B-type stars are identified, and it isestimated that no more than 15 can be misidentified. Upper limits to theX-ray emission of the remaining stars are presented. In addition tosummarizing the X-ray measurements and giving other relevant opticaldata, the present extensive catalog discusses the reduction process andanalyzes selection effects associated with both SAO catalog completenessand IPC target selection procedures. It is concluded that X-rayemission, at the level of Lx not less than 10 exp 30 ergs/s, is quitecommon in B stars of early spectral types (B0-B3), regardless ofluminosity class, but that emission, at the same level, becomes lesscommon, or nonexistent, in later B-type stars.
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Galactic OB associations in the northern Milky Way Galaxy. I - Longitudes 55 deg to 150 deg
The literature on all OB associations was reviewed, and their IRAS pointsource content was studied, between galactic longitude 55 and 150 deg.Only one third of the 24 associations listed by Ruprecht et al. (1981)have been the subject of individual studies designed to identify thebrightest stars. Distances to all of these were recomputed using themethod of cluster fitting of the B main sequence stars, which makes itpoossible to reexamine the absolute magnitude calibration of the Ostars, as well as for the red supergiant candidate stars. Also examinedwas the composite HR diagram for these associations. Associations withthe best defined main sequences, which also tend to contain very youngclusters, referred to here as OB clusters, have extremely few evolved Band A or red supergiants. Associations with poorly defined mainsequences and few OB clusters have many more evolved stars. They alsoshow an effect in the upper HR diagram referred to as a ledge byFitzpatrick and Garmany (1990) in similar data for the Large MagellanicCloud. It is suggested that the differences in the associations are notjust observational selection effects but represent real differences inage and formation history.
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Close binaries observed polarimetrically
Not Available
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Atlas of the wavelength dependence of ultraviolet extinction in the Galaxy
The paper presents a collection of 115 extinction curves derived fromlow-dispersion IUE spectra. The spectra have been reduced with the useof techniques designed to reduce the effects of random noise and theinfluence of residual spectral features due to classification mismatch.The magnitudes of other instrumental and interpretational uncertaintiesare estimated. The extinction curves are presented with normalization toE(B-V) = 1 and the FUV portion (below 170 nm) is also shown for E(13-17)= 1. The atlas includes examples of extinction originating in thediffuse medium and several major nebulae and dense clouds.
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The interstellar 217 NM band - A third catalogue of equivalent widths
A catalog of equivalent widths of the 217 nm interstellar absorptionband as well as other parameters characterizing the extinction curve inthe ultraviolet has been compiled for 790 O and B stars. A relativelytight correlation between the equivalent width of the 217 nm band andE(B-V) indicates that the absorber of this band is connected with thepopulation of larger interstellar grains responsible for the visualextinction. The parameter characterizing the amount of extinction in thefar UV is only weakly correlated with E(B-V), a result in accord withthe assumption that a second population of very small grains causes therapid increase of the far-UV extinction.
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A catalog of ultraviolet interstellar extinction excesses for 1415 stars
Ultraviolet interstellar extinction excesses are presented for 1415stars with spectral types B7 and earlier. The excesses with respect to Vare derived from Astronomical Netherlands Satellite (ANS) 5-channel UVphotometry at central wavelengths of approximately 1550, 1800, 2500, and3300 A. A measure of the excess extinction in the 2200-A extinction bumpis also given. The data are valuable for investigating the systematicsof peculiar interstellar extinction and for studying the character of UVinterstellar extinction in the general direction of stars for which theextinction-curve shape is unknown.
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Ultraviolet observations of interstellar extinction near the Cepheus OB3 molecular cloud
New IUE observations and available data for O and B stars new Cep OB3are presented, and extinction curves for the stars are derived. Thedifferences in those curves are examined in detail, showing that whilethe level of the far-UV extinction differs greatly throughout theregion, the shape of the 2175 A bump does not. The different curves forma family which can be parametrized by the strength of the bump perE(B-V). This suggests that some single physical process dominates themodification of the grains in the region. Evidence is presented whichindicates that this process is related to the evolution of the grainsonce they emerge from the Cep OB3 molecular cloud. The practicality ofusing the strength of the bump per E(B-V) for dereddening stars in aregion where the form of the UV extinction differs from place to placeis demonstrated.
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The interstellar 2200-A band - A second catalogue of equivalent widths and preliminary statistical analysis
A second catalogue of equivalent widths of the interstellar 2200-A bandis presented. It is based on spectrophotometric data obtained with theTD-I satellite and supplements the catalogue of Guertler et al. (1982).Both catalogues list a total of 779 stars. The reliability of thederived parameters is analyzed. There is a satisfying agreement withspectrophotometric data obtained with the OAO-2 satellite. Therelationship between the equivalent width of the 2200-A band and thecolor excess is discussed, making use of additional data for morestrongly reddened stars obtained with OAO-2 and IUE.
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The graphite rich Cepheus OB 3 association
The four optically brightest stars of the Cepheus OB 3 association havebeen observed with the IUE satellite in the spectral range 1150-3200 A.The extinction suffered by the stars has been investigated. Both theshape of the bump at approximately 2200 A and the behavior of theextinction at longer wavelengths are close to those of the meaninterstellar curve. The behavior shortward of 2000 A is peculiar andreveals the existence of a component of dust which belongs to theassociation. A fit with theoretical extinction curves shows that astrong excess of graphite relative to silicates in the local componentis required to explain the observed extinction in the Cepheus OB 3association.
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Anomalous extinction in the Cepheus OB 3 association
The UV extinction of the four brightest stars of the Cepheus OB 3association was investigated. While the shape of the bump at 2200 A andthe extinction at longer wavelengths are close to the mean interstellarcurve, the behavior shortward of 2000 A is peculiar. A fit withtheoretical extinction curves shows that a strong excess of graphiterelative to silicates in the local component is required to explainobserved extinction in the association.
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A search for weak galactic binary X-ray sources
Observations undertaken to investigate the relation of mass transferrates to X-ray luminosities in accreting binary X-ray sources in theGalaxy are discussed. Einstein Observatory Imaging Proportional Counterobservations were made of 23 binary systems selected as possiblycontaining a compact object. Only three of the original 17 targetobjects were detected as sources, plus two more among the six also foundto be within Einstein IPC fields. None of the sources detected, however,shows evidence for the presence of a compact component. It is concludedthat there are few, if any, binaries in which a compact star is in a lowX-ray state, and that the known hard X-ray binaries constitute theentire galactic population of such objects.
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The thermal radio emission from the S 155 nebula and the Cepheus OB 3 association.
Abstract image available at:http://adsabs.harvard.edu/abs/1978A&A....69..199F
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Seventh catalogue of the orbital elements of spectroscopic binary systems.
Not Available
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Helium abundance in atmospheres of stars appearing in OB associations and young clusters
An improved version of Liubimkov's (1974) method is used to determinethe relative helium abundance, N(He)/N(H), in the atmospheres of 80stars of spectral types O6.5 to B2 belonging to OB associations andyoung clusters. Specific results are presented for Mon OB1 and OB2, CepOB2 and OB3, Sco OB2, Lac OB1, Ori OB1, and Cas OB6. It is shown thatthe mean value of N(He)/N(H) increases with increasing stellar age andincreasing cluster or association size. A relative helium abundance of0.09 to 0.10 is found to be appropriate for stars that are severalmillion years old, and a relative abundance of 0.13 is obtained forstars older than 10 million years. It is noted that the latter value isalso characteristic of hot field stars.
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On the kinematical and spatial coincidence of optical and radio spiral arms in our galaxy.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1973A&A....24..393M&db_key=AST
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Spectroscopic binaries - 12th complementary catalogue
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1973A&AS...10..105P&db_key=AST
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Internal motions in the association Cep OB3.
Abstract image available at:http://adsabs.harvard.edu/abs/1973AJ.....78..185G
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Seven new spectroscopic binaries in Cepheus.
Abstract image available at:http://adsabs.harvard.edu/abs/1972AJ.....77...38G
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