Contents
Images
Upload your image
DSS Images Other Images
Related articles
The Projected Rotational Velocity Distribution of a Sample of OB stars from a Calibration Based on Synthetic He I Lines
We derive projected rotational velocities (v sin i) for a sample of 156Galactic OB star members of 35 clusters, H II regions, and associations.The He I lines at 4026, 4388, and 4471 Å were analyzed in order todefine a calibration of the synthetic He I full widths at half-maximum(FWHMs) versus stellar v sin i. A grid of synthetic spectra of He I lineprofiles was calculated in non-LTE using an extensive helium model atomand updated atomic data. The v sin i values for all stars were derivedusing the He I FWHM calibrations, but also, for those target stars withrelatively sharp lines, v sin i values were obtained from best-fitsynthetic spectra of up to 40 lines of C II, N II, O II, Al III, Mg II,Si III, and S III. This calibration is a useful and efficient tool forestimating the projected rotational velocities of O9-B5 main-sequencestars. The distribution of v sin i for an unbiased sample of early Bstars in the unbound association Cep OB2 is consistent with thedistribution reported elsewhere for other unbound associations.
| 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.
| 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.
| Chemical Abundances of OB Stars with High Projected Rotational Velocities
Elemental abundances of carbon, nitrogen, oxygen, magnesium, aluminum,and silicon are presented for a sample of 12 rapidly rotating OB star(vsini>60kms-1) members of the Cep OB2, Cyg OB3, and CygOB7 associations. The abundances are derived from spectrum synthesis,using both LTE and non-LTE calculations. As found in almost all previousstudies of OB stars, the average abundances are slightly below solar, byabout 0.1 to 0.3 dex. In the case of oxygen, even with the recentlyderived low solar abundances, the OB stars are closer to, but stillbelow, the solar value. Results for the nine Cep OB2 members in thissample can be combined with results published previously for eight CepOB2 stars with low projected rotational velocities to yield the mostcomplete set of abundances, to date, for this particular association.These abundances provide a clear picture of both the general chemicaland individual stellar evolution that has occurred within thisassociation. By placing the Cep OB2 stars studied in an HR-diagram weidentify the presence of two distinct age subgroups, with both subgroupshaving quite uniform chemical abundances. Two stars are found in theolder subgroup that show significant N/O overabundances, with both starsbeing two of the most massive, the most evolved, and the most rapidlyrotating of the members studied in Cep OB2. These characteristics ofincreased N abundances being tied to high mass, rapid rotation, and anevolved phase are those predicted from models of rotating stars thatundergo rotationally driven mixing.
| Chemical Abundances of OB Stars in the Cepheus OB2 Association
LTE and non-LTE abundances of carbon, nitrogen, oxygen, and silicon, aswell as LTE abundances of Fe, are presented from analyses of C II, N II,O II, Si III, and Fe III lines in the spectra of eight main-sequence OBstars in the Cep OB2 association. We find that the chemical compositionof the studied stars in this association is very homogeneous: theabundances of all elements analyzed do not show significant variations,and the observed abundance dispersions can be explained in terms of theuncertainties in the analysis. The abundance results indicate that thisassociation is slightly metal poor ([Fe/H]=-0.3) with the abundances ofall studied elements being subsolar by roughly the same amount.
| Origin and Evolution of the Cepheus Bubble
We have imaged a 10 deg x 10 deg region of the Cepheus bubble in the J =1-0 line of CO and the 21 cm line of atomic hydrogen. The CO emissiondefines a giant expanding shell 120 pc in diameter, which is similar tothat seen in the IRAS sky maps. We estimate the total gas mass in theregion to be ~4 x 10^5 M_ȯ. The total kinetic energy from theobserved spread of velocities of the molecular clouds is ~10^51 ergs. Wesuggest that the members of earlier generations of massive stars in NGC7160 are responsible for the origin of the Cepheus bubble. These starscreated an expanding compressed shell of gas that became gravitationallyunstable at an age of ~7 Myr. The members of the Cepheus OB2 associationcomprise the second, intermediate generation of stars in this regionthat formed as a consequence of this instability. The numerous colorselected IRAS point sources represent the third and youngest generationof stars in this region. Our observations suggest the great importanceof sequentially triggered star formation in the region of the Cepheusbubble.
| 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.
| A New Bright Eclipsing Variable in Cepheus
Not Available
| 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.
| 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.
| Spectrophotometric investigation of OB stars in the region of the association CEP OB2
The results are given of spectrophotometric investigation of 39 OB starsin the region of the association Cep OB2. The blue (4000-4800 A)absolute spectrophotometric gradients, the color excesses in the UBVsystem, and the distances of these stars have been determined. Analysisof the results suggests that the absorbing material is basicallyconcentrated within the association itself.
| Space Distribution of Stars in a Region of Cepheus around NGC 7160
Objective prism spectral types and photographic U, B, V magnitudes havebeen determined for 1810 stars in a region of 19.5 square degrees ofCepheus centered on the galactic cluster NGC 7160. A catalogue of datatogether with identification charts is given. The magnitude limit isapproximately V= 12.5. The field contains a part of the supposed oldersubsystem of the association Cepheus OB2. The interstellar absorption inthe region is smooth. The visual absorption is 1.0 mag. at the distanceof the association for the northern part of the field, and is about 1.4mag. for the southern part. Space densities of the stars have beencomputed as a function of spectral type and distance from the sun.Concentrations of B and early A type stars are found at 800 pc from thesun. Concentrations of B and early A type stars are found at 800 pc, andan attempt was made to derive the shape of the luminosity function ofthe association subgroup.
| H-beta photometry of northern intermediate galactic latitude early-type stars and galactic structure away from the plane
Photoelectric H-beta photometry is presented for 255 early-type stars atintermediate galactic latitudes. Absolute magnitudes and distances arederived for the more luminous stars. Those with visual magnitudes lessthan or equal to 2.5 and at distances of up to 1 kpc from the galacticplane may follow the spiral structure in the plane.
| UBV photometry and MK spectral classification of northern early-type stars at intermediate galactic latitudes
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1977MNRAS.180..691H&db_key=AST
| Photoelectric photometry of early-type stars in a Milky Way field in Cepheus
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1970A&AS....2..251S&db_key=AST
| A Spectroscopic and Photometric Investigation of the Association Cepheus OB2
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1968ApJ...154..923S&db_key=AST
|
Submit a new article
Related links
Submit a new link
Member of following groups:
|
Observation and Astrometry data
| Constellation: | ケフェウス座 |
| Right ascension: | 21h50m40.63s |
| Declination: | +61°48'11.2" |
| Apparent magnitude: | 8.21 |
| Distance: | 1408.451 parsecs |
| Proper motion RA: | -5.2 |
| Proper motion Dec: | -1.9 |
| B-T magnitude: | 8.331 |
| V-T magnitude: | 8.22 |
Catalogs and designations:
|
