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The Ca II infrared triplet as indicator of anomalous Ca isotopic mixture in HgMn stars
For the first time we present observational evidence for an anomalousisotopic structure of Ca II in mercury-manganese (HgMn) stars. Thecentroid wavelengths of Ca II infrared triplet lines in a number ofstars have been found redshifted with respect to the centroids of theterrestrial Ca II lines. The record holder is the star HD 175640 forwhich the measured wavelength is consistent with Ca II being present inthe atmosphere entirely in form of the heaviest stable isotope48Ca. This is a very striking result as 48Ca makesup only 0.187% of the terrestrial Ca mixture.Based on observations obtained at the European Southern Observator, LaSilla and Paranal, Chile (ESO programme Nos. 65.L-0316 and 67.D-0579).
| Vertical distribution of chromium in the atmospheres of HgMn stars
We use multiplet 30 Cr II lines in the wings of Hbeta totest the hypothesis of an anomalous concentration of Cr in the upperlayers of the atmospheres of a sample of 10 HgMn stars. These lines areat different distances from the H_beta line center and are thereforeformed at different depths in the stellar atmosphere. Except for HD49606, all HgMn stars show an increase in Cr abundance with height inthe stellar atmosphere. A similar vertical distribution of Cr, but lesspronounced, has been previously found in Am stars. In contrast, novariation of Cr abundance with the depth has been found for the normallate B-type star HD 196426 and the weak magnetic late B-type star HD168733. It is possible that in HgMn stars the vertical stratificationparameter, a, depends on T_eff, with the strongest vertical gradientbeing found in the hotter stars. No correlation was found between a andthe average stellar abundance log varepsilon (Cr/H).Based on observations obtained at the European Southern Observatory, LaSilla and Paranal, Chile (ESO programmes Nos. 62.L-0348, 65.I-0644,67.D-0579).
| On the elemental abundance and isotopic mixture of mercury in HgMn stars
Optical region spectra of 31 HgMn stars have been studied for theabundance and isotope mixture of mercury. In the course of theinvestigation the lines Hg I lambda 4358 and Hg Ii lambda lambda3984,6149 have been studied, with abundances established for all threelines in several HgMn stars. The mercury isotope mixture has beendetermined from high resolution spectra of the lambda 3984 line.Possible signs of an ionization anomaly have been detected by thecomparison of the abundance derived from the Hg I line and the Hg Iilines in seven of the observed HgMn stars. A possible correlation of themercury abundance with Teff has been detected. Possible signsof a weak anticorrelation of the manganese and mercury abundance in HgMnstars have been found, which could be interpreted as a sign ofinhomogeneous surface distribution of these elements. For a number ofthe HgMn stars in this study the mercury abundance and isotope mixtureare reported for the first time.
| The presence of Nd and Pr in HgMn stars
Optical region spectra for a number of upper main sequence chemicallypeculiar (CP) stars have been observed to study singly and doublyionized praseodymium and neodymium lines. In order to improve existingatomic data of these elements, laboratory measurements have been carriedout with the Lund VUV Fourier Transform Spectrometer (FTS). From thesemeasurements wavelengths and hyperfine structure (hfs) have been studiedfor selected Pr Ii, Pr Iii and Nd Iii lines of astrophysical interest.Radiative lifetimes for some excited states of Pr Ii have beendetermined with the aid of laser spectroscopy at the Lund Laser Center(LLC) and have been combined with branching fractions measured in thelaboratory to calculate gf values for some of the stronger optical linesof Pr Ii. With the aid of the derived gf values and laboratorymeasurements of the hfs, a praseodymium abundance was derived fromselected Pr Ii lines in the spectrum of the Am star 32 Aqr. Thisabundance was used to derive astrophysical gf values for selected Pr Iiilines in 32 Aqr, and these gf values were used to get a praseodymiumabundance for the HgMn star HR 7775. The praseodymium abundance in HR7775 was then utilized to derive astrophysical gf values for allobservable Pr Iii lines in this star. The neodymium abundance, derivedfrom unblended lines of Nd Ii in HR 7775, has been utilized to establishastrophysical gf values for observed Nd Iii lines in the optical regionof this star. Selected Pr Iii and Nd Iii lines have been identified andstudied in a number of HgMn stars and three hot Am stars. Thepraseodymium and neodymium abundance change rapidly from an approximate1-1.2 dex enhancement for the hot Am stars to 1.5-3 dex enhancement forthe cool HgMn stars, indicating a well-defined boundary between the hotAm and HgMn stars in the vicinity of 10 500 K. The enhancement ofpraseodymium and neodymium in Am and HgMn stars may be explained bydiffusive processes active in the stellar atmosphere, while the observeddiscontinuity might be explained by a thin hydrogen convection zonethought to be present for the Am stars, but absent in the HgMn stars.The absence of a convection zone would cause the diffused elements togather higher in the atmosphere of HgMn stars compared to Am stars, andexplain the observed increase in abundance.
| Search for magnetic fields in HgMn stars by using relative strengths of multiplet 74 Fe II lines
The anomalous strength of the Fe II lambda 6147.7 line relative to Fe IIlambda 6149.2 in the stars with magnetic fields is used for detectingmagnetic fields in very slowly rotating HgMn stars. The diagnosis basedon this pair of magnetically sensitive Fe lines is a simple and fasttool, but its application to more rapidly rotating HgMn stars ishampered by blending with Hg II lambda 6149.5. For spectra ofsharp-lined HgMn stars (with v sin i<4 km s(-1) ) taken at highresolving power (R>= 100 000) both lines, Fe II lambda 6149.25 and HgII lambda 6149.48, become fully unblended. The observed relativedifferences between the equivalent widths of the two Fe II lines arecompared with those derived from synthetic spectra computed byneglecting magnetic field effects. This comparison has shown that threeHgMn stars, HD 175640, HD 178065 and HD 186122 are very likely topossess a magnetic field that could be larger than 2 kG. Based onobservations obtained at the European Southern Observatory, La Silla,Chile (ESO programme No.~61.D-0480)
| 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.
| 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.
| 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.
| A study of visual double stars with early type primaries. IV Astrophysical data
Astrophysical parameters (MK class, color excess, absolute magnitude,distance, effective temperature, mass, and age) are derived fromcalibrations of the uvby-beta indices for the members of 253 doublestars with O or B type primaries and faint secondaries. The photometricspectral classification is compared to the MK classes, and the agreementis very good. The derived data together with spectroscopic and JHKL dataare used for deciding which pairs are likely to be physical and whichare optical, and it is shown that 98 (34 percent) of the secondaries arelikely to be members of physical systems. For 90 percent of the physicalpairs the projected separation between the components is less than25,000 AU. A majority of the physical secondaries are late-type stars,and 50 percent of them are contracting towards the zero-agemain-sequence. Also presented are new uvby-beta data for 43 secondariesand a computer program for determining astrophysical parameters fromuvby-beta data.
| A study of visual double stars with early type primaries. II - Photometric results
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1983A&AS...51..161L&db_key=AST
| A study of visual double stars with early type primaries. I - Spectroscopic results
Attention is given to spectral peculiarities found in data on thespectral classes of 486 stars in 254 visual doublet or multiplet systemswith O or B type primaries, in order to isolate a group of very youngstars that may serve for the study of early stellar evolutioncharacteristics. It is noted that the material contains a substantialfraction of secondaries that are likely to be physical, and that severalof these may be in the premain-sequence phase of stellar evolution, orhave reached the zero-age main sequence.
| Intermediate band photometry of early-type stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1977PASP...89..205E&db_key=AST
| 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
| Combined-light UBV Photometry of 103 Bright Southern Visual Doubles
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