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A high-resolution spectroscopy survey of β Cephei pulsations in bright stars
We present a study of absorption line-profile variations in early-B typenear-main-sequence stars without emission lines. We have surveyed atotal of 171 bright stars using the Nordic Optical Telescope (NOTSA),William Herschel Telescope (ING) and Coudé Auxiliary Telescope(ESO). Our sample contains 75% of all O9.5-B2.5 III-V non-emission-linestars brighter than 5.5 mag. We obtained high signal-to-noise,high-resolution spectra of the SiIII λ4560 triplet - for 125stars of our sample we obtained more than one spectrum - and examinedthese for pulsational-like line-profile variations and/or structure. Weconclude that about half of our sample stars show evidence forline-profile variations (LPV). We find evidence for LPV in about 65% ofour sample stars brighter than V=5.5. For stars with rotationalbroadening V sin i 100 km s-1, we find evidence for LPVin about 75% of the cases. We argue that it is likely that these LPV areof pulsational origin, and that hence more than half of thesolar-neighbourhood O9.5-B2.5 III-V stars is pulsating in modes that canbe detected with high-resolution spectroscopy. We detected LPV in 64stars previously unknown to be pulsators, and label these stars as newβ Cep candidates. We conclude that there is no obvious differencein incidence of (pulsational) LPV for early-B type near-main-sequencestars in binaries or in OB associations, with respect to single fieldstars.
| New runaway OB stars with HIPPARCOS
A Monte Carlo method for detection of runaway OB stars fromobservational data is proposed. 61 runaway OB star candidates have beendetected by an analysis of Hipparcos proper motions. The peculiartangential and total transverse velocities have been determined forthese stars. A list of the detected runaway star candidates ispresented. The evidence of a discrepancy between photometric andparallactic distances of runaway OB star candidates is presented.
| CHARM2: An updated Catalog of High Angular Resolution Measurements
We present an update of the Catalog of High Angular ResolutionMeasurements (CHARM, Richichi & Percheron \cite{CHARM}, A&A,386, 492), which includes results available until July 2004. CHARM2 is acompilation of direct measurements by high angular resolution methods,as well as indirect estimates of stellar diameters. Its main goal is toprovide a reference list of sources which can be used for calibrationand verification observations with long-baseline optical and near-IRinterferometers. Single and binary stars are included, as are complexobjects from circumstellar shells to extragalactic sources. The presentupdate provides an increase of almost a factor of two over the previousedition. Additionally, it includes several corrections and improvements,as well as a cross-check with the valuable public release observationsof the ESO Very Large Telescope Interferometer (VLTI). A total of 8231entries for 3238 unique sources are now present in CHARM2. Thisrepresents an increase of a factor of 3.4 and 2.0, respectively, overthe contents of the previous version of CHARM.The catalog is only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/431/773
| Anomalous dust-to-gas ratios in the Galaxy
Lines of sight with E(B-V)/N(HI) considerably smaller than the averagevalue for the solar neighbourhood have been selected from the catalogueof Diplas & Savage. In order to develop quantitative considerations,estimates of the molecular hydrogen column density were obtained usingthe relation of Savage et al. extended at E(B-V) > 0.4 with therecent data of Rachford et al. Contrary to the prevailing opinion in theliterature for sightlines with similar behaviour, we found that only 22per cent of our sample was characterized by both an average gas densitylarger than 1 cm-3 and a value of RV larger thanthat in the diffuse interstellar medium. By computing extinction models,we were able to fit the E(B-V)/N(HI) by changing the value ofRV only for some sightlines. For the remaining ones, aρd/ρH ratio different from the averageGalactic value must be invoked. The application of the Kramers-Kronigrelation to the observed extinction curves confirmed this possibility.Moreover, attempts to fit such curves with models having grain volumescorresponding to the standard ρd/ρH ratiofailed.We find a linear relation between ρd/ρHand E(B-V)/N(H) for our sightlines. The average Galactic value marks theseparation into two groups characterized by lower abundances of C and Sitrapped into the grains when E(B-V)/N(H) is smaller than the Galacticvalue, and by larger abundances when E(B-V)/N(H) is greater.
| Statistics of the Instability Strip of β Cephei Stars
We present a study of the β Cephei instability strip based on asample of 49 stars of this type. After deriving their effectivetemperatures and luminosities from their observed (B-V), (U-B) colorsand parallaxes we find their positions in the HR diagram to be mostlyconfined to the main sequence, and their masses to lie between 7Mȯ and 30 Mȯ. Their distribution on theHR diagram matches well with our previous theoretical instability stripwhich has an upper bound in the luminosity and rather tight boundariesin the effective temperature.
| 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.
| CHARM: A Catalog of High Angular Resolution Measurements
The Catalog of High Angular Resolution Measurements (CHARM) includesmost of the measurements obtained by the techniques of lunaroccultations and long-baseline interferometry at visual and infraredwavelengths, which have appeared in the literature or have otherwisebeen made public until mid-2001. A total of 2432 measurements of 1625sources are included, along with extensive auxiliary information. Inparticular, visual and infrared photometry is included for almost allthe sources. This has been partly extracted from currently availablecatalogs, and partly obtained specifically for CHARM. The main aim is toprovide a compilation of sources which could be used as calibrators orfor science verification purposes by the new generation of largeground-based facilities such as the ESO Very Large Interferometer andthe Keck Interferometer. The Catalog is available in electronic form atthe CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/386/492, and from theauthors on CD-Rom.
| EURD: The Mission and the Stellar Absolute Fluxes of B-Type Stars
We present here stellar spectra of B stars obtained with the EURDspectrograph, one of the three instruments on board MINISAT-01. EURD isa spectrograph specially designed to detect diffuse radiation in thewavelength range between 350 and 1100 Å with 5 Å spectralresolution. EURD main scientific targets are: the spectrum ofinterstellar medium, atmospheric airglow, decaying neutrinos, Moon andearly type stars.
| Research Note Hipparcos photometry: The least variable stars
The data known as the Hipparcos Photometry obtained with the Hipparcossatellite have been investigated to find those stars which are leastvariable. Such stars are excellent candidates to serve as standards forphotometric systems. Their spectral types suggest in which parts of theHR diagrams stars are most constant. In some cases these values stronglyindicate that previous ground based studies claiming photometricvariability are incorrect or that the level of stellar activity haschanged. Table 2 is only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/367/297
| On the origin of the O and B-type stars with high velocities. II. Runaway stars and pulsars ejected from the nearby young stellar groups
We use milli-arcsecond accuracy astrometry (proper motions andparallaxes) from Hipparcos and from radio observations to retrace theorbits of 56 runaway stars and nine compact objects with distances lessthan 700 pc, to identify the parent stellar group. It is possible todeduce the specific formation scenario with near certainty for twocases. (i) We find that the runaway star zeta Ophiuchi and the pulsarPSR J1932+1059 originated about 1 Myr ago in a supernova explosion in abinary in the Upper Scorpius subgroup of the Sco OB2 association. Thepulsar received a kick velocity of ~ 350 km s-1 in thisevent, which dissociated the binary, and gave zeta Oph its large spacevelocity. (ii) Blaauw & Morgan and Gies & Bolton alreadypostulated a common origin for the runaway-pair AE Aur and mu Col,possibly involving the massive highly-eccentric binary iota Ori, basedon their equal and opposite velocities. We demonstrate that these threeobjects indeed occupied a very small volume ~ 2.5 Myr ago, and show thatthey were ejected from the nascent Trapezium cluster. We identify theparent group for two more pulsars: both likely originate in the ~ 50 Myrold association Per OB3, which contains the open cluster alpha Persei.At least 21 of the 56 runaway stars in our sample can be linked to thenearby associations and young open clusters. These include the classicalrunaways 53 Arietis (Ori OB1), xi Persei (Per OB2), and lambda Cephei(Cep OB3), and fifteen new identifications, amongst which a pair ofstars running away in opposite directions from the region containing thelambda Ori cluster. Other currently nearby runaways and pulsarsoriginated beyond 700 pc, where our knowledge of the parent groups isvery incomplete.
| Intrinsically-Variable B Stars in Eclipsing Binary Systems
We have investigated the use of Hipparcos epoch photometry for studyingpossible intrinsic variability in B0-B3 stars in eclipsing binarysystems with well-determined masses.
| The Origin of Runaway Stars
Milliarcsecond astrometry provided by Hipparcos and by radioobservations makes it possible to retrace the orbits of some of thenearest runaway stars and pulsars to determine their site of origin. Theorbits of the runaways AE Aurigae and μ Columbae and of the eccentricbinary ι Orionis intersected each other ~2.5 Myr ago in the nascentTrapezium cluster, confirming that these runaways were formed in abinary-binary encounter. The path of the runaway star ζ Ophiuchiintersected that of the nearby pulsar PSR J1932+1059, ~1 Myr ago, in theyoung stellar group Upper Scorpius. We propose that this neutron star isthe remnant of a supernova that occurred in a binary system that alsocontained ζ Oph and deduce that the pulsar received a kick velocityof ~350 km s-1 in the explosion. These two cases provide thefirst specific kinematic evidence that both mechanisms proposed for theproduction of runaway stars, the dynamical ejection scenario and thebinary-supernova scenario, operate in nature.
| The Characteristics of High-Velocity O and B Stars Which Are Ejected from Supernovae in Binary Systems
We perform binary population synthesis calculations to study the originand the characteristics of runaway O and B stars which are ejected bythe supernova explosion of the companion star in a binary system. Thenumber of OB runaways can be explained from supernova ejections only ifhigh-mass stars are preferentially formed in binaries, the initial massratio distribution is strongly peaked to unity, and stars arerejuvenated to zero age upon accretion of mass from a companion star.Taking these requirements into consideration we conclude that at most30% of the runaway O stars, but possibly all runaway B stars, obtainhigh velocities due to supernovae in evolving binaries. Stars whichobtain high velocities via supernova ejections have the followingcharacteristics: (1) at least 10% of the high-velocity B stars and halfthe O stars have a mass greater than the turnoff mass of the cluster inwhich they are born and would be observed as blue stragglers in theparent cluster, (2) their equatorial rotational velocities areproportional to their space velocity, and (3) between 20% and 40% of therunaways have neutron star companions, but less than 1% are visible asradio pulsars in part of the orbit.
| A Second Catalog of Orbiting Astronomical Observatory 2 Filter Photometry: Ultraviolet Photometry of 614 Stars
Ultraviolet photometry from the Wisconsin Experiment Package on theOrbiting Astronomical Observatory 2 (OAO 2) is presented for 614 stars.Previously unpublished magnitudes from 12 filter bandpasses withwavelengths ranging from 1330 to 4250 Å have been placed on thewhite dwarf model atmosphere absolute flux scale. The fluxes wereconverted to magnitudes using V=0 for F(V)=3.46x10^-9 ergs cm^-2 s^-1Å^-1, or m_lambda=-2.5logF_lambda-21.15. This second catalogeffectively doubles the amount of OAO 2 photometry available in theliterature and includes many objects too bright to be observed withmodern space observatories.
| Bow Shocks Around Runaway Stars.III.The High Resolution Maps
In a recent survey for bow shock structures around OB runaway starsusing the ISSA/IRAS archival data and excess maps at 60 \mum, 58candidates were found. These objects are surrounded by extended infraredemission at 60 \mum, characteristic of warm dust heated by ultravioletphotons, a signature of wind bow shocks. High resolution IRAS (HiRes)images have been produced for these 58 objects and some of thosespatially resolved are presented in this study. The images were used todistinguish between multiple confused IR sources, possible artifacts andunambiguous bow shocks, as the sources of the extended 60 \mum emission.Six new bow shocks have been identified using this method, and threehave been rejected. Twenty two of the targets, however, remain spatiallyunresolved even at the nominal HiRes resolution of ~ 1arcmin . For thelarger and better defined bow shocks some internal substructure isdiscernible. The length of these features suggest that they arise as theresult of a subtle dynamical instability. It can not be ruled out,however, that some of the bow shock morphology could be imprinted by thesurrounding medium.
| A Spectral Atlas of Hot, Luminous Stars at 2 Microns
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996ApJS..107..281H&db_key=AST
| A Search for Pulsar Companions to OB Runaway Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996ApJ...461..357S&db_key=AST
| 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
| DO OB Runaway Stars Have Pulsar Companions?
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996AJ....111.1220P&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.
| OB-runaways as a result of massive star evolution.
We investigated four OB-associations and tried to model six runawayswhich were possibly ejected from these associations. From the positionand space velocity of each runaway we tried to trace back its birthplaceand birthdate in the subgroup of the parent association where therunaway started its space travel. We used massive star evolutionaryresults to check if all known parameters of the runaway star can beexplained: its atmospheric hydrogen abundance and the fact that itsposition in the HRD, i.e. spectral type and luminosity is hit by theevolutionary track at the correct time. It is found that the runawayζ Oph can be modeled only by the binary scenario, where thesecondary was ejected after the SN event of its primary out of Upp CenLup. ζ Pup can be explained by single star evolution only when itwas ejected from Vela R2, implying a luminosity that is significantlyhigher than commonly used. A binary scenario for ζ Pup can be foundprovided that the binary was a field star. The three runaways of Orioncan be modeled by binary evolution with ejection from the subgroup OriOB1a. For two of them, single star evolution with ejection from Ori OB1cworks equally well. Finally, the OB-runaway optical component of VelaX-1 is still bound to its SN remnant and thus certainly a result ofbinary evolution. The system originated presumably in Vela OB1.
| 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 Orion OB1 association. II. The Orion-Eridanus Bubble.
Observations of the interstellar medium in the vicinity of the Orion OB1association show a cavity filled with hot ionized gas, surrounded by anexpanding shell of neutral hydrogen (the Orion-Eridanus Bubble). In thispaper we examine this cavity and the surrounding bubble with the aid ofdata from the Leiden/Dwingeloo HI survey. We present neutral-hydrogenmaps for the Orion-Eridanus region which allow identification of the HIfilaments and arcs delineating the Bubble and derivation of itsexpansion velocity. The X-ray emission from the Orion-Eridanus region isenhanced with respect to the Galactic background emission. Comparisonwith the HI data shows a detailed anti-correlation of the X-rayenhancement with kinematically-narrow features. This confirms theassociation of the X-ray enhancement with the cavity in HI. Comparisonof the derived column densities in HI with the IRAS 100μm intensitiesshows that the HI shell emission is optically thin. This justifies aderivation of the mass of the HI shell by direct conversion of theobserved HI emission to column densities. Models of wind-blown bubblesare considered, to investigate if the cavity was formed by the stellarwinds and supernovae from Orion OB1. Using a model that takes thedensity stratification of the Galactic HI layer into account, we showthat the stellar winds and supernovae from stars in Orion OB1 canaccount for the size as well as for the expansion velocity of the HIshell. However, density inhomogeneities in the ambient interstellarmedium cause significant discrepancies between our model and theobserved shell.
| Photometric variability in early B stars I. 53 ARIETIS
Not Available
| An IUE survey of interstellar H I LY alpha absorption. 1: Column densities
We measure Galactic interstellar neutral hydrogen column densities byanalyzing archival interstellar Ly alpha absorption line data toward 554B2 and hotter stars observed at high resolution with the IUE satellite.This study more than doubles the number of lines of sight with measuresof N(H I) based on Ly alpha. We have included the scattered lightbackground correction algorithm of Bianchi and Bohlin in our datareduction. We use the correlation between the Balmer discontinuity(c1) index and the stellar Ly alpha absorption in order toassess the effects of stellar Ly alpha contamination. Approximately 40%of the B stars with measured (c1) index, exhibit seriousstellar Ly alpha contamination. One table contains the derived values ofthe interstellar N(H I) for 393 stars with at most small amounts ofstellar contamination. Another lists the observed values of total N(H I)for 161 stars with suspected stellar Ly alpha contamination and/oruncertain stellar parameters.
| The Orion OB1 association. 1: Stellar content
Walfraven photometry of established and probable members of the OrionOB1 association is presented. Effective temperature, surface gravity,luminosity and mass are derived for all stars, using atmosphere model byKurucz (1979). Absolute magnitudes are calculated using the Straizys andKuriliene (1981) tables. Distance moduli and visual extinctions aredetermined. A comparison of the visual extinctions to IRAS 100micrometers data shows that the near edge of the Orion A and B cloudslies at a distance of approximately 320 pc, while the far edge is atapproximately 500 pc. A method for deriving the ages of the subgroups bycomparing theoretical isochrones to the observations in the log g, logTeff plane is presented. The derived ages suggest, contraryto earlier studies, that subgroup 1b is younger than 1c, which canpossibly be explained by past geometries of the system of stars and gas.The initial mass function for Orion OB1 is derived with the aid of theKolmogorov-Smirnoff test. Through extensive simulations, we show that itis very difficult to derive accurately the Initial Mass Function (IMF)from the available data. To within somewhat weak limits the IMF is foundto be of the form xi(log M) = AM-1.7 +/- 0.2 for allsubgroups. The energy output of the subgroups in the form of stellarwinds and supernovae is calculated and compared to the observed size andexpansion velocity of the Orion-Eridanus bubble. It is shown that theenergy output of the association can account for the morphology andkinematics of the interstellar medium (ISM).
| Is Geminga a runaway member of the Orion association?
Using the age and distance estimates for the neutron star Geminga, aswell as its measured proper motion, we examine the possible spacemotions of Geminga in an attempt to determine the origin of itsprogenitor star. As argued by Frisch (1993), we also find that Geminga'sprogenitor was quite likely a member of the Orion association. Inaddition, we suggest that the progenitor star may have been ejected fromthe Orion association before its supernova explosion, as an OB runawaystar in which case the supernova could have occurred some distance awayfrom the association. We also point out that if the supernova occurredin the association itself, the most likely region might be within thelambda Ori association.
| Massive close binaries, observational characteristics
Not Available
| The distribution of interstellar dust in the solar neighborhood
We surveyed the IRAS data base at the positions of the 1808 O6-B9.5stars in The Bright Star Catalog for extended objects with excessemission at 60 microns, indicating the presence of interstellar dust atthe location of the star. Within 400 pc the filling factor of theinterstellar medium, for dust clouds with a density greater than 0.5/cucm is 14.6 + or - 2.4%. Above a density of 1.0/cu cm, the densitydistribution function appears to follow a power law index - 1.25. Whenthe dust clouds are mapped onto the galactic plane, the sun appears tobe located in a low-density region of the interstellar medium of widthabout 60 pc extending at least 500 pc in the direction of longitudes 80deg - 260 deg, a feature we call the 'local trough'.
| A high-resolution optical and radio study of Milky Way halo gas
Optical interstellar absorption lines of Ti II and Ca II and the 21 cmemission line of H I were observed at high-resolution (6 and 1 km/s,respectively) and high detection sensitivity along 25 lines of sight inthe Galactic halo. The sample includes 16 distant halo stars matchedwith one or more nearly aligned foreground stars as well as local starsalong five extragalactic sight lines. The data show substantialinterstellar material, at both low and intermediate velocities, between250 and 1000 pc beyond the Galactic plane. As much as one-third of thetotal gas observed in Ca II absorption may be beyond 1 kpc, and thegaseous Ti II may lie in an even thicker layer. The directly determinedgaseous Ti abundance above the Galactic plane exceeds that in the disk,on the average, by a factor of 4 to 6 and, for individual cloudcomponents, is further enhanced at higher LSR velocity. Thirty threediscrete high-latitude clouds are detected in Ca II absorption, and 17discrete clouds, including three high-velocity clouds, are identified inH I emission. The kinematics of the high-latitude gas observed in Ti IIand Ca II absorption is characterized by significant peculiar velocitieswith respect to a model corotating halo.
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| Csillagkép: | Kos |
| Rektaszcenzió: | 03h07m25.70s |
| Deklináció: | +17°52'48.0" |
| Vizuális fényesség: | 6.11 |
| Távolság: | 231.481 parszek |
| RA sajátmozgás: | -22.7 |
| Dec sajátmozgás: | 7.3 |
| B-T magnitude: | 5.969 |
| V-T magnitude: | 6.098 |
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