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Runaway Massive Binaries and Cluster Ejection Scenarios
The production of runaway massive binaries offers key insights into theevolution of close binary stars and open clusters. The stars HD 14633and HD 15137 are rare examples of such runaway systems, and in this workwe investigate the mechanism by which they were ejected from theirparent open cluster, NGC 654. We discuss observational characteristicsthat can be used to distinguish supernova ejected systems from thoseejected by dynamical interactions, and we present the results of a newradio pulsar search of these systems, as well as estimates of theirpredicted X-ray flux assuming that each binary contains a compactobject. Since neither pulsars nor X-ray emission are observed in thesesystems, we cannot conclude that these binaries contain compactcompanions. We also consider whether they may have been ejected bydynamical interactions in the dense environment where they formed, andour simulations of four-body interactions suggest that a dynamicalorigin is possible but unlikely. We recommend further X-ray observationsthat will conclusively identify whether HD 14633 or HD 15137 containneutron stars.
| A Spectroscopic Study of Field and Runaway OB Stars
Identifying binaries among runaway O- and B-type stars offers valuableinsight into the evolution of open clusters and close binary stars. Herewe present a spectroscopic investigation of 12 known or suspectedbinaries among field and runaway OB stars. We find new orbital solutionsfor five single-lined spectroscopic binaries (HD 1976, HD 14633, HD15137, HD 37737, and HD 52533), and we classify two stars thought to bebinaries (HD 30614 and HD 188001) as single stars. In addition, wereinvestigate their runaway status using our new radial velocity datawith the UCAC2 proper-motion catalogs. Seven stars in our study appearto have been ejected from their birthplaces, and at least three of theserunaways are spectroscopic binaries and are of great interest for futurestudy.
| X-Ray Counterparts of Runaway Stars
An X-ray search for possible compact companions of runaway OB stars hasbeen conducted using pointed ROSAT observations. Of a list of 71 runawaystars, ROSAT exposures were available for 24, of which 13 are detected.These numbers are nearly 3 times larger than for a previously studiedEinstein sample, and spectral information is exploited as well.Luminosities, hardness ratios, and long-term variability are as fornormal OB stars and do not suggest the presence of collapsed companions.A result like this is often interpreted as support for dynamicalejection from a dense group rather than a supernova event in a binary asa production process for runaway stars. There are, however, severalcircumstances that may adversely affect the observability of a compactcompanion, or after a supernova explosion systems may be disruptedbecause of the large natal kick velocity imparted to the neutron star asa result of asymmetries in the explosions. It is noted that there isactually evidence for both of these production routes and that they maybe expected to occur sequentially in the evolution of OB associations.
| The Massive Runaway Stars HD 14633 and HD 15137
We present results from a radial velocity study of two runaway O-typestars, HD 14633 (ON8.5 V) and HD 15137 [O9.5 III(n)]. We find that HD14633 is a single-lined spectroscopic binary with an orbital period of15.4083 days. The second target, HD 15137, is a radial velocity variableand a possible single-lined spectroscopic binary with a period close to1 month. Both binaries have large eccentricity, small semiamplitude, anda small mass function. We show the trajectories of the stars in the skybased on an integration of motion in the Galactic potential, and wesuggest that both stars were ejected from the vicinity of the opencluster NGC 654 in the Perseus spiral arm. The binary orbital parametersand runaway velocities are consistent with the idea that both thesestars were ejected by supernova explosions in binaries and that theyhost neutron star companions. We find that the time of flight sinceejection is longer than the predicted evolutionary timescales for thestars. This discrepancy may indicate that the stars have a lower massthan normally associated with their spectral classifications, that theywere rejuvenated by mass transfer prior to the supernova, or that theirlives have been extended through rapid rotation.Based in part on observations made at the Observatoire de Haute Provence(CNRS), France.
| On the Hipparcos parallaxes of O stars
We compare the absolute visual magnitude of the majority of bright Ostars in the sky as predicted from their spectral type with the absolutemagnitude calculated from their apparent magnitude and the Hipparcosparallax. We find that many stars appear to be much fainter thanexpected, up to five magnitudes. We find no evidence for a correlationbetween magnitude differences and the stellar rotational velocity assuggested for OB stars by Lamers et al. (1997, A&A, 325, L25), whosesmall sample of stars is partly included in ours. Instead, by means of asimulation we show how these differences arise naturally from the largedistances at which O stars are located, and the level of precision ofthe parallax measurements achieved by Hipparcos. Straightforwardlyderiving a distance from the Hipparcos parallax yields reliable resultsfor one or two O stars only. We discuss several types of bias reportedin the literature in connection with parallax samples (Lutz-Kelker,Malmquist) and investigate how they affect the O star sample. Inaddition, we test three absolute magnitude calibrations from theliterature (Schmidt-Kaler et al. 1982, Landolt-Börnstein; Howarth& Prinja 1989, ApJS, 69, 527; Vacca et al. 1996, ApJ, 460, 914) andfind that they are consistent with the Hipparcos measurements. AlthoughO stars conform nicely to the simulation, we notice that some B stars inthe sample of \citeauthor{La97} have a magnitude difference larger thanexpected.
| A Galactic O Star Catalog
We have produced a catalog of 378 Galactic O stars with accuratespectral classifications that is complete for V<8 but includes manyfainter stars. The catalog provides cross-identifications with othersources; coordinates (obtained in most cases from Tycho-2 data);astrometric distances for 24 of the nearest stars; optical (Tycho-2,Johnson, and Strömgren) and NIR photometry; group membership,runaway character, and multiplicity information; and a Web-based versionwith links to on-line services.
| The N Enrichment and Supernova Ejection of the Runaway Microquasar LS 5039
We present an investigation of new optical and ultraviolet spectra ofthe mass donor star in the massive X-ray binary LS 5039. The opticalband spectral line strengths indicate that the atmosphere is N-rich andC-poor, and we classify the stellar spectrum as type ON6.5 V((f)). TheN-strong and C-weak pattern is also found in the stellar wind P Cygnilines of N V λ1240 and C IV λ1550 (narrow absorptioncomponents in the former indicate that the wind terminal velocity isV&infy;=2440+/-190 km s-1). We suggest that the Nenrichment may result from internal mixing if the O star was born as arapid rotator or the O star may have accreted N-rich gas prior to acommon envelope interaction with the progenitor of the supernova. Wereevaluated the orbital elements to find an orbital period ofP=4.4267+/-0.0005 days. We compared the spectral line profiles with newnon-LTE line-blanketed model spectra from Lanz and Hubeny, from which wederive an effective temperature Teff=37.5+/-1.7 kK, gravitylogg=4.0+/-0.1, and projected rotational velocity Vsini=140+/-8 kms-1. We fitted the UV, optical, and IR flux distribution byusing a model spectrum and extinction law with parametersE(B-V)=1.28+/-0.02 and R=3.18+/-0.07. We confirm the covariability ofthe observed X-ray flux and stellar wind mass-loss rate derived from theHα profile, which supports the wind accretion scenario for theX-ray production in LS 5039. Wind accretion models indicate that thecompact companion has mass MX/Msolar=1.4+/-0.4,consistent with its identification as a neutron star. We argue that theO star has mass in the range 20-35 Msolar (based on a lowerlimit for the distance and the lack of eclipses). The observedeccentricity and runaway velocity of the binary can be reconciled onlyif the neutron star received a modest kick velocity due to a slightasymmetry in the supernova explosion (during which more than 5Msolar was ejected).Based on observations with the NASA/ESA Hubble Space Telescope obtainedat the Space Telescope Science Institute, which is operated by theAssociation of Universities for Research in Astronomy, Inc., under NASAcontract NAS5-26555.
| Rotational mixing in early-type main-sequence stars
We present quantitative observational investigations into the importanceof rotationally induced mixing in late-O stars. First, we conductnon-LTE, hydrostatic, plane-parallel H/He model-atmosphere analyses ofthe optical spectra of three of the most rapidly rotating late-Onear-main-sequence stars known: HD 93521 (O9.5 V), HD 149757 (ζOphiuchi; O9.5 V), and HD 191423 (ON9 III: n), all of which haveequatorial rotation velocities of ~430kms-1 and[formmu8]ωe/ωe(crit)~=0.9. Theanalysis allows for the expected (von Zeipel) variation ofTeff and logg with latitude. These three stars are found toshare very similar characteristics, including substantially enhancedsurface-helium abundances [formmu9](y~=0.2). Secondly, we compare thedistribution of projected rotational velocities for ON andmorphologically normal dwarf O stars, and demonstrate that the ON starsare drawn from a population with more rapid rotation. The resultsprovide qualitative support for rotationally induced mixing, althoughthere remain discrepancies between atmospheric and evolutionary models(which we show employ inappropriate mass-loss rates for late-Omain-sequence stars). We show that the most rapid rotator known, HD191423, is an ON star, and note the implied disparity between O/ONmorphology and surface helium abundance; we discuss consequences for theinterpretation of spectral morphology in O-type main-sequence stars. Wedemonstrate a new, purely spectroscopic, method of distancedetermination for rapid rotators, and thereby confirm that HD 93521 liesat ~2kpc, and is not, as previously suggested, a low-mass Population IIstar. Finally, our models contradict earlier claims of stronglydifferential surface rotation, and are consistent with uniform angularvelocity at the surface.
| Distances and Metallicities of High- and Intermediate-Velocity Clouds
A table is presented that summarizes published absorption linemeasurements for the high- and intermediate-velocity clouds (HVCs andIVCs). New values are derived for N(H I) in the direction of observedprobes, in order to arrive at reliable abundances and abundance limits(the H I data are described in Paper II). Distances to stellar probesare revisited and calculated consistently, in order to derive distancebrackets or limits for many of the clouds, taking care to properlyinterpret nondetections. The main conclusions are the following. (1)Absolute abundances have been measured using lines of S II, N I, and OI, with the following resulting values: ~0.1 solar for one HVC (complexC), ~0.3 solar for the Magellanic Stream, ~0.5 solar for a southern IVC,and ~solar for two northern IVCs (the IV Arch and LLIV Arch). Finally,approximate values in the range 0.5-2 solar are found for three moreIVCs. (2) Depletion patterns in IVCs are like those in warm disk or halogas. (3) Most distance limits are based on strong UV lines of C II, SiII, and Mg II, a few on Ca II. Distance limits for major HVCs aregreater than 5 kpc, while distance brackets for several IVCs are in therange 0.5-2 kpc. (4) Mass limits for major IVCs are0.5-8×105 Msolar, but for major HVCs theyare more than 106 Msolar. (5) The Ca II/H I ratiovaries by up to a factor 2-5 within a single cloud, somewhat morebetween clouds. (6) The Na I/H I ratio varies by a factor of more than10 within a cloud, and even more between clouds. Thus, Ca II can beuseful for determining both lower and upper distance limits, but Na Ionly yields upper limits.
| Optical observations of three Galactic halo stars: evidence for cloudlets in intermediate- and high-velocity interstellar clouds
Very high resolution (R ~ 160000) absorption line measurements of theinterstellar Ca Ii K and Na I D lines and medium resolution (R ~ 50000)measurements of the interstellar Ti Ii (3384 Ä) line towards threeGalactic halo stars are presented. The data have signal-to-noise ratiosof ~ 90-240. The sightlines studied clearly show severalintermediate-high velocity interstellar clouds with local standard ofrest velocities in the range ~ - 40 to -110 \km. Two different methodshave been used to analyze these data. Line profile fitting allows us tomodel multiple components for the different high-velocity cloudsseparated by only a few km. The close proximity of the lines in velocityspace indicates that the cloudlets are related. Conversion of theabsorption profiles to apparent optical depth profiles also allows us toexamine the column densities and their ratios as a function of velocity.Variations in N(ion {Ca}{ii})/N(ion {Na}i), N(ion {Ca}{ii})/N(ion{Ti}{ii}) and N(ion {Ti}{ii})/N(ion {Na}i) with cloud velocity arediscussed.
| Diffuse interstellar bands in low E(B-V) objects
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1998MNRAS.295..437G&db_key=AST
| On the normal energy distribution in stellar spectra: O5-O8 stars
The spectral energy curves for a number of O4-O8 stars are analyzedusing measurements taken from six sources of spectrophotometric data.Based on the normal UBV color indices for O stars, these stars aredivided into three groups (O5, O6-O7, and O8), for each of which thenormal energy distribution is derived and presented. Comparison of thesedistributions indicates clear differences between the O5 and O8subclasses at UV wavelengths. A single normal distribution curve is,therefore, insufficient to characterize the O spectral class as a whole.
| ICCD speckle observations of binary stars. XIX - an astrometric/spectroscopic survey of O stars
We present the results of a speckle interferometric survey made with theCHARA speckle camera and 4 m class telescopes of Galactic O-type starswith V less than 8. We can detect with the speckle camera binaries inthe angular separation range 0.035-1.5 arcsec with delta M less than 3,and we have discovered 15 binaries among 227 O-type systems. We combinedour results on visual binaries with measurements of wider pairs from theWashington Double Star Catalog and fainter pairs from the HipparcosCatalog, and we made a literature survey of the spectroscopic binariesamong the sample. We then investigated the overall binary frequency ofthe sample and the orbital characteristics of the known binaries.Binaries are common among O stars in clusters and associations but lessso among field and especially runaway stars. There are many triplesystems among the speckle binaries, and we discuss their possible rolein the ejection of stars from clusters. The period distribution of thebinaries is bimodal in log P, but we suggest that binaries with periodsof years and decades may eventually be found to fill the gap. The massratio distribution of the visual binaries increases toward lower massratios, but low mass ratio companions are rare among close,spectroscopic binaries. We present distributions of the eccentricity andlongitude of periastron for spectroscopic binaries with ellipticalorbits, and we find strong evidence of a bias in the longitude ofperiastron distribution.
| Massive stars
We describe the present state of massive star research seen from theviewpoint of stellar evolution, with special emphasis on close binaries.Statistics of massive close binaries are reasonably complete for theSolar neighbourhood. We defend the thesis that within our knowledge,many scientific results where the effects of binaries are not included,have an academic value, but may be far from reality. In chapter I, wesummarize general observations of massive stars where we focus on the HRdiagram, stellar wind mass loss rates, the stellar surface chemistry,rotation, circumstellar environments, supernovae. Close binaries can notbe studied separately from single stars and vice versa. First, theevolution of single stars is discussed (chapter I). We refer to newcalculations with updated stellar wind mass loss rate formalisms andconclusions are proposed resulting from a comparison with representativeobservations. Massive binaries are considered in chapter II. Basicprocesses are briefly described, i.e. the Roche lobe overflow and masstransfer, the common envelope process, the spiral-in process in binarieswith extreme mass ratio, the effects of mass accretion and the mergingprocess, the implications of the (asymmetric) supernova explosion of oneof the components on the orbital parameters of the binary. Evolutionarycomputations of interacting close binaries are discussed and generalconclusions are drawn. The enormous amount of observational data ofmassive binaries is summarized. We separately consider the non-evolvedand evolved systems. The latter class includes the semi-detached andcontact binaries, the WR binaries, the X-ray binaries, the runaways, thesingle and binary pulsars. A general comparison between theoreticalevolution and observations is combined with a discussion of speciallyinteresting binaries: the evolved binaries HD 163181, HD 12323, HD14633, HD 193516, HD 25638, HD 209481, Φ Per and silon Sgr; theWR+OB binary V444 Cyg; the high mass X-ray binaries Vela X-1, Wray 977,Cyg X-1; the low mass X-ray binaries Her X-1 and those with a black holecandidate; the runaway ζ Pup, the WR+compact companion candidatesCyg X-3, HD 50896 and HD 197406. We finally propose an overallevolutionary model of massive close binaries as a function of primarymass, mass ratio and orbital period. Chapter III deals with massive starpopulation synthesis with a realistic population of binaries. We discussthe massive close binary frequency, mass ratio and period distribution,the observations that allow to constrain possible asymmetries during thesupernova explosion of a massive star. We focuss on the comparisonbetween observed star numbers (as a function of metallicity) andtheoretically predicted numbers of stellar populations in regions ofcontinuous star formation and in starburst regions. Special attention isgiven to the O-type star/WR star/red supergiant star population, thepulsar and binary pulsar population, the supernova rates.
| Cross-correlation characteristics of OB stars from IUE spectroscopy
We present a catalogue of homogeneous measures of the linewidthparameter, v_esin i, for 373 O-type stars and early B supergiants(including the separate components of 25 binary and three triplesystems), produced by cross-correlating high-resolution,short-wavelength IUE spectra against a `template' spectrum of tauSco. Wealso tabulate terminal velocities. There are no O supergiants in oursample with v_esin i<65 km s^-1, and only one supergiant earlier thanB5 has v_esin i<50 km s^-1, confirming that an important linebroadening mechanism in addition to rotation must be present in theseobjects. A calibration of the area under the cross-correlation peakagainst spectral type is used to obtain estimates of continuum intensityratios of the components in 28 spectroscopically binary or multiplesystems. At least seven SB2 systems show evidence for the `Struve-Sahadeeffect', a systematic variation in relative line strength as a functionof orbital phase. The stellar wind profiles of the most rapid rotator inour sample, the O9III:n* star HD 191423 (v_esin i=436km s^-1), show itto have a `wind-compressed disc' similar to that of HD 93521; this starand other rapid rotators are good candidates for studies of non-radialpulsation.
| Observational manifestations of early mixing in B and O type stars.
Not Available
| Coronal Gas in the Halo. II. ORFEUS Observations of Galactic Halo Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996ApJ...465..296H&db_key=AST
| Projected Rotational Velocities of O-Type Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996ApJ...463..737P&db_key=AST
| Metal line strengths of blue stragglers towards the young galactic association Perseus OB1.
We present equivalent width measurements of lines of HeI, CIII, NIII,OII, MgII and SiIV from high resolution optical spectra of eight bluestragglers towards the young galactic association Perseus OB1, togetherwith similar data from ultraviolet spectra. We have carried outintercomparisons of the observed line strengths between target stars ofsimilar effective temperatures, and comparisons between the target starsand data for other O-type stars, in order to search for possibleabundance anomalies in our target stars. We find firm evidence that twostars, HD 12323 and HD 13268, exhibit CNO bicycle processed material attheir surfaces, and we outline evolutionary scenarios to explain thisphenomenon. One further star, HD 12993, also shows marginal evidence forprocessed material at its surface. There is no evidence for abundanceanomalies in the five remaining stars, and we consider that they may notbe association members. Hence their identification as blue stragglers isin doubt.
| 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 Lyman-Continuum Fluxes and Stellar Parameters of O and Early B-Type Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996ApJ...460..914V&db_key=AST
| Observation of Turbulent Fluctuations in the Interstellar Plasma Density and Magnetic Field on Spatial Scales of 0.01 to 100 Parsecs
Abstract image available at:http://adsabs.harvard.edu/abs/1996ApJ...458..194M
| Terminal Velocities and the Bistability of Stellar Winds
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJ...455..269L&db_key=AST
| 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.
| Far-Ultraviolet (912--1900 Angstrom ) Energy Distribution in Early-Type Main-Sequence Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJ...449..280C&db_key=AST
| Radio continuum emission from stars: a catalogue update.
An updated version of my catalogue of radio stars is presented. Somestatistics and availability are discussed.
| An atlas of ultraviolet P Cygni profiles
We have selected spectra of 232 stars from the International UltravioletExplorer (IUE) archives for inclusion in an atlas intended for varioususes but tailored especially for the study of stellar winds. The atlascovers the range in spectral types from O3 to F8. The full atlas coversthe reduced and normalized high resolution spectra from the IUE long-and short-wavelength spectrographs. Here we discuss the selection of thestars and the data reduction, and we present in velocity units theprofiles of lines formed in the stellar winds. The selected lines covera wide range of ionizations, allowing a comparison of the profiles fromdifferent ions in the wind of each star and a comparison of thedifferent wind lines as a function spectral type and luminosity. We alsopresent the basic data on the program stars to facilitate study of thedependence of wind features on stellar parameters such as luminosity,temperature, escape velocity, and v sin i. We provide an overview of thecharacteristic behavior of the wind lines in the H-R diagram. Thecomplete spectra are available in digital form through the NASAAstrophysics Data System (ADS). We offer a description of the electronicdatabase that is available through the ADS and guidelines for obtainingaccess to that database.
| 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 Zn^+^/Na^0^ interstellar ratio
We study the behaviour of the interstellar R_n_=n(Zn^+^)/n(Na^0^) ratioin ionization equilibrium conditions. The ratio is very sensitive tovariations of the physical state of the gas and is only marginallyaffected by variations of interstellar depletion. We find logR_n_ {in}[=~-2,=~0] dex in cold molecular clouds, logR_n_ {in} about [0,+1] dexin cold atomic gas, and logR_n_ {in} about [+1,+3] dex in warm gas. Wecompare the theoretical R_n_ ratio with the column-density ratioR_N_=N(ZnII)/N(NaI) measured in a sample of 48 interstellar lines ofsight. The comparison supports the validity of the assumption ofionization equilibrium and indicates that R_N_ is a good indicator ofthe physical state of the gas. The few deviations from ionizationequilibrium that we find are all located in the general direction ofβ CMa, where studies of the local ISM revealed the presence of anextended (=~ 2x10^2^ pc) tunnel of hot gas. Finally, we report theresults of a correlation analysis logR_N_-logN(NaI) and logR_N_-logN(H).The correlations that we derive imply the presence of a mechanismlinking the physical state of interstellar clouds to their columndensity. A practical consequence of the correlation with N(NaI) is thata NaI measurement alone is sufficient to estimate the physical state ofthe gas in many situations of interest.
| Physical characteristics of close binary system components
An approximate approach for evaluating the mass of invisible satellitesof close binary systems with the mass-function f(M) much less than 1 issuggested. A possibility of using it is shown for 62 close binarysystems.
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| קבוצת-כוכבים: | אנדרומדה |
| התרוממות ימנית: | 02h22m54.29s |
| סירוב: | +41°28'47.7" |
| גודל גלוי: | 7.442 |
| מרחק: | 909.091 פארסק |
| תנועה נכונה: | -0.4 |
| תנועה נכונה: | -7.7 |
| B-T magnitude: | 7.171 |
| V-T magnitude: | 7.42 |
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