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Spectropolarimetry and Radiative Transfer Modeling of Three Proto-Planetary Nebulae
We measured the spectrum of polarization for three proto-planetarynebulae (PPNs), IRAS 17411-2411, IRAS 08005-2356, and IRAS 04296+3429,and made model calculations with the dust-scattering Monte Carlo codeDIRTY and the dust emission code 2Dust. We show that high levels ofpolarization in these PPNs correlate with extreme asymptotic giantbranch (AGB) superwind mass-loss rates in excess of 10-4Msolar yr-1. All three objects show evidence forevacuated lobes cleared by collimated fast winds, and two indicate asignificant equatorial mass enhancement. Our best-fit models requiresharply peaked grain size distributions, suggesting that most of thelight is being scattered by grains of a characteristic size in IRAS17441-2411 and IRAS 08005-2356. IRAS 17441-2411 and IRAS 08005-2356 havelobes with wide opening angles, perhaps produced by deflection of apolar jet from an accreting companion by the AGB superwind. Modeling thespectropolarimetry of IRAS 04296+3429 indicates a point-symmetric,multipolar morphology in the PPN phase. The modeling ofspectropolarimetry and other observations of PPNs provides a powerfulway to constrain circumstellar morphology and dust parameters.
| Large-scale wind structures in OB supergiants: a search for rotationally modulated Hα variability
We present the results of a long-term monitoring campaign of theHα line in a sample of bright OB supergiants (O7.5-B9) which aimsat detecting rotationally modulated changes potentially related to theexistence of large-scale wind structures. A total of 22 objects weremonitored during 36 nights spread over six months in 2001-2002.Coordinated broad-band photometric observations were also obtained forsome targets. Conspicuous evidence for variability in Hα is foundfor the stars displaying a feature contaminated by wind emission. Mostchanges take place on a daily time-scale, although hourly variations arealso occasionally detected. Convincing evidence for a cyclical patternof variability in Hα has been found in two stars: HD 14134 and HD42087. Periodic signals are also detected in other stars, butindependent confirmation is required. Rotational modulation is suggestedfrom the similarity between the observed recurrence time-scales (in therange 13-25 d) and estimated periods of stellar rotation. We callattention to the atypical case of HD 14134, which exhibits a clear12.8-d periodicity, both in the photometric and in the spectroscopicdata sets. This places this object among a handful of early-type starswhere one may observe a clear link between extended wind structures andphotospheric disturbances. Further modelling may test the hypothesisthat azimuthally-extended wind streams are responsible for the patternsof spectral variability in our target stars.
| Catalogue of averaged stellar effective magnetic fields. I. Chemically peculiar A and B type stars
This paper presents the catalogue and the method of determination ofaveraged quadratic effective magnetic fields < B_e > for 596 mainsequence and giant stars. The catalogue is based on measurements of thestellar effective (or mean longitudinal) magnetic field strengths B_e,which were compiled from the existing literature.We analysed the properties of 352 chemically peculiar A and B stars inthe catalogue, including Am, ApSi, He-weak, He-rich, HgMn, ApSrCrEu, andall ApSr type stars. We have found that the number distribution of allchemically peculiar (CP) stars vs. averaged magnetic field strength isdescribed by a decreasing exponential function. Relations of this typehold also for stars of all the analysed subclasses of chemicalpeculiarity. The exponential form of the above distribution function canbreak down below about 100 G, the latter value representingapproximately the resolution of our analysis for A type stars.Table A.1 and its references are only 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/407/631 and Tables 3 to 9are only available in electronic form at http://www.edpsciences.org
| High-resolution Keck I spectroscopy of Galactic halo post-asymptotic giant branch stars
Absolute and differential abundance analyses have been performed fromhigh-resolution, high signal-to-noise ratio optical (Keck I) spectra forthree evolved Galactic halo stars, namely PG 1704 + 222, HD 341617 andLS IV -04 01. Their derived atmospheric parameters indicate that allthree objects are undergoing a post-asymptotic giant branch (post-AGB)phase of evolution. A differential abundance analysis reveals HD 341617as having a mild carbon deficiency of 0.74 dex, possibly due to the starhaving evolved off the AGB before the onset of the third dredge-up.Although such carbon underabundances are typical of hot post-AGBobjects, the same trend is not observed in PG 1704 + 222, where thecarbon abundance is found to be consistent with those derived fornitrogen and oxygen. Hence, a dredge-up scenario need not be invoked toexplain the chemical composition of PG 1704 + 222. For LS IV -04 01 noiron deficiency is apparent relative to magnesium and silicon, and hencea gas-dust separation event in the AGB progenitor need not be invokedfor this star.
| 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.
| Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics
The Catalogue, available at the Centre de Données Stellaires deStrasbourg, consists of 13 573 records concerning the results obtainedfrom different methods for 7778 stars, reported in the literature. Thefollowing data are listed for each star: identifications, apparentmagnitude, spectral type, apparent diameter in arcsec, absolute radiusin solar units, method of determination, reference, remarks. Commentsand statistics obtained from CADARS are given. The Catalogue isavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcar?J/A+A/367/521
| Galactic B-supergiants: A non-LTE model atmosphere analysis to estimate atmospheric parameters and chemical compositions
A non-LTE model atmosphere analysis of moderate resolution (R ~ 5 000)spectra of 46 Galactic B-type supergiants is presented. Standardtechniques are adopted, viz. plane-parallel geometry and radiative andhydrostatic equilibrium. Spectroscopic atmospheric parameters (T_eff,log g & v_turb) and chemical abundances (He, C, N, O, Mg & Si)are estimated, both as a test of the validity of such an approach and inan attempt to provide consistent results for supergiants covering asignificant range of spectral types. The values of the estimatedatmospheric parameters and their dependence on the physics adopted inthe model atmospheres calculations are discussed. The absolute metalabundances are compared to those of main sequence B-type stars and, ingeneral, their chemical compositions appear to be similar. Theabundances for He, C, N & O are considered in some detail and arediscussed in the context of possible evolutionary histories for thisstellar sample. Specifically, it is found that the supergiant sample canbe subdivided into a number of evolutionarily distinct groups. The lowermass objects are predominantly chemically near-normal i.e. theirphotospheres show little or no evidence for chemical processing, whereasthe higher mass supergiants have CNO ratios which are indicative of CNand possibly NO-cycle burning. An attempt is made to quantify thedifference in nitrogen and carbon abundances between the high and lowmass targets but this is hampered by theoretical uncertainties. Thepossibilities that the most highly processed supergiants may have eitherlarger rotational velocities or have undergone mass transfer within abinary system are discussed.
| 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.
| 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.
| 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
| 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.
| The abundance of boron in evolved A- and B-type stars.
Boron abundances in A- and B-type stars may be a successful way to trackevolutionary effects in these hot stars. The light elements - Li, Be,and B - are tracers of exposure to temperatures more moderate than thosein which the H-burning CN-cycle operates. Thus, any exposure of surfacestellar layers to deeper layers will affect these light elementabundances. Li and Be are used in this role in investigations ofevolutionary processes in cool stars, but are not observable in hotterstars. An investigation of boron, however, is possible through the BII1362A resonance line. We have gathered high resolution spectra from theIUE database of A- and B-type stars near 10Msun_ for whichnitrogen abundances have been determined (by Gies & Lambert andVenn). The BII 1362A line is blended throughout the temperature range ofthis program, requiring spectrum syntheses to recover the boronabundances. For no star could we synthesize the 1362A region using themeteoritic/solar boron abundance of logɛ(B)=2.88 (Anders &Grevesse); a lower boron abundance was necessary which may reflectevolutionary effects (e.g., mass loss or mixing near the main-sequence),the natal composition of the star forming regions, or a systematic errorin the analyses (e.g., non-LTE effects). Regardless of the initial boronabundance, and despite the possibility of non-LTE effects, it seemsclear that boron is severely depleted in some stars. It may be that thenitrogen and boron abundances are anticorrelated, as would be expectedfrom mixing between the H-burning and outer stellar layers. If, as wesuspect, a residue of boron is present in the A-type supergiants, we mayexclude a scenario in which mixing occurs continuously between thesurface and the deep layers operating the CN-cycle. Further exploitationof the BII 1362A line as an indicator of the evolutionary status of A-and B-type stars will require a larger stellar sample to be observedwith higher signal-to-noise as attainable with the Hubble SpaceTelescope.
| CNO Abundances and the Evolutionary Status of Galactic, A-Type Supergiants
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJ...449..839V&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.
| Abundance analysis of the hot post-AGB star Barnard 29.
We present a model atmosphere analysis for the relatively bright (V~13)globular cluster post-AGB star, Barnard 29, using IUE and highresolution (0.06A FWHM) optical spectra. The derived atmosphericparameters are T_eff_=20000+/-1000K and logg=3.0+/-0.1dex, which imply acurrent mass of ~0.55Msun_. The chemical composition providesimportant constraints on the post-AGB evolutionary stage. We find anoverall metal deficiency of 1.46+/-0.11dex, which is compatible with themean [Fe/H] obtained from previous M13 studies. The most interestingfeature is the severe carbon deficiency of more than 2.0dex which hasalso been observed in a number of high latitude B-type low gravitystars. Hence the present results supports the recent classification ofthese objects as hot post-AGB stars. Relative to the overallmetallicity, the observed carbon deficiency of Barnard 29 coupled with asignificant nitrogen overabundance indicates that this star has left theAGB before the third dredge-up has occurred. The implications for AGBand post-AGB evolution are briefly discussed.
| The chemical composition of B-supergiant atmospheres
Not Available
| Galactic B-supergiants. II - Line strengths in the visible: Evidence for evolutionary effects?
Following the discovery by Lennon et al. (1992) of anomalously weakcarbon lines in the Galactic B-supergiants, a search was conducted forthe signatures of CNO processed material in the atmospheres of thesestars. It was found that the NII line strengths around spectral type B2correlate with luminosity, but exhibit a clear anticorrelation with theCII lines. It is suggested that this trend may be evidence for CNOprocessed material contaminating the atmospheres of the most luminousstars. The CNO processing signature was found to be most pronounced inthe more luminous supergiants, in qualitative agreement with stellarevolution calculations (provided that such stars have passed through aprevious red-supergiant phase of evolution).
| Groups of stars with common motion in the Galaxy. Groups of O and B stars
Not Available
| Galactic B-supergiants. I - an atlas of O9-B9 supergiant spectra from 3950 A to 4950 A
CCD spectra are presented for supergiants of spectral types O9-B9 andluminosity subclasses Ia and Ib. They cover the wavelength region fromapproximately 3950 A to 4950 A at a resolution of 0.8 A, and normallyhave a signal-to-noise in excess of 150 at 4600 A. The spectra arediscussed in respect to their classification. A number of stars showclear evidence of the 'filling in' of hydrogen lines by emission fromthe stellar wind, while HD 190603, a B1.5 Ia(+) hypergiant, exhibits anH-beta P-Cygni type line-profile. Also reported is the finding of a newnitrogen weak star, HD 13866, in the Per OB1 association which isclassified here as BC2 Ib.
| The stellar temperature scale for stars of spectral types from O8 to F6 and the standard deviation of the MK spectral classification
Empirical effective temperature of 211 early-type stars found in aprevious investigation (Kontizas and Theodossiou, 1980; Theodossiou,1985) are combined with the effective temperatures of 313 early-typestars from the literature. From these effective temperatures of a totalnumber of 524 early-type stars of spectral types from O8 to F6 a newstellar temperature scale is developed along with the standard deviationof the MK spectral classification.
| Groups of stars with common motion in the Galaxy - Groups of B stars of luminosity classes I and II and their comparison with groups of long-period Cepheids and open clusters
In a sample of 93 stars of luminosity classes I and II, ten groups withcommon motion in space are isolated. The reality of five groups isestablished by numerical experiment. A comparison is made with groups oflong-period Cepheids and open clusters. Regularities in the distributionof groups of different objects in space are found. The reality of therotation of a star aggregate consisting of three Cepheid groups isestablished.
| 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.
| The diffuse interstellar bands. VI - New features near 6800 A
A group of about 29 weak lines lying between 6767 and 6862 A has beenfound on high signal-to-noise ratio (S/N) scans of reddened stars. Theyhave been observed in stars between types O3 and A5, do not appear inunreddened stars of those types observed with the same equipment, andstrengthen with icreasing E(B-V). For these reasons, they are believedto be interstellar. Although narrow, they are not perfectly sharp at aresolution of 35,000. Five or six of the stronger features are nearlyuniformly spaced at intervals of 35/cm, which is suggestive of thespacing expected for rotational structure of light hydrides such as CH,NH and OH, but no plausible carrier of those species has beenidentified.
| Small Magellanic Cloud: H-gamma-line equivalent widths and luminosity classes of the brightest blue star members
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1987A&AS...69..421A&db_key=AST
| The Mv-W(H-gamma) calibration for O6 to A3 supergiants
The Mv-W(H-gamma) calibration of main-sequence stars of Millward andWalker (1985) is evaluated by observing bright supergiants in clusters.Fifty-two spectra of 39 O, B, and A supergiants combined with 19 higherdispersion spectra of 18 stars are studied. Wing profiles were generatedby fitting a two-component, absorption-coefficient model to the H-gammaprofiles. The calculated Mv data are compared to photometric values. Itis observed that there is a difference in the present calibration andthe Millward and Walker calibration due to the manner in which the wingprofiles are defined; however, the nonlinear relation between thespectral types and W(H-gamma) found by Millward and Walker is confirmed.
| Observations of interstellar diffuse absorption band at 4430 A
Observations of the interstellar diffuse absorption band at 4430 A for800 O and B stars in Neckel's (1967) catalog are being carried out, and482 spectra obtained up to September 1983 have been reduced. It isconfirmed that the strength of the interstellar diffuse absorption bandat 4430 A does not simply relate to the abundance of interstellar grainson the line of sight. The relation between the color excess E(B-V) andthe equivalent width of the band to the direction of l = 130-140 deg andb = -5 to +5 deg shows that some parameter(s) other than E(B-V) is (are)needed to understand the cause of this band.
| Catalog of O-B stars observed with Tokyo Meridian Circle
A catalog of the O-B stars, selected from 'Blaauw-Parenago' list andRubin's catalog, has been compiled on the FK4 system by the observationsmade with Gautier 8-inch Meridian Circle at the Tokyo AstronomicalObservatory during the period, 1971 to 1979. It contains 1059 stars andwas compiled for the future establishment of high precision propermotions of O-B stars.
| A study of B-type supergiants with the uvby,beta photometric system
The applicability of the uvby,beta photometric system to theclassification and study of B-type supergiants (BTS) is investigatedusing published data on 157 BTS and observations of 17 BTS made with the36-in. reflector at McDonald Observatory. The results are presented intabular form and analyzed to produce preliminary calibrations ofluminosity class vs. beta index and of absolute magnitude (Mv) vs. beta(or delta Mv vs. delta beta) for four associations of stars. Theeffectiveness of various color indices as temperature indicators isdiscussed. It is shown that there is good correspondence between MK anduvby,beta classifications of B-type main-sequence stars, giants, andBTS, confirming the usefulness of the uvby,beta system in furtherresearch on BTS.
| A survey of interstellar neutral potassium. I - Abundances and physical conditions in clouds toward 188 early-type stars
Observations of interstellar absorption in the resonance doublet 7664,7698 A of neutral potassium toward 188 early-type stars at a spectralresolution of 8 km/s are reported. The 7664 A line is successfullyseparated from nearly coincident telluric O2 absorption for all but afew of the 165 stars for which K I absorption is detected, makingpossible an abundance analysis by the doublet ratio method. Therelationships between the potassium abundances and other atomicabundances, the abundance of molecular hydrogen, and interstellarreddening are investigated.
| Four-color and H-beta photometry for O-A0 type stars in three regions near the galactic equator
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1982A&AS...49..561W&db_key=AST
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Observation and Astrometry data
| Constellation: | Auriga |
| Right ascension: | 04h56m19.90s |
| Declination: | +36°10'08.0" |
| Apparent magnitude: | 6.07 |
| Distance: | 3571.429 parsecs |
| Proper motion RA: | 0.5 |
| Proper motion Dec: | -4.9 |
| B-T magnitude: | 6.492 |
| V-T magnitude: | 6.13 |
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