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High-resolution spectroscopic observations of two chemically peculiar metal-poor stars: HD 10613 and BD+04°2466
Aims: We determined the atmospheric parameters and abundance pattern oftwo chemically peculiar metal-poor stars: HD 10613 and BD+04°2466 inorder to better understand their evolutionary state and the nature ofthe s-element enhancement of these stars. Methods: We used highresolution optical spectroscopy. Atmospheric parameters and abundanceswere determined in the local-thermodynamic-equilibrium model atmospheresof Kurucz using the spectral analysis code MOOG. Results: Weconclude that HD 10613 is another metal-poor barium star with C/O = 0.52and [Fe/H] = -0.82, while BD+04°2466 is a CH star with C/O = 3.6 and[Fe/H] = -1.92 rather than a metal-deficient barium star as it waspreviously classified. BD+04°2466 appears to be enriched in leadwith [Pb/Ce] = +0.85 and [Pb/La] = +0.72. For BD+04°2466 theabundance of lead is in agreement with predictions from AGB models. Dueto the low luminosity of these two stars, their observed s-processoverabundance is better explained by mass-transfer in the past from anAGB star.Based on observations made with the 1.52 m and 2.2 m telescope at theEuropean Southern Observatory (La Silla, Chile).
| Light Element Abundances in Two Chemically Peculiar Stars: HD 104340 and HD 206983
We derive carbon, nitrogen, oxygen, and lithium abundances as well as12C/13C isotopic ratios in two chemically peculiarred giant stars: HD 104340 and HD 206983. The abundances were determinedvia spectrum synthesis of optical high-resolution spectra containingC2, CH, CN, [O I], and Li I lines. Our results indicate thatHD 206983 is a barium star, while HD 104340, although showingenhancements of s-process elements, should not be considered as aclassical barium star: its barium star nature can be explained byinternal nucleosynthesis. The low metallicity giant HD 104340 canexperience deeper convective mixing and, consequently, a largerdredge-up of CNO-cycle products compared to normal red giants. The lightelement abundance pattern of HD 104340 resembles anomalies resultingfrom the appearance on the stellar surface of material enriched bytriple-α and CNO cycling.Based on the observations made with the 1.52 m telescope at the EuropeanSouthern Observatory (La Silla, Chile) under the agreement withObservatório Nacional (Brazil).
| The Origin of Carbon Enhancement and the Initial Mass Function of Extremely Metal-poor Stars in the Galactic Halo
It is known that the carbon-enhanced, extremely metal-poor (CEMP) starsconstitute a substantial proportion of the extremely metal-poor (EMP)stars of the Galactic halo, and a by far larger proportion than CH starsamong Population II stars. We investigate their origin by taking intoaccount an additional evolutionary path to the surface carbonenrichment, triggered by hydrogen engulfment by the helium flashconvection, in EMP stars with [Fe/H]<~-2.5. This process is distinctfrom the third dredge-up operating in more metal-rich stars and in EMPstars. In binary systems of EMP stars, the secondary stars become CEMPstars through mass transfer from the low- and intermediate- mass primarystars that have developed the surface carbon enhancement. Our binaryscenario can predict the variations in the abundances not only forcarbon but also for nitrogen and s-process elements and can reasonablyexplain the observed properties such as the stellar distributions of thecarbon abundances, the binary periods, and the evolutionary stages.Furthermore, from the observed frequencies of CEMP stars with andwithout s-process element enhancement, we demonstrate that the initialmass function of EMP stars needed gives the mean mass~10Msolar under the reasonable assumptions for the distributionsof orbital separations and mass ratios of the binary components. Thisalso indicates that the currently observed EMP stars were exclusivelyborn as the secondary members of binaries, making up ~10% of EMP binarysystems, with mass~108 Msolar in total; inaddition to CEMP stars with white dwarf companions, a significantfraction of them have experienced supernova explosions of theircompanions. We discuss the implications of the present results for theformation of the Galactic halo.
| Galactic model parameters for field giants separated from field dwarfs by their 2MASS and V apparent magnitudes
We present a method which separates field dwarfs and field giants bytheir 2MASS and V apparent magnitudes. This method is based onspectroscopically selected standards and is hence reliable. We appliedit to stars in two fields, SA 54 and SA 82, and we estimated a full setof Galactic model parameters for giants including their total localspace density. Our results are in agreement with the ones given in therecent literature.
| On metal-deficient barium stars and their link with yellow symbiotic stars
This paper addresses the question of why metal-deficient barium starsare not yellow symbiotic stars (YSyS). Samples of (suspected)metal-deficient barium (mdBa) stars and YSyS have been collected fromthe literature, and their properties reviewed. It appears in particularthat the barium nature of the suspected mdBa stars needs to beascertained by detailed abundance analyses. Abundances are thereforederived for two of them, HD 139409 and HD 148897, which reveal that HD148897 should not be considered a barium star. HD 139409 is a mildbarium star, with overabundances observed only for elements belonging tothe first s-process peak (Y and Zr). It is only moderately metal-poor([Fe/H] = -0.4). The evidence for binarity among mdBa stars is thenreviewed, using three different methods: (i) radial-velocity variations(from CORAVEL observations), (ii) Hipparcos astrometric data, and (iii)a method based on the comparison between the Hipparcos and Tycho-2proper motions. An orbit is obtained for HIP 55852, whereas evidence forthe (so far unknown) binary nature of HIP 34795, HIP 76605, HIP 97874and HIP 107478 is presented. No conclusion regarding the binary natureof HIP 11595, HIP 25161 could be reached. Two stars with no evidence forbinarity whatsoever (HIP 58596 and BD +3°2688) are candidateslow-metallicity thermally-pulsing asymptotic giant branch stars, asinferred from their large luminosities. The reason why mdBa stars arenot YSyS is suggested to lie in their different orbital perioddistributions: mdBa stars have on average longer orbital periods thanYSyS, and hence their companion accretes matter at a lower rate, for agiven mass loss rate of the giant star. The definite validation of thisexplanation should nevertheless await the determination of the orbitalperiods for the many mdBa stars still lacking periods, in order to makethe comparison more significant.
| Spectroscopic Verification of Barium Dwarf Candidates: The Analysis of HD 8270, HD 13551, and HD 22589
This work presents the abundance patterns of three barium dwarfcandidates, HD 8270, HD 13551, and HD 22589, based on high-resolutionoptical spectra. This work also reports the spectroscopic stellarparameters, temperature, and microturbulent velocity, as well as thestellar surface gravity from a solution of excitation and ionizationequilibria of Fe I and Fe II lines under the assumption of localthermodynamic equilibrium. The abundance analysis reveals that HD 8270,HD 13551, and HD 22589 have metallicities of [Fe/H]=-0.43, -0.28, and-0.12, respectively. It was found that the abundances of iron group andα-elements follow the abundance pattern of a disk population. Theheavy-element abundance patterns of the three stars show enhancements bya factor of 4-8 with respect to the Sun. The abundances of the s-processelements are discussed and compared with other barium giants and dwarfsthrough diagrams involving the indices [hs/ls] and [s/Fe]. Themetallicity distribution of barium giants and dwarfs is also discussed.Based on observations made with the 1.52 m telescope at the EuropeanSouthern Observatory (La Silla, Chile) under agreement withObservatório Nacional (Brazil).
| Carbon-rich giants in the HR diagram and their luminosity function
The luminosity function (LF) of nearly 300 Galactic carbon giants isderived. Adding BaII giants and various related objects, about 370objects are located in the RGB and AGB portions of the theoretical HRdiagram. As intermediate steps, (1) bolometric corrections arecalibrated against selected intrinsic color indices; (2) the diagram ofphotometric coefficients 1/2 vs. astrometric trueparallaxes varpi are interpreted in terms of ranges of photosphericradii for every photometric group; (3) coefficients CR andCL for bias-free evaluation of mean photospheric radii andmean luminosities are computed. The LF of Galactic carbon giantsexhibits two maxima corresponding to the HC-stars of the thick disk andto the CV-stars of the old thin disk respectively. It is discussed andcompared to those of carbon stars in the Magellanic Clouds and Galacticbulge. The HC-part is similar to the LF of the Galactic bulge,reinforcing the idea that the Bulge and the thick disk are part of thesame dynamical component. The CV-part looks similar to the LF of theLarge Magellanic Cloud (LMC), but the former is wider due to thesubstantial errors on HIPPARCOS parallaxes. The obtained meanluminosities increase with increasing radii and decreasing effectivetemperatures, along the HC-CV sequence of photometric groups, except forHC0, the earliest one. This trend illustrates the RGB- and AGB-tracks oflow- and intermediate-mass stars for a range in metallicities. From acomparison with theoretical tracks in the HR diagram, the initial massesMi range from about 0.8 to 4.0 Msun for carbongiants, with possibly larger masses for a few extreme objects. A largerange of metallicities is likely, from metal-poor HC-stars classified asCH stars on the grounds of their spectra (a spheroidal component), tonear-solar compositions of many CV-stars. Technetium-rich carbon giantsare brighter than the lower limit Mbol =~ -3.6+/- 0.4 andcentered at =~-4.7+0.6-0.9 at about =~(2935+/-200) K or CV3-CV4 in our classification. Much like the resultsof Van Eck et al. (\cite{vaneck98}) for S stars, this confirms theTDU-model of those TP-AGB stars. This is not the case of the HC-stars inthe thick disk, with >~ 3400 K and>~ -3.4. The faint HC1 and HC2-stars( =~ -1.1+0.7-1.0) arefound slightly brighter than the BaII giants ( =~-0.3+/-1.3) on average. Most RCB variables and HdC stars range fromMbol =~ -1 to -4 against -0.2 to -2.4 for those of the threepopulation II Cepheids in the sample. The former stars show the largestluminosities ( <~ -4 at the highest effectivetemperatures (6500-7500 K), close to the Mbol =~ -5 value forthe hot LMC RCB-stars (W Men and HV 5637). A full discussion of theresults is postponed to a companion paper on pulsation modes andpulsation masses of carbon-rich long period variables (LPVs; Paper IV,present issue). This research has made use of the Simbad databaseoperated at CDS, Strasbourg, France. Partially based on data from theESA HIPPARCOS astrometry satellite. Table 2 is only available inelectronic form at the 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/390/967
| New periodic variables from the Hipparcos epoch photometry
Two selection statistics are used to extract new candidate periodicvariables from the epoch photometry of the Hipparcos catalogue. Theprimary selection criterion is a signal-to-noise ratio. The dependenceof this statistic on the number of observations is calibrated usingabout 30000 randomly permuted Hipparcos data sets. A significance levelof 0.1 per cent is used to extract a first batch of candidate variables.The second criterion requires that the optimal frequency be unaffectedif the data are de-trended by low-order polynomials. We find 2675 newcandidate periodic variables, of which the majority (2082) are from theHipparcos`unsolved' variables. Potential problems with theinterpretation of the data (e.g. aliasing) are discussed.
| The Abundance Pattern of Two Barium Stars in the Galactic Halo: HD 104340 and HD 206983
We present the abundance pattern of two barium stars in the Galactichalo, HD 104340 and HD 206983, based on high-resolution optical spectra.We also determined the spectroscopic stellar atmospheric parameters,temperature, and microturbulent velocity, as well as stellar surfacegravity from a solution of excitation and ionization equilibria of Fe Iand Fe II lines under the assumption of local thermodynamic equilibrium.The abundance analysis reveals HD 104340 to be a metal-poor K giant with[Fe/H]=-1.72 and HD 206983 also a metal-poor K giant with [Fe/H]=-1.43.From a set of Fe I lines, the radial velocity is found to be 263.3+/-0.6km s-1 and -319.2+/-4.4 km s-1 for HD 104340 andHD 206983, respectively. Their high velocity, low metallicity, and highgalactic latitude imply that both stars are members of a Galactic halopopulation. From our study and by using information from the literaturewe believe that HD 206983 is another member of a group known asmetal-deficient barium stars. We compare the abundance pattern with theabundances of a halo population. We found that the abundances of theiron group, α-elements, manganese, copper, and zinc, as well assodium and magnesium, of HD 104340 and HD 206983 follow the abundancepattern of a halo population. The heavy element abundance pattern ofboth stars shows enhancement by a factor of 4-8 with respect to themetal-poor stars with the same metallicity as that analyzed by us. Wealso discuss the abundances of the s-process elements and compare ourresults with other objects that display the same degree of enrichmentdue to neutron capture reactions, binary systems, and AGB stars, througha diagram of metallicity versus neutron exposure given by the [hs/ls]index. Based on the observations made with the 1.52 m telescope at theEuropean Southern Observatory (La Silla, Chile) under agreement withObservatório Nacional (Brazil).
| Catalogue of [Fe/H] determinations for FGK stars: 2001 edition
The catalogue presented here is a compilation of published atmosphericparameters (Teff, log g, [Fe/H]) obtained from highresolution, high signal-to-noise spectroscopic observations. This newedition has changed compared to the five previous versions. It is nowrestricted to intermediate and low mass stars (F, G and K stars). Itcontains 6354 determinations of (Teff, log g, [Fe/H]) for3356 stars, including 909 stars in 79 stellar systems. The literature iscomplete between January 1980 and December 2000 and includes 378references. The catalogue is made up of two tables, one for field starsand one for stars in galactic associations, open and globular clustersand external galaxies. The catalogue is distributed through the CDSdatabase. Access to the catalogue with cross-identification to othersets of data is also possible with VizieR (Ochsenbein et al.\cite{och00}). The catalogue (Tables 1 and 2) is only available inelectronic form at the 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/373/159 and VizieRhttp://vizier.u-strasbg.fr/.
| The 74th Special Name-list of Variable Stars
We present the Name-list introducing GCVS names for 3153 variable starsdiscovered by the Hipparcos mission.
| Barium stars, galactic populations and evolution.
In this paper HIPPARCOS astrometric and kinematical data together withradial velocities from other sources are used to calibrate bothluminosity and kinematics parameters of Ba stars and to classify them.We confirm the results of our previous paper (where we used data fromthe HIPPARCOS Input Catalogue), and show that Ba stars are aninhomogeneous group. Five distinct classes have been found i.e. somehalo stars and four groups belonging to disk population: roughlysuper-giants, two groups of giants (one on the giant branch, the otherat the clump location) and dwarfs, with a few subgiants mixed with them.The confirmed or suspected duplicity, the variability and the range ofknown orbital periods found in each group give coherent resultssupporting the scenario for Ba stars that are not too highly massivebinary stars in any evolutionary stages but that all were previouslyenriched with Ba from a more evolved companion. The presence in thesample of a certain number of ``false'' Ba stars is confirmed. Theestimates of age and mass are compatible with models for stars with astrong Ba anomaly. The mild Ba stars with an estimated mass higher than3Msun_ may be either stars Ba enriched by themselves or``true'' Ba stars, which imposes new constraints on models.
| A catalogue of [Fe/H] determinations: 1996 edition
A fifth Edition of the Catalogue of [Fe/H] determinations is presentedherewith. It contains 5946 determinations for 3247 stars, including 751stars in 84 associations, clusters or galaxies. The literature iscomplete up to December 1995. The 700 bibliographical referencescorrespond to [Fe/H] determinations obtained from high resolutionspectroscopic observations and detailed analyses, most of them carriedout with the help of model-atmospheres. The Catalogue is made up ofthree formatted files: File 1: field stars, File 2: stars in galacticassociations and clusters, and stars in SMC, LMC, M33, File 3: numberedlist of bibliographical references The three files are only available inelectronic form at the Centre de Donnees Stellaires in Strasbourg, viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5), or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Absolute magnitudes and kinematics of barium stars.
The absolute magnitude of barium stars has been obtained fromkinematical data using a new algorithm based on the maximum-likelihoodprinciple. The method allows to separate a sample into groupscharacterized by different mean absolute magnitudes, kinematics andz-scale heights. It also takes into account, simultaneously, thecensorship in the sample and the errors on the observables. The methodhas been applied to a sample of 318 barium stars. Four groups have beendetected. Three of them show a kinematical behaviour corresponding todisk population stars. The fourth group contains stars with halokinematics. The luminosities of the disk population groups spread alarge range. The intrinsically brightest one (M_v_=-1.5mag,σ_M_=0.5mag) seems to be an inhomogeneous group containing bariumbinaries as well as AGB single stars. The most numerous group (about 150stars) has a mean absolute magnitude corresponding to stars in the redgiant branch (M_v_=0.9mag, σ_M_=0.8mag). The third group containsbarium dwarfs, the obtained mean absolute magnitude is characteristic ofstars on the main sequence or on the subgiant branch (M_v_=3.3mag,σ_M_=0.5mag). The obtained mean luminosities as well as thekinematical results are compatible with an evolutionary link betweenbarium dwarfs and classical barium giants. The highly luminous group isnot linked with these last two groups. More high-resolutionspectroscopic data will be necessary in order to better discriminatebetween barium and non-barium stars.
| A New Version of the Catalog of CH and Related Stars (CH95 Catalog)
A new version of the catalog of CH and related stars contains 244 fieldstars and 17 globular cluster stars. Here a list of these stars withtheir coordinates, their positions in the HR diagram and somestatistical diagrams is presented. The catalog will soon be available inthe printed and computerized versions.
| UBV photometry of barium stars
Magnitudes in V and B-V and U-B colors observed by the 91-cm telescopeat Okayama are presented for 109 stars including both classical andmarginal barium stars. The two-color diagram shows a fair amount ofspread. This can be interpreted by interstellar reddening and variableamounts of line blocking effect. Both classical and marginal bariumstars form a fairly homogeneous group.
| Subgiant CH stars. II - Chemical compositions and the evolutionary connection with barium stars
Chemical abundances in 15 subgiant CH stars, five barium stars, and fourobjects classified as metal-deficient barium stars are determinedthrough model-atmosphere analyses of high-resolution photographicechelle spectrograms. The stars in each of these groups show enhancedsurface abundances of carbon and the very heavy elements produced bys-process neutron-capture reactions. The atmospheric parameters ofsubgiant CH stars are found to be typical of F- and G-type main-sequencestars and subgiants. Barium stars are more luminous G- and K-typegiants. Both classes of objects constitute about 1 percent of theirrespective populations, and exhibit a high incidence (about 100 percent)of the membership in wide spectroscopic binaries. Subgiant CH starsoccur on the main sequence, but only in the T(eff) range 6000-6800 K. Itis argued that subgiant CH stars are created when an AGB star in a widebinary contaminates its main-sequence companion with carbon ands-processed material.
| Taxonomy of barium stars
Spectral classification, barium intensity, radial velocity, luminosity,and kinematical properties are determined for 389 barium stars byanalyzing image-tube spectra and photometric observation data. Diskkinematics for the stars are based on whether they are Ba weak or Bastrong. Weak barium stars in general have smaller velocity dispersions,brighter apparent magnitude, and lower luminosity than strong bariumstars. These characteristics are confirmed by solving for meanspectroscopic distances, z-scale height distances, and reduced propermotions.
| Kinematic and spatial distributions of barium stars - Are the barium stars and AM stars related?
The possibility of an evolutionary link between Am stars and bariumstars is considered, and an examination of previous data suggests thatbarium star precursors are main-sequence stars of intermediate mass, aremost likely A and/or F dwarfs, and are intermediate-mass binaries withclose to intermediate orbital separations. The possible role of masstransfer in the later development of Am systems is explored. Masstransfer and loss from systems with a range of masses and orbitalseparations may explain such statistical peculiarities of barium starsas the large dispersion in absolute magnitude, the large range ofelemental abundances from star to star, and the small number of starswith large peculiar velocities.
| Intermediate-infrared excesses of barium stars
Some barium stars show large excesses at 10 microns. These excessesappear unrelated to other atmospheric broadband characteristics, and arestrongly indicative of circumstellar dust. This supports theories thatprevious mass transfer in an evolved binary system may be responsiblefor their spectral peculiarities. Spectral energy distributions ofbarium stars indicate that other broadband peculiarities are likely asfollows: strong deficiencies exist in the regions of the B and Ifilters, while weak excesses appear in the H and M spectral regions.These peculiarities appear to correlate with the barium intensity.Energy exceses are insufficient to balance deficiencies unless either(1) the V band itself represents an excess, or (2) there are additionalexcesses at shorter wavelengths. The precise atmospheric phenomenonleading to such deviation from a blackbody spectral distribution isunknown.
| Infrared Excesses of Barium Stars
Not Available
| A catalog of spectral classification and photometry of barium stars
Many other Ba II stars have been found, since the enhancement of theline of singly ionized barium (4554 A) in late-type, high-luminositystars was discovered by Bidelman and Keenan (1951). The majority ofstars so identified are listed in a study conducted by MacConnell et al.(1972). MacConnell et al. identified 150 'certain' barium stars and anadditional 90 'marginal' barium stars from inspection of objective-prismplates of the Michigan Spectral Survey of the southern sky. Since themajority of known Ba II stars were discovered with objective-prismplates, they have lacked high-quality spectral classifications. It hasbeen attempted to obtain these data along with broad- andintermediate-band photometry, in order to study the properties of thissubgroup of stars in greater detail than has heretofore been possible.Except for the stars recently identified by Bidelman (1981), the list ofspectroscopic and photometric data in Table 1 includes virtually allrecognized barium stars. The stars identified by Bidelman are listed inTable 2.
| Radial velocities of faint stars from objective prism plates
A simple method by which the approximate radial velocity of a star maybe obtained from objective prism plates is described in detail. Themethod has been used to derive the velocities of 41 faint stars, most ofwhich have metal-weak spectra and are shown to be high-velocity objects.It is shown that this method may be generalized so that the radialvelocities for all measurable stars on an objective prism plate can beobtained.
| The absolute magnitudes of the barium stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1972AJ.....77..384M&db_key=AST
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| Csillagkép: | Holló |
| Rektaszcenzió: | 12h00m57.27s |
| Deklináció: | -21°15'02.8" |
| Vizuális fényesség: | 8.18 |
| Távolság: | 10000000 parszek |
| RA sajátmozgás: | -12.7 |
| Dec sajátmozgás: | -44.5 |
| B-T magnitude: | 9.962 |
| V-T magnitude: | 8.328 |
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