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Photospheric CNO Abundances of Solar-Type Stars
We determined the C, N, and O abundances of 160 nearby F, G, and Kdwarfs and subgiants by using spectra obtained with the HIDESspectrograph at Okayama Astrophysical Observatory, with the purposes of(1) establishing the runs of [C/Fe], [N/Fe], and [O/Fe] for thesegalactic disk stars in the metallicity range of -1 ≲ [Fe/H] ≲+0.4, (2) searching for any difference in the CNO abundances ofplanet-host stars as compared to non-planet-host stars, and (3)examining the consistency of the abundances derived from different linesto check the validity of the analysis. The non-LTE effect on theabundance determination was taken into consideration based on ourextensive statistical-equilibrium calculations. We confirmed thatconsistent abundances are mostly accomplished between different lines,and that [C/Fe] as well as [O/Fe] progressively increase with a decreasein [Fe/H] with the slope of the former ( 0.2‑0.3) beingshallower than the latter ( 0.4‑0.5), while [N/Fe] does notshow any clear systematic trend with the metallicity. The [C/Fe],[N/Fe], and [O/Fe] values of 27 planet-harboring stars (included in oursample of 160 stars) were shown to be practically indistinguishable fromthose exhibited by non-planet-harboring stars of similar metallicities.
| Estimation of Carbon Abundances in Metal-Poor Stars. I. Application to the Strong G-Band Stars of Beers, Preston, and Shectman
We develop and test a method for the estimation of metallicities([Fe/H]) and carbon abundance ratios ([C/Fe]) for carbon-enhancedmetal-poor (CEMP) stars based on the application of artificial neuralnetworks, regressions, and synthesis models to medium-resolution (1-2Å) spectra and J-K colors. We calibrate this method by comparisonwith metallicities and carbon abundance determinations for 118 starswith available high-resolution analyses reported in the recentliterature. The neural network and regression approaches make use of apreviously defined set of line-strength indices quantifying the strengthof the Ca II K line and the CH G band, in conjunction with J-K colorsfrom the Two Micron All Sky Survey Point Source Catalog. The use ofnear-IR colors, as opposed to broadband B-V colors, is required becauseof the potentially large affect of strong molecular carbon bands onbluer color indices. We also explore the practicality of obtainingestimates of carbon abundances for metal-poor stars from the spectralinformation alone, i.e., without the additional information provided byphotometry, as many future samples of CEMP stars may lack such data. Wefind that although photometric information is required for theestimation of [Fe/H], it provides little improvement in our derivedestimates of [C/Fe], and hence, estimates of carbon-to-iron ratios basedsolely on line indices appear sufficiently accurate for most purposes.Although we find that the spectral synthesis approach yields the mostaccurate estimates of [C/Fe], in particular for the stars with thestrongest molecular bands, it is only marginally better than is obtainedfrom the line index approaches. Using these methods we are able toreproduce the previously measured [Fe/H] and [C/Fe] determinations withan accuracy of ~0.25 dex for stars in the metallicity interval-5.5<=[Fe/H]<=-1.0 and with 0.2<=(J-K)0<=0.8. Athigher metallicity, the Ca II K line begins to saturate, especially forthe cool stars in our program, and hence, this approach is not useful insome cases. As a first application, we estimate the abundances of [Fe/H]and [C/Fe] for the 56 stars identified as possibly carbon-rich, relativeto stars of similar metal abundance, in the sample of ``strong G-band''stars discussed by Beers, Preston, and Shectman.
| Magnesium abundances in mildly metal-poor stars from different indicators
We present Mg abundances derived from high-resolution spectra usingseveral MgI and two high-excitation MgII lines for 19 metal-poor starswith [Fe/H] values between -1.1 and +0.2. The main goal is to search forsystematic differences in the derived abundances between the twoionization state lines. Our analysis shows that the one-dimensionallocal thermodynamic equilibrium (LTE) and non-LTE (N-LTE) study finds avery good agreement between these features. The [Mg/Fe] versus [Fe/H]relationship derived, despite the small sample of stars, is also inagreement with the classical figure of increasing [Mg/Fe] withdecreasing metallicity. We find a significant scatter however, in the[Mg/Fe] ratio at [Fe/H]~-0.6 which is currently explained as aconsequence of the overlap at this metallicity of thick- and thin-discstars, which were probably formed from material with differentnucleosynthesis histories. We speculate on the possible consequences ofthe agreement found between MgI and MgII lines on the very well-known Oproblem in metal-poor stars. We also study the [O/Mg] ratio in thesample stars using O abundances from the literature and find that thecurrent observations and nucleosynthetic predictions from Type IIsupernovae disagree. We briefly discuss some alternatives to solve thisdiscrepancy.
| Oxygen line formation in late-F through early-K disk/halo stars. Infrared O I triplet and [O I] lines
In order to investigate the formation of O I 7771-5 and [O I] 6300/6363lines, extensive non-LTE calculations for neutral atomic oxygen werecarried out for wide ranges of model atmosphere parameters, which areapplicable to early-K through late-F halo/disk stars of variousevolutionary stages.The formation of the triplet O I lines was found to be well described bythe classical two-level-atom scattering model, and the non-LTEcorrection is practically determined by the parameters of theline-transition itself without any significant relevance to the detailsof the oxygen atomic model. This simplifies the problem in the sensethat the non-LTE abundance correction is essentially determined only bythe line-strength (Wlambda ), if the atmospheric parametersof Teff, log g, and xi are given, without any explicitdependence of the metallicity; thus allowing a useful analytical formulawith tabulated numerical coefficients. On the other hand, ourcalculations lead to the robust conclusion that LTE is totally valid forthe forbidden [O I] lines.An extensive reanalysis of published equivalent-width data of O I 7771-5and [O I] 6300/6363 taken from various literature resulted in theconclusion that, while a reasonable consistency of O I and [O I]abundances was observed for disk stars (-1 <~ [Fe/H] <~ 0), theexistence of a systematic abundance discrepancy was confirmed between OI and [O I] lines in conspicuously metal-poor halo stars (-3 <~[Fe/H] <~ -1) without being removed by our non-LTE corrections, i.e.,the former being larger by ~ 0.3 dex at -3 <~ [Fe/H] <~ -2.An inspection of the parameter-dependence of this discordance indicatesthat the extent of the discrepancy tends to be comparatively lessenedfor higher Teff/log g stars, suggesting the preference ofdwarf (or subgiant) stars for studying the oxygen abundances ofmetal-poor stars.Tables 2, 5, and 7 are 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/402/343 and Table\ref{tab3} is only available in electronic form athttp://www.edpsciences.org
| ICCD Speckle Observations of Binary Stars. XXIII. Measurements during 1982-1997 from Six Telescopes, with 14 New Orbits
We present 2017 observations of 1286 binary stars, observed by means ofspeckle interferometry using six telescopes over a 15 year period from1982 April to 1997 June. These measurements constitute the 23dinstallment in CHARA's speckle program at 2 to 4 m class telescopes andinclude the second major collection of measurements from the MountWilson 100 inch (2.5 m) Hooker Telescope. Orbital elements are alsopresented for 14 systems, seven of which have had no previouslypublished orbital analyses.
| Abundances of light elements in metal-poor stars. III. Data analysis and results
We present the results of the analysis of an extensive set of new andliterature high quality data concerning Fe, C, N, O, Na, and Mg. Thisanalysis exploited the T_eff scale determined in Gratton et al. (1996a),and the non-LTE abundance corrections computed in Gratton et al.(1999a). Results obtained with various abundance indices are discussedand compared. Detailed comparison with models of galactic chemicalevolution will be presented in future papers of this series. Our non-LTEanalysis yields the same O abundances from both permitted and forbiddenlines for stars with T_eff >4600 K, in agreement with King (1993),but not with other studies using a lower T_eff -scale for subdwarfs.However, we obtain slightly smaller O abundances for the most luminousmetal-poor field stars than for fainter stars of similar metallicities,an effect attributed to inadequacies of the adopted model atmospheres(Kurucz 1992, with overshooting) for cool stars. We find a nearlyconstant O overundance in metal-poor stars ([Fe/H]<-0.8), at a meanvalue of 0.46+/- 0.02 dex (sigma =0.12, 32 stars), with only a gentleslope with [Fe/H] ( ~ -0.1); this result is different from the steeperslope recently obtained using OH band in the near UV. If only bonafideunmixed stars are considered, C abundances scale with Fe ones (i.e.[C/Fe]~ 0) down to [Fe/H] ~ -2.5. Due to our adoption of a differentT_eff scale, we do not confirm the slight C excess in the most metalpoor disk dwarfs (-0.8<[Fe/H]<-0.4) found in previousinvestigations. Na abundances scale as Fe ones in the high metallicityregime, while metal-poor stars present a Na underabundance. None of thefield stars analyzed belong to the group of O-poor and Na-rich starsobserved in globular clusters. Na is deficient with respect to Mg inhalo and thick disk stars; within these populations, Na deficiency maybe a slow function of [Mg/H]. Solar [Na/Mg] ratios are obtained for thindisk stars. Tables~ 2 to 9 are only available in electronic form at theCDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strabg.fr/Abstract.html
| Two-colour photometry for 9473 components of close Hipparcos double and multiple stars
Using observations obtained with the Tycho instrument of the ESAHipparcos satellite, a two-colour photometry is produced for componentsof more than 7 000 Hipparcos double and multiple stars with angularseparations 0.1 to 2.5 arcsec. We publish 9473 components of 5173systems with separations above 0.3 arcsec. The majority of them did nothave Tycho photometry in the Hipparcos catalogue. The magnitudes arederived in the Tycho B_T and V_T passbands, similar to the Johnsonpassbands. Photometrically resolved components of the binaries withstatistically significant trigonometric parallaxes can be put on an HRdiagram, the majority of them for the first time. Based on observationsmade with the ESA Hipparcos satellite.
| ICCD Speckle Observations of Binary Stars. XVII. Measurements During 1993-1995 From the Mount Wilson 2.5-M Telescope.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1997AJ....114.1639H&db_key=AST
| 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
| Classification of Population II Stars in the Vilnius Photometric System. I. Methods
The methods used for classification of Population II stars in theVilnius photometric system are described. An extensive set of standardswith known astrophysical parameters compiled from the literature sourcesis given. These standard stars are classified in the Vilnius photometricsystem using the methods described. The accuracy of classification isevaluated by a comparison of the astrophysical parameters derived fromthe Vilnius photometric system with those estimated from spectroscopicstudies as well as from photometric data in other systems. For dwarfsand subdwarfs, we find a satisfactory agreement between our reddeningsand those estimated in the uvbyscriptstyle beta system. The standarddeviation of [Fe/H] deter mined in the Vilnius system is about 0.2 dex.The absolute magnitude for dwarfs and subdwarfs is estimated with anaccuracy of scriptstyle <=0.5 mag.
| Abundances of light elements in metal-poor stars. I. Atmospheric parameters and a new T_eff_ scale
We present atmospheric parameters for about 300 stars of differentchemical composition, whose spectra will be used to study the galacticenrichment of Fe and light elements. These parameters were derived usingan homogeneous iterative procedure, which considers new calibrations ofcolour-T_eff_ relations for F, G and K-type stars based on Infrared FluxMethod (IRFM) and interferometric diameters for population I stars, andthe Kurucz (1992) model atmospheres. We found that these calibrationsyield a self-consistent set of atmospheric parameters forT_eff_>4400K, representing a clear improvement over results obtainedwith older model atmospheres. Using this T_eff_ -scale and Feequilibrium of ionization, we obtained very low gravities (implyingluminosities incompatible with that expected for RGB stars) formetal-poor stars cooler than 4400K; this might be due either to amoderate Fe overionization (expected from statistical equilibriumcalculations) or to inadequacy of Kurucz models to describe theatmospheres of very cool giants. Our T_eff_ scale is compared with otherscales recently used for metal-poor stars; it agrees well with thoseobtained using Kurucz (1992) models, but it gives much larger T_eff_'sthan those obtained using OSMARCS models (Edvardsson et al. 1993). Thisdifference is attributed to the different treatment of convection in thetwo sets of models. For the Sun, the Kurucz (1992) model appears to bepreferable to the OSMARCS ones because it better predicts the solar limbdarkening; furthermore, we find that our photometric T_eff_ 's formetal-poor stars agree well with both direct estimates based on theIRFM, and with T_eff_'s derived from Hα wings when using Kuruczmodels.
| The carbon-to-oxygen ratio in halo dwarfs
C I and O I lines have been observed in 34 metal-poor dwarfs andsubgiants, and both LTE and non-LTE analyses of these lines have beenperformed. Analysis of the lines is vitiated by a systematictemperature-dependent error, showing that present methods of analysismay not give the correct elemental abundances. The (C/O) ratios are,however, almost independent of effective temperature and are thereforereliable. These ratios are found to be essentially constant over themetallicity range (Fe/H) = -2.7 - -1.0 in the survey. The mean value is(C/O) = -0.57 +/- 0.12. Analysis of CH lines gives (C/Fe) = -0.14 +/-0.20. It is considered that the O abundance in halo stars is morereliably indicated by the forbidden O I line, and it is suggested that(O/Fe) = +0.45 +/- 0.1 is representative for (Fe/H) less than -1. It issuggested that (C/Fe) = -0.1 and (O/Fe) about +0.5 are representative ofthe halo.
| A survey of proper-motion stars. II - Extracting metallicities from high-resolution, low-S/N spectra
Calculations of a grid of high-resolution synthetic spectra coveringwavelengths 5150-5250 A, Teff 4750-6500 K, metal abundances from +0.5 to-3.0, and gravities of log g = 4.5 or 4.0 are discussed. Metallicitiesfor 48 stars whose abundances have been previously determined fromhigh-resolution, high-S/N spectra and conventional fine-analysistechniques are estimated. None of the observed spectra are high S/N, yetthey result in metallicities with internal scatter of typically 0.1 dex.Comparison with published fine analyses shows excellent agreement (-0.03plus or minus 0.02 dex) for metal-poor stars, and a small systematicerror at higher abundances, which is easily corrected.
| Carbon abundances in halo dwarfs
A spectrum synthesis analysis has been made of Digicon observations ofCH in 32 halo F and G dwarfs with iron abundances as low as (Fe/H)approximately equal to -2.5. The results, combined with earlier results,also based on spectrum synthesis of Digicon CH spectra, show that carbonfollows iron down to (Fe/H) about -1.8; at lower metallicities there isevidence of a positive trend in (C/Fe). It is suggested that the changein slope of the (C/Fe) vs (Fe/H) relationship at (Fe/H) about -1.8 isdue to the appearance of Type I supernovae. The sense of the change ofslope is consistent with the prediction that Type I supernovae areinefficient producers of carbon. More carbon abundances, determined fromanalysis of CH in even more metal-deficient stars and, also, determinedfrom C I lines, are needed in order to establish the relationshipbetween carbon and iron abundances in extremely metal-deficient (Fe/Hless than about -2.0) dwarfs more firmly. One of the program stars (BD-0 degrees 4470) is found to be a double-lined spectroscopic binarycomposed of two nearly identical halo dwarfs.
| Metal-Deficient Giants in the Galactic Field - Catalogue and Some Physical Parameters
Not Available
| Three-dimensional calssification of F-M type halo stars in the Vilnius photometric system
Not Available
| UVBY beta photometry and MK spectral classification.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1976A&AS...24...69O&db_key=AST
| A Search for Metal-Deficient Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1970ApJS...22..117B&db_key=AST
| New double stars of small separation
Not Available
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| Csillagkép: | Pegazus |
| Rektaszcenzió: | 22h10m57.52s |
| Deklináció: | +24°29'18.8" |
| Vizuális fényesség: | 8.737 |
| Távolság: | 156.495 parszek |
| RA sajátmozgás: | 55.7 |
| Dec sajátmozgás: | 23.9 |
| B-T magnitude: | 9.209 |
| V-T magnitude: | 8.776 |
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