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Infrared Study of J-Type Carbon Stars Based on Infrared Astronomical Satellite, Two Micron All Sky Survey, and Infrared Space Observatory Data
We collected 113 J-type carbon stars from the published literature.Observations from 2MASS, IRAS, and ISO show that, except for silicatecarbon stars in the J-type carbon star domain, the infrared propertiesof the other J-type carbon stars are quite similar to those of ordinarycarbon stars. The above results imply that the chemical peculiarity ofenhanced 13C for J-type carbon stars is not reflected in theinfrared region. In addition, the possible evolutionary scenario andbinarity for J-type carbon stars are also discussed.
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| Hipparcos red stars in the HpV_T2 and V I_C systems
For Hipparcos M, S, and C spectral type stars, we provide calibratedinstantaneous (epoch) Cousins V - I color indices using newly derivedHpV_T2 photometry. Three new sets of ground-based Cousins V I data havebeen obtained for more than 170 carbon and red M giants. These datasetsin combination with the published sources of V I photometry served toobtain the calibration curves linking Hipparcos/Tycho Hp-V_T2 with theCousins V - I index. In total, 321 carbon stars and 4464 M- and S-typestars have new V - I indices. The standard error of the mean V - I isabout 0.1 mag or better down to Hp~9 although it deteriorates rapidly atfainter magnitudes. These V - I indices can be used to verify thepublished Hipparcos V - I color indices. Thus, we have identified ahandful of new cases where, instead of the real target, a random fieldstar has been observed. A considerable fraction of the DMSA/C and DMSA/Vsolutions for red stars appear not to be warranted. Most likely suchspurious solutions may originate from usage of a heavily biased color inthe astrometric processing.Based on observations from the Hipparcos astrometric satellite operatedby the European Space Agency (ESA 1997).}\fnmsep\thanks{Table 7 is onlyavailable 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/qcat?J/A+A/397/997
| 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
| Long period variable stars: galactic populations and infrared luminosity calibrations
In this paper HIPPARCOS astrometric and kinematic data are used tocalibrate both infrared luminosities and kinematical parameters of LongPeriod Variable stars (LPVs). Individual absolute K and IRAS 12 and 25luminosities of 800 LPVs are determined and made available in electronicform. The estimated mean kinematics is analyzed in terms of galacticpopulations. LPVs are found to belong to galactic populations rangingfrom the thin disk to the extended disk. An age range and a lower limitof the initial mass is given for stars of each population. A differenceof 1.3 mag in K for the upper limit of the Asymptotic Giant Branch isfound between the disk and old disk galactic populations, confirming itsdependence on the mass in the main sequence. LPVs with a thin envelopeare distinguished using the estimated mean IRAS luminosities. The levelof attraction (in the classification sense) of each group for the usualclassifying parameters of LPVs (variability and spectral types) isexamined. Table 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/374/968 or via ASTRIDdatabase (http://astrid.graal.univ-montp2.fr).
| The effective temperatures of carbon-rich stars
We evaluate effective temperatures of 390 carbon-rich stars. Theinterstellar extinction on their lines of sights was determined andcircumstellar contributions derived. The intrinsic (dereddened) spectralenergy distributions (SEDs) are classified into 14 photometric groups(HCi, CVj and SCV with i=0,5 and j=1,7). The newscale of effective temperatures proposed here is calibrated on the 54angular diameters (measured on 52 stars) available at present from lunaroccultations and interferometry. The brightness distribution on stellardiscs and its influence on diameter evaluations are discussed. Theeffective temperatures directly deduced from those diameters correlatewith the classification into photometric groups, despite the large errorbars on diameters. The main parameter of our photometric classificationis thus effective temperature. Our photometric < k right >1/2 coefficients are shown to be angular diameters on arelative scale for a given photometric group, (more precisely for agiven effective temperature). The angular diameters are consistent withthe photometric data previously shown to be consistent with the trueparallaxes from HIPPARCOS observations (Knapik, et al. \cite{knapik98},Sect. 6). Provisional effective temperatures, as constrained by asuccessful comparison of dereddened SEDs from observations to modelatmosphere predictions, are in good agreement with the values directlycalculated from the observed angular diameters and with those deducedfrom five selected intrinsic color indices. These three approaches wereused to calibrate a reference angular diameter Phi 0 and theassociated coefficient CT_eff. The effective temperatureproposed for each star is the arithmetic mean of two estimates, one(``bolometric'') from a reference integrated flux F0, theother (``spectral'') from calibrated color indices which arerepresentative of SED shapes. Effective temperatures for about 390carbon stars are provided on this new homogeneous scale, together withvalues for some stars classified with oxygen-type SEDs with a total of438 SEDs (410 stars) studied. Apparent bolometric magnitudes are given.Objects with strong infrared excesses and optically thick circumstellardust shells are discussed separately. The new effective temperaturescale is shown to be compatible and (statistically) consistent with thesample of direct values from the observed angular diameters. Theeffective temperatures are confirmed to be higher than the mean colortemperatures (from 140 to 440 K). They are in good agreement with thepublished estimates from the infrared flux method forTeff>= 3170 K, while an increasing discrepancy is observedtoward lower temperatures. As an illustration of the efficiency of thephotometric classification and effective temperature scale, the C/Oratios and the Merrill-Sanford (M-S) band intensities are investigated.It is shown that the maximum value, mean value and dispersion of C/Oincrease along the photometric CV-sequence, i.e. with decreasingeffective temperature. The M-S bands of SiC2 are shown tohave a transition from ``none'' to ``strong'' at Teff =~(2800+/- 150right ) K. Simultaneously, with decreasing effectivetemperature, the mean C/O ratio increases from 1.04 to 1.36, thetransition in SiC2 strength occurring while 1.07<= C/O<= 1.18. This research has made use of the Simbad database operatedat CDS, Strasbourg, France. Table 10 is only available in electronicform at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)}or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/369/178
| General Catalog of Galactic Carbon Stars by C. B. Stephenson. Third Edition
The catalog is an updated and revised version of Stephenson's Catalogueof Galactic Cool Carbon Stars (2nd edition). It includes 6891 entries.For each star the following information is given: equatorial (2000.0)and galactic coordinates, blue, visual and infrared magnitudes, spectralclassification, references, designations in the most significantcatalogs and coordinate precision classes. The main catalog issupplemented by remarks containing information for which there was noplace in entries of the main part, as well as some occasional notesabout the peculiarities of specific stars.
| The Chemical Composition of Carbon Stars. II. The J-Type Stars
Abundances of lithium, heavy elements, and carbon isotope ratios havebeen measured in 12 J-type Galactic carbon stars. The abundance analysisshows that in these stars the abundances of s-process elements withrespect to the metallicity are nearly normal. Tc is not present in mostof them, although upper limits have been derived for WZ Cas and WX Cyg,perhaps two SC-type rather than J-type carbon stars. The Rb abundances,obtained from the resonance λ7800 Rb I line, are surprisinglylow, probably owing to strong non-LTE effects in the formation of thisline in cool carbon-rich stars. Lithium and 13C are found tobe enhanced in all the stars. These results together with the nitrogenabundances and oxygen isotope ratios measured by Lambert et al. andHarris et al. are used to discuss the origin of J stars. The luminosityand variability class of the stars studied would indicate that they arelow-mass (M<~2-3 Msolar), less evolved objects than thenormal carbon stars, although the presence of some luminous(Mbol<-5.5) J stars in our Galaxy (WZ Cas may be anexample) and in other galaxies, suggests the existence of at least twotypes of J stars, with different formation scenarios depending upon theinitial mass of the parent star. Standard evolutionary AGB models aredifficult to reconcile with all the observed chemical characteristics.In fact, they suggest the existence of an extra mixing mechanism thattransports material from the convective envelope down to hotter regionswhere some nuclear burning occurs. This mechanism would act preferablyon the early-AGB phase in low-mass stars. Mixing at the He-core flashand the binary system hypothesis are also discussed as alternatives tothe above scenario.
| The chemical composition of the rare J-type carbon stars.
Abundances of lithium, heavy elements and carbon isotope ratios havebeen derived in 12 J-type galactic carbon stars. The abundance analysisshows that in these stars the abundances of s-process elements withrespect to the metallicity are nearly solar. Tc is not present in mostof them. The Rb abundances, obtained from the resonance 7800 {\AA} RbIline, are surprisingly low, probably due to stroong non-LTE effects.Lithium and $^{13}$C are found to be enhanced in all the stars. Theseresults are used to discuss the origin of J-stars.
| Absolute magnitudes of carbon stars from HIPPARCOS parallaxes
Hipparcos trigonometric parallaxes and photometric data for about 40bright carbon stars have been analysed. Individual absolute visual andbolometric magnitudes, normal color indices (B-V)_0, absorption valuesand distance moduli were determined. By comparison with stellarevolutionary tracks for initial mass 1<= M/M_ȯ<=4 it is foundthat the majority of CH- and R-stars are on the giant and subgiantbranches, but N-stars occupy a region -4
| Classification and Identification of IRAS Sources with Low-Resolution Spectra
IRAS low-resolution spectra were extracted for 11,224 IRAS sources.These spectra were classified into astrophysical classes, based on thepresence of emission and absorption features and on the shape of thecontinuum. Counterparts of these IRAS sources in existing optical andinfrared catalogs are identified, and their optical spectral types arelisted if they are known. The correlations between thephotospheric/optical and circumstellar/infrared classification arediscussed.
| The Spectrum Near Maximum Light of the Unusual R Coronae Borealis Variable DY Persei
DY Per was confirmed photometrically as an R CrB variable by Alksnis in1994. Spectra near maximum light show the high-speed ejection of matter(sodium at -174 km/sec in DY Per) characteristic of many of thesevariable stars. Moderate hydrogen deficiency may also be present. DY Peris remarkable in having a temperature many hundreds of degrees lowerthan most of the R CrB variables. It is unusual also in not showingclear spectroscopic evidence of high luminosit. (SECTION: Stars)
| 12C/13C ratios and Li abundances in C stars: evidence for deep mixing?
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1997MNRAS.289L..11A&db_key=AST
| Interstellar extinction and the intrinsic spectral distribution of variable carbon stars.
We present a new method of evaluation of the extinction by interstellardust on cool carbon variables. These late-type stars show no markedrelationship between spectral classification (the R, N- and C-types) andphotometric colour indices. The pair method is thus ruled out, at leastin the form currently in use for early-type or intermediate stars. Ourmethod makes use of the whole spectral energy distributions from UV toIR. A sample of 60 unreddened carbon variables is delineated and newcolour-colour diagrams are proposed where the reddening vector is nearlyperpendicular to their narrow intrinsic locus. Six photometric groups(or boxes : CV1 to 6) are derived among unreddened stars. They show acontinuous range of spectral energy distributions from "bluer" to"redder", and mean colour indices are obtained. A pair method isdescribed where each presumably reddened star is compared to these meanunreddened stars, a given extinction law being assumed. As anillustration, the results are shown for a sample of 133 well-documentedstars. The mean extinction law usually adopted for the diffuseinterstellar medium (R_V_=~3.1) is shown to provide good fits. Thethreshold for reddening detection turns to be E(B-V)=~0.02-0.03A goodcorrelation is observed when the derived colour excesses are compared tovalues from maps in the literature. The mean rate of visual extinctionamounts to =~1.25+/-1.1 , ranging from 0.37 nearl=~240° (intercloud) to 2.1 (cloud + intercloud) in two structurescorrelated with Gould's belt.
| The R Stars: Carbon Stars of a Different Kind
After $\sim$16 years of radial-velocity observations of a sample of 22R-type carbon stars, no evidence for binary motion has been detected inany of them. This is surprising considering that approximately 20\% ofnormal late-type giants are spectroscopic binaries, and the fraction isclose to 100\% in barium, CH, and subgiant/dwarf CH and barium stars. Itis suggested, therefore, that a process that has caused the mixing ofcarbon to the surface of these stars cannot act in a wide binary system.Possibly, the R stars were once all binaries, but with separations thatwould not allow them to evolve completely up the giant and asymptoticgiant branchs without coalescing. This coalescence may be the agentwhich causes carbon produced in the helium-core flash to be mixedoutwards to a region where convection zones can bring it to the surfaceof the star. (SECTION: Stars)
| A Moderate-Resolution Spectral Atlas of Carbon Stars: R, J, N, CH, and Barium Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996ApJS..105..419B&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.
| New Spectra of Carbon Stars from the IRAS Low-Resolution Spectrometer
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1994MNRAS.268..113C&db_key=AST
| A high-resolution spectral atlas of carbon stars
We present a spectral atlas of six bright carbon stars (U Hya, TX Psc,RZ Peg, V Oph, Y CVn, and UV Cam) observed with the Hamilton EchelleSpectrograph at coude using the 3 m telescope at Lick Observatory. Thesedata are of high resolution (0.13 A at 6100 A) and high signal-to-noise.The spectral range spans from 5080 to 7850 A; however, there are gapsdue to the unmatched size of the echelle format and the charge coupleddevices (CCD). We have observed a total of 87 carbon stars in the solarneighborhood over the period from 1988 May through 1991 September, withtwo or more observations for 67 stars of the sample. The reduced spectra(40 orders per observation for a total of nearly 9200 individualspectra) will be available to the scientific community via theAstrophysics Data System (ADS). The current study has produced the mostdetailed multi-epoch observations to date of a large number of carbonstars. Presented here, along with spectra of the six sample stars, areseparate template plots to be used as a tool for the ADS on-linedatabase. These templates are of atomic features, as well as (12)CN and(12)C2 transitions taken from the tables of Davis & Phillips (1963)and Phillips & Davis (1968), respectively. We have calculated bandhead positions for the isotopic species (13)C (14)N, (12)C (13)C and(13)C (13)C, whose transitions contribute significantly to the spectraof carbon stars with enhanced C-13 abundance, known as J-type carbonstars.
| A Catalog of li Abundances and Equivalent Widths in a Sample of Galactic C-Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1993A&AS..102..361B&db_key=AST
| Multi-epoch optical velocities of bright carbon stars
Cross-correlated optical radial velocities are presented of 87 brightcarbon stars, 67 with multiple epochs, as well as the velocities ofatomic transitions of K I, Li I, and Mg I. The mean optical velocityvariation is about 3 km/s for SR and Lb variables and 8.7 km/s forMiras. The spread in velocities among atomic lines at a given epoch issignificantly greater in Miras than in SR and Lb variables. Although LiI shows significant velocity variation in Miras, K I is more stable.Thirteen of 33 carbon stars with H-alpha emission also show bright Mg Iemission in a type of inverse P-Cygni profile, and each of these 13stars shows a clear splitting of the K I resonance line. Only two stars,R For and CL Mon, show K I as P-Cygni profile. J-type carbon stars havedeeper Li absorption profiles than other carbon stars in the sample.
| Stellar Maser Characteristics and Their Analysis Based on IRAS Data
Not Available
| A general catalogue of cool carbon stars
Not Available
| A flux-limited sample of Galactic carbon stars
Published observational data (including IRAS observations) for aflux-limited sample of 215 Galactic carbon stars (CSs) selected from the2-micron sky survey of Neugebauer and Leighton (1969) are compiled inextensive tables and graphs and analyzed statistically. The sample isfound to penetrate a volume of radius 1.5 kpc, and the local CS spacedensity and surface density are calculated as log rho0 (per cu kpc) =2.0 + or - 0.4 and log N (per sq kpc) = 1.6 + or - 0.2, respectively.The total Galactic mass-return rate from these CSs is estimated as 0.013solar mass/yr, implying a time scale of 0.1-1 Myr for the CSevolutionary phase and a mass of 1.2-1.6 solar mass for the (probablyF-type) main-seqence progenitors of CSs.
| Low Temperature Carbon Stars in the Vilnius Photometric System - Part Two
Not Available
| Ultraviolet spectra and chromospheres of R stars
Long-wavelength IUE spectra of 13 normal R stars and twohydrogen-deficient R0 supergiants were obtained. Early R stars are notedto have line spectra and levels of flux in the ultravioletcharacteristic of G5-K2 III stars, whereas late R stars were observed tohave colors and line spectra similar to late K and M stars, but withgreatly enhanced strength of low-lying multiplets of neutral metals.Hydrogen-deficient carbon stars show readily apparent differences fromthe normal early R stars, reflecting their luminosity and somewhathigher temperatures. The lines of neutral metals in these stars areweakened, while those of ionized metals are strengthened.
| A deep near infrared objective prism survey for carbon stars toward the galactic center and anticenter
In order to assess the problem of the asymmetric distribution of coolcarbon stars in the Milky Way for the case of a relatively faint sampleof stars, a deep, near-IR search for carbon stars has been carried outin the direction of both the galactic center and anticenter. A catalogof 283 carbon stars is presented of which 123 stars have not previouslybeen reported, and a statistical analysis of the surface and spacedistribution of the stars in the catalog indicates that the number ofcarbon stars observed toward the galactic anticenter is greater thanthat observed toward the center by a factor of 3.0. The carbon stars inthe sample appear to be concentrated at average distances from the sunof 5.5 kpc toward the galactic center, and 0.5 and 5.0 kpc toward theanticenter. Evidence is found for an increase in the population ofcarbon stars from about 2.0 kpc from the center outwards.
| Additional Identification of Variable Stars in a General Catalogue of Cool Carbon Stars
Not Available
| Photometry and Radial Velocities of Southern Carbon Stars
Not Available
| 59th Name-List of Variable Stars
Not Available
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| קבוצת-כוכבים: | נחש |
| התרוממות ימנית: | 18h19m21.82s |
| סירוב: | -15°36'46.1" |
| גודל גלוי: | 8.494 |
| מרחק: | 364.964 פארסק |
| תנועה נכונה: | 3.3 |
| תנועה נכונה: | -2.5 |
| B-T magnitude: | 11.096 |
| V-T magnitude: | 8.709 |
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