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Публикации по объекту
Infrared Spectroscopy of Symbiotic Stars. V. First Orbits for Three S-Type Systems: Henize 2-173, CL Scorpii, and AS 270
Infrared radial velocities have been used to compute first orbits of theM giants in three southern S-type symbiotic systems. Of the three, Hen2-173 has the longest orbital period, 911 days, and also has anoncircular orbit with an eccentricity of 0.21. The large value of itsmass function suggests that Hen 2-173 may be an eclipsing system. For CLSco our spectroscopic orbital period of 626 days is essentiallyidentical to the previously determined light variability period of 625days, and we have adopted the latter. AS 270 has an orbital period ofsimilar length, 671 days, and both CL Sco and AS 270 have circularorbits. Only CL Sco has been extensively investigated previously, and wecompare our results with the conclusions of Kenyon & Webbink. Wealso have examined the period-eccentricity relation for 30 S-typesymbiotics. Circular orbits are found for 81% of the systems withorbital periods up to 800 days, while they occur for only 22% withperiods greater than 800 days. This distribution is quite unlike thatfor G and K giants; rather, it is similar to that for barium stars,another type of mass-transfer binary, which also consists of a late-typegiant and a white dwarf companion.
| Two Micron All Sky Survey, Infrared Astronomical Satellite, and Midcourse Space Experiment Color Properties of Intrinsic and Extrinsic S Stars
We attempt to select new candidate intrinsic and extrinsic S stars inthe General Catalogue of Galactic S Stars (GCGSS) by combining data fromthe Two Micron All Sky Survey, the Infrared Astronomical Satellite, andthe Midcourse Space Experiment. Catalog entries are cross-identified,yielding 528 objects, out of which 29 are known extrinsic S stars and 31are known intrinsic S stars. Their color-color diagrams,(H-[12])-(K-[12]) and (K-[12])-(J-[25]), are drawn and used to identifya new sample of 147 extrinsic and 256 intrinsic S star candidates, whilethe nature of 65 stars remains identified. We infer that about 38%+/-10%of the GCGSS objects are of extrinsic type. Moreover, we think thatcolors such as J-[25] can be used to split off the two categories of Sstars, while single colors are not appropriate. The color-colordiagrams, such as (H-[12])-(K-[12]) and (K-[12])-(J-[25]), are proven tobe powerful tools for distinguishing the two kinds of S stars.
| UBV(RI)C photometric sequences for symbiotic stars. III
We present accurate UBV(RI)C photometric sequences andastrometric positions for a final set of 41 symbiotic stars. In asimilar manner to the 40 targets of Papers I and II, these sequencesextend over wide brightness and color ranges and are suited to coveringboth quiescence and outburst phases. They are intended to assist boththe CCD photometric monitoring of current variability and exploitationof old photographic plates from historical archives.
| A catalogue of eclipsing variables
A new catalogue of 6330 eclipsing variable stars is presented. Thecatalogue was developed from the General Catalogue of Variable Stars(GCVS) and its textual remarks by including recently publishedinformation about classification of 843 systems and making correspondingcorrections of GCVS data. The catalogue1 represents thelargest list of eclipsing binaries classified from observations.
| An abundance analysis of the symbiotic star CH Cygni
The photospheric abundances for the cool component of the symbiotic starwere calculated for the first time using high-resolution near-infraredspectra and the method of of standard LTE analysis and atmosphericmodels. The iron abundance for CH Cyg was found to besolar, [Fe/H] = 0.0 ± 0.19. The atmospheric parameters (T_eff =3100 K, log g = 0.0 (cgs), ξt = 2.2 km s-1) andmetallicity for CH Cyg are found to be approximately equal to those fornearby field M7 giants. The calculated [C/H] = -0.15, [N/H] = +0.16,[O/H] = -0.07, and the isotopic ratios of 12C/13Cand 16O/17O are close to the mean values forsingle M giants that have experienced the first dredge-up. A reasonableexplanation for the absence of barium star-like chemical peculiaritiesseems to be the high metallicity of CH Cyg. The emission line techniquewas explored for estimating CNO ratios in the wind of the giant.
| An Abundance Analysis of Two S Stars at High Galactic Latitude
We present abundances of Ti, Fe, and Ni as well as 10 post-iron-peakelements in two Galactic S stars, S UMa and Stephenson 1303. Based uponthe presence or absence of Tc in their spectra, S UMa is an intrinsic Sstar and Stephenson 1303 is an extrinsic S star. Both stars are slightlymetal-poor and at high Galactic latitude; they thus make an interestingcomparison as well as a further test of current models ofnucleosynthesis in low-mass stars. In addition, the abundance ratio ofheavy to light s-process elements, [hs/ls], correlates with themetallicities of Stephenson 1303 and S UMa as expected if the13C neutron source drives the s-process.
| Symbiotic Stars as Laboratories for the Study of Accretion and Jets: A Call for Optical Monitoring
Symbiotic binary stars typically consist of a white dwarf (WD) thataccretes material from the wind of a companion red giant. Orbitalperiods for these binaries are on the order of years, and theirrelatively small optical outbursts tend to occur every few years todecades. In some symbiotics, material that is transferred from the redgiant to the WD forms a disk around the WD. Thus, symbiotic stars are abit like overgrown cataclysmic variables (CVs), but with less violenteruptions. Symbiotic stars are not as well understood as CVs, in partbecause their longer variability time scales mean that observations overmany years are required to cover different outburst states and orbitalphases. The recent discovery of collimated outflows ("jets") from anumber of symbiotics provides a new motivation for such long-term studyof these objects. Astrophysical jets are observed in almost every typeof accretion-powered system, and symbiotic stars may help us understandthese structures. Optical monitoring by amateurs can identify systemsin outburst, and also help to build a comprehensive database of outburstand quiescent symbiotic light curves. Together with radio through X-rayobservations that will be performed when new outbursts are found,long-term optical light curves will improve understanding of symbioticoutbursts, jet production, and the connection between outbursts, jets,and accretion disks in symbiotic stars.
| Abundances of Post-Iron-Peak Elements in HD 35155: A Symbiotic Star of Spectral Type S
We present abundances of Ti, Fe, and Ni as well as 10 post-iron-peakelements in the extrinsic, Galactic S star HD 35155. This star is ofinterest because it shows many characteristics of symbiotic stars anddisplays the same pattern of abundance enhancements observed in yellowsymbiotic stars. It is clear that HD 35155 is associated with thesymbiotic stars and provides an important link between the symbioticphenomena and chemically peculiar stars. In addition, the abundanceratio of heavy to light s-process elements correlates with themetallicity of HD 35155, as is expected if the 13C neutronsource drives the s-process. Our models predict that the abundance oflead should be enhanced by a factor of between 50 to 500 in HD 35155.
| 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
| Zirconium to Titanium Ratios in a Large Sample of Galactic S Stars
The [Zr/Ti] ratio for a large sample of Galactic S stars has beendetermined using high-quality, high-resolution spectra. The pattern ofZr enhancements in intrinsic and extrinsic S stars is found to differ,and the [Zr/Ti] ratio in the extrinsic S stars clearly links them to thestrong barium stars. In addition, the pattern of [Zr/Ti] ratios seems toindicate that the progression of spectral type M to MS to S to SC is duelargely to an increase in the abundance of s-process elements and notsolely to a changing C/O ratio as claimed by some investigators (such asScalo and Ross).
| The Henize sample of S stars. IV. New symbiotic stars
The properties of the few symbiotic stars detected among the 66 binary Sstars from the Henize sample are discussed. Two stars (Hen 18 and Hen121) exhibit both a strong blue-violet continuum and strongHalpha emission (FWHM of 70 km s-1), whereas Hen134 and 137 exhibit weak Halpha emission. TheHalpha profiles are typical of non-dusty symbiotic starsbelonging to class S-3 as defined by Van Winckel et al. (1993, A&AS102, 401). In that class as in the Henize symbiotic S stars, He I, [NII] or [S II] emission lines are absent, suggesting that the nebulardensity is high but the excitation rather low. The radial velocity ofthe centre of the Halpha emission is identical to that of thecompanion star (at least for Hen 121 where this can be checked from theavailable orbital elements), thus suggesting that the Halphaemission originates in gas moving with the companion star. For Hen 121,this is further confirmed by the disappearance of the ultraviolet Balmercontinuum when the companion is eclipsed by the S star. Hen 121 is thusthe second eclipsing binary star discovered among extrinsic S stars (thefirst one is HD 35155). A comparison of the available data on orbitalperiods and Halpha emission leads to the conclusion thatHalpha emission in s stars seems to be restricted to binarysystems with periods in the range 600-1000 d, in agreement with thesituation prevailing for red symbiotic stars (excluding symbioticnovae). Symbiotic S stars are found among the most evolved extrinsic Sstars. Based on observations carried out at the European SouthernObservatory (ESO, La Silla, Chile; program 60.E-0805) and at the Swiss70 cm telescope (La Silla, Chile).
| Near-infrared observations of candidate extrinsic S stars
Photometric observations in the near infrared for 161 S stars, including18 Tc-rich (intrinsic) stars, 19 Tc-deficient (extrinsic) ones and 124candidates for Tc-deficient S stars, are presented in this paper. Basedon some further investigations into the infrared properties of bothTc-rich and Tc-deficient S stars, 104 candidates are identified as verylikely Tc-deficient S stars. The large number of infrared-selectedTc-deficient S stars provides a convenient way to study the physicalproperties and the evolutionary status of this species of S stars.
| Nucleosynthesis and Mixing on the Asymptotic Giant Branch. III. Predicted and Observed s-Process Abundances
We present the results of s-process nucleosynthesis calculations forasymptotic giant branch (AGB) stars of different metallicities anddifferent initial stellar masses (1.5 and 3 Msolar), and wepresent comparisons of them with observational constraints fromhigh-resolution spectroscopy of evolved stars over a wide metallicityrange. The computations were based on previously published stellarevolutionary models that account for the third dredge-up phenomenonoccurring late on the AGB. Neutron production is driven by the13C(α,n)16O reaction during the interpulseperiods in a tiny layer in radiative equilibrium at the top of the He-and C-rich shell. The neutron source 13C is manufacturedlocally by proton captures on the abundant 12C; a few protonsare assumed to penetrate from the convective envelope into the radiativelayer at any third dredge-up episode, when a chemical discontinuity isestablished between the convective envelope and the He- and C-richzones. A weaker neutron release is also guaranteed by the marginalactivation of the reaction 22Ne(α,n)25Mgduring the convective thermal pulses. Owing to the lack of a consistentmodel for 13C formation, the abundance of 13Cburnt per cycle is allowed to vary as a free parameter over a wideinterval (a factor of 50). The s-enriched material is subsequently mixedwith the envelope by the third dredge-up, and the envelope compositionis computed after each thermal pulse. We follow the changes in thephotospheric abundance of the Ba-peak elements (heavy s [hs]) and thatof the Zr-peak ones (light s [ls]), whose logarithmic ratio [hs/ls] hasoften been adopted as an indicator of the s-process efficiency (e.g., ofthe neutron exposure). Our model predictions for this parameter show acomplex trend versus metallicity. Especially noteworthy is theprediction that the flow along the s-path at low metallicities drainsthe Zr and Ba peaks and builds an excess at the doubly magic208Pb, which is at the termination of the s-path. We thendiscuss the effects on the models of variations in the crucialparameters of the 13C pocket, finding that they are notcritical for interpreting the results. The theoretical predictions arecompared with published abundances of s-elements for AGB giants ofclasses MS, S, SC, post-AGB supergiants, and for various classes ofbinary stars, which supposedly derive their composition by mass transferfrom an AGB companion. This is done for objects belonging both to theGalactic disk and to the halo. The observations in general confirm thecomplex dependence of neutron captures on metallicity. They suggest thata moderate spread exists in the abundance of 13C that isburnt in different stars. Although additional observations are needed,it seems that a good understanding has been achieved of s-processoperation in AGB stars. Finally, the detailed abundance distributionincluding the light elements (CNO) of a few s-enriched stars atdifferent metallicities are examined and satisfactorily reproduced bymodel envelope compositions.
| A catalogue of symbiotic stars
We present a new catalogue of symbiotic stars. In our list we include188 symbiotic stars as well as 30 objects suspected of being symbiotic.For each star, we present basic observational material: coordinates, Vand K magnitudes, ultraviolet (UV), infrared (IR), X-ray and radioobservations. We also list the spectral type of the cool component, themaximum ionization potential observed, references to finding charts,spectra, classifications and recent papers discussing the physicalparameters and nature of each object. Moreover, we present the orbitalphotometric ephemerides and orbital elements of known symbioticbinaries, pulsational periods for symbiotic Miras, Hipparcos parallaxesand information about outbursts and flickering.
| The Henize sample of S stars --- III. Uncovering the binary intruders
The properties of S stars are investigated thanks to a large observingprogram devoted to the well-defined Henize sample (205 S stars south ofδ = -25̂ and brighter than R = 10.5, covering allgalactic latitudes), in order to derive the respective properties of theintrinsic S stars (genuine thermally-pulsing AGB stars) and of theextrinsic S stars (post mass-transfer binaries). The stellar sample isfirst cleaned from a few stars misclassified as S thanks to UBV Genevaphotometry and low-resolution spectroscopy. These low-resolution spectraalso allow to successfully distinguish subclasses within the S starfamily. Dedicated Geneva photometry and high-resolution spectroscopyhave led to the discovery of two symbiotic S stars. The more stringentdifference between extrinsic and intrinsic stars is their technetiumcontent, but several other observational parameters are shown to beefficient to some extent in segregating intrinsic S stars from theirextrinsic masqueraders (UBV , JHKL and IRAS photometry, radial-velocitystandard deviation, shape of the CORAVEL cross-correlation dip,combination of band strength indices derived from low-resolutionspectra). Multivariate classification has been performed on the Henizedata sample in order to guarantee a classification as objective aspossible and handling at the same time a large number of parameters. Theresulting clusters separate efficiently extrinsic and intrinsic S stars,allowing to derive the respective properties of these two distinctstellar classes. The population difference between intrinsic andextrinsic S stars is for the first time clearly demonstrated, sinceintrinsic S stars are far more concentrated towards the galactic planethan extrinsic S stars (zint = 200 ∓ 100 pc andzext = 600 ∓ 100 pc), and are therefore believed tobelong to a younger, more massive population. The frequency of extrinsicand intrinsic S stars in the magnitude-limited Henize sample amounts to33% and 67%, respectively. In a volume-limited sample, this proportionis subject to large uncertainties mainly because of uncertainluminosities. There are probably as many as 40% extrinsic stars among Sstars in a volume-limited sample. Based on observations carried out atthe European Southern Observatory (ESO, La Silla, Chile) and at theSwiss 70 cm telescope (La Silla, Chile)
| A homogeneous study of the s-process in the 21 mu m carbon-rich post-AGB objects
We present in this paper a homogeneous photospheric abundance study, onthe basis of the analysis of high resolution optical spectra, of sixpost-AGB objects displaying a 21mu m, circumstellar dust feature intheir IR spectrum. The F-G spectral type of the 21mu m, stars make thata large range of elements including a wide variety of s-processelements, can be studied by their atomic lines. The high C/O-ratiostogether with the large overabundance of s-process elements prove thatthe objects are descendants of field carbon stars. We discuss in detailthe s-process abundance distribution displayed by these 21mu m, starsand conclude that the 3rd dredge-up efficiency is closely related to thestrength of the integrated neutron irradiation. The expectedanti-correlation of the neutron irradiation with metallicity, on theother hand, contains a large intrinsic scatter. Finally we compare ourresults with other intrinsic and extrinsic s-process enriched objectsand conclude that the post-AGB stars offer very useful complementarydata to constrain the evolutionary models of AGB nucleosynthesis anddredge-up processes. based on observations collected at the EuropeanSouthern Observatory in Chile (61.E-0426), and at Roque de los Muchachosat La Palma Spain
| Speckle Interferometry of New and Problem HIPPARCOS Binaries
The ESA Hipparcos satellite made measurements of over 12,000 doublestars and discovered 3406 new systems. In addition to these, 4706entries in the Hipparcos Catalogue correspond to double star solutionsthat did not provide the classical parameters of separation and positionangle (rho,theta) but were the so-called problem stars, flagged ``G,''``O,'' ``V,'' or ``X'' (field H59 of the main catalog). An additionalsubset of 6981 entries were treated as single objects but classified byHipparcos as ``suspected nonsingle'' (flag ``S'' in field H61), thusyielding a total of 11,687 ``problem stars.'' Of the many ground-basedtechniques for the study of double stars, probably the one with thegreatest potential for exploration of these new and problem Hipparcosbinaries is speckle interferometry. Results are presented from aninspection of 848 new and problem Hipparcos binaries, using botharchival and new speckle observations obtained with the USNO and CHARAspeckle cameras.
| JHK photometry of symbiotic stars
We present the results of multi-epoch JHK photometry of a sample of 30known or suspected symbiotics and related objects. These are the firstresults of an ongoing programme of near-IR monitoring of symbiotic starsfrom the Mt. Abu IR Observatory of Physical Research Laboratory (PRL).
| Heavy-element abundances in seven SC stars and several related stars
We employ spectra of resolution 20-35,000 of seven SC stars, four Sstars, two Ba stars, and two K-M stars to derive abundances of a varietyof elements from Sr to Eu relative to iron. Special attention is paid toRb and Tc, and to the ratio of the heavy s-process species to the lights-process elements. Abundances are derived in LTE, both by using modelatmospheres in which the carbon and oxygen abundances are nearly equaland by using curves of growth. Spectrum synthesis is used for criticallines, such as the 5924-A line of Tc and the 7800-A line of Rb. For mostof the heavy-element stars, the enhancement of the s-process elements isabout a factor of 10. The ratio of the heavy to light s-process speciesis not far from solar, except for RR Her, for which the same ratio is +0.45 dex. For Tc the blending by other lines is severe. While we haveprobably detected the 5924-A line, we can only present abundances in theless-than-or-equal-to category.
| On the Variability of S Stars as Observed by the Hipparcos
The Hipparcos photometry of S type stars shows that they are allvariable. The intrinsic S stars show a larger range of amplitudes thando the extrinsic S stars.
| Spectra of Cool Stars in the J Band (1.0-1.3 μm) at Medium Resolution
A spectroscopic survey of 103 cool S-, C-, and M-type stars wasundertaken with the Kitt Peak cryogenic spectrograph on the 1.3 mtelescope to make a detailed search for new molecular bands in the1.0-1.3 μm J-band region. While the spectra have high signal-to-noiseratios and good repeatability, no strong new features were found. Higherresolution spectra of a small sample of representative stars observedwith the 4 m Fourier transform spectrometer were invoked in order toidentify the features in these spectra. With few exceptions, the detailsof these spectra are well understood. Laboratory spectra were obtainedto aid in the identification of some weak features. Spectral featuresfrom dominant lines of Ti, Fe, Al, Si, Mn, Na, and K, and molecularbands due to TiO, TiS, ZrO, ZrS, VO, H_2O, and CN, have been identifiedin the spectra. Several weak unidentified bands are found.
| A CORAVEL radial-velocity monitoring of S stars: Symbiotic activity vs. orbital separation. III.
Orbital elements are presented for the Tc-poor S stars HR 363 (= HD7351) and HD 191226. With an orbital period of 4592 d (=12.6 y), HR 363has the longest period known among S stars, and yet it is a strong X-raysource. Its X-ray flux is similar to that of HD 35155, an S star withone of the shortest orbital periods (640 d). This surprising result isput in perspective with other diagnostics of binary interaction observedin binary S stars. They reveal that there is no correlation between thelevel of binary interaction and the orbital period. All these activitydiagnostics moreover exhibit a strong time-variability. In thewell-documented case of HR 1105, this time-variability appears to be acombination of orbital modulation and secular variation. A stream of gasfrom the red-giant wind, which is heated when funneled through the innerLagrangian point, has been proposed as the source of the hard photons\cite[(Shcherbakov & Tuominen 1992).]{S} Different viewing angles ofthe stream during the orbital cycle account for the orbital modulation,whereas long-term fluctuations of the mass-loss rate account for thesecular variations. Little dependence to the orbital separation isexpected for this kind of activity. If such streams are causing theactivity observed in the other binary S stars as well, it would providea natural explanation for the absence of correlation between orbitalperiods and activity levels, since the red-giant mass loss rate would bethe dominant factor. The existence of such funneled streams is moreoverpredicted by smooth particle hydrodynamics simulations of mass transferin detached binary systems. Based on observations performed with theSwiss telescope at the Haute-Provence Observatory, France.
| A CORAVEL radial-velocity monitoring of giant BA and S stars: Spectroscopic orbits and intrinsic variations. I.
With the aim of deriving the binary frequency among Ba and S stars, 56new spectroscopic orbits (46 and 10, respectively) have been derived forthese chemically-peculiar red giants monitored with the \coravel\spectrometers. These orbits are presented in this paper (38 orbits) andin a companion paper \cite[(Udry et al. 1998,]{Udry} Paper II; 18orbits). The results for 12 additional long-period binary stars (6 and6, respectively), for which only minimum periods (generally exceeding 10y) can be derived, are also presented here (10) and in Paper II (2). Theglobal analysis of this material, with a few supplementary orbits fromthe literature, is presented in \cite[Jorissen et al.(1998).]{Jorissen98} For the subsample of Mira S, SC and (Tc-poor) Cstars showing intrinsic radial-velocity variations due to atmosphericphenomena, orbital solutions (when available) have been retained if thevelocity and photometric periods are different (3 stars). However, it isemphasized that these orbit determinations are still tentative. Threestars have been found with radial-velocity variations synchronous withthe light variations. Pseudo-orbital solutions have been derived forthose stars. In the case of RZ Peg, a line-doubling phenomenon isobserved near maximum light, and probably reflects the shock wavepropagating through the photosphere. Based on observations obtained atthe Haute-Provence Observatory (France) and at the European SouthernObservatory (ESO, La Silla, Chile).
| CO observations and mass loss of MS- and S-stars
We present (12) CO J = 1-0 and 2-1 observations of 14 S-stars, andreport 6 new detections. Two stars were observed in the (13) CO J = 1-0and 2-1 lines, and one tentative 2-1 detection is reported. Acompilation is presented of all CO observations of S-stars. The stars inthis sample are separated into ``intrinsic'' and ``extrinsic'' S-stars,based on direct observation of the Technetium line, or infraredproperties. The dust mass loss rate per unit distance is derived fromIRAS 60 mu m data taking into the fact that for small mass loss ratesthe observed flux is an overestimate of the excess emission due to dust.The gas mass loss rate per unit distance is derived from CO data.Distances and luminosities are estimated, partly from hipparcos parallaxdata. The largest mass loss rate derived is that for W Aql with(0.8-2.0) x 10(-5) {Msun} yr(-1) , and the lowest is that foro Ori with <1.2 x 10(-9) {Msun} yr(-1) . The S-starswithout Tc have smaller mass loss rates, than those with Tc. Diagramsshowing mass loss rate, dust-to-gas ratio and expansion velocity versuspulsation period are presented, and compared to similar data for carbon-and oxygen-rich Miras. The S-Miras stand not out in any way from the C-or O-Miras in these diagrams. In the diagram with expansion velocityversus pulsation period, the S-SRs span the same range in velocity asthe S-Miras, but they have periods which are about a factor of 2.5shorter. This was previously noted for O-rich SRs. As in that case, themost straightforward explanantion is that the SRs among the S-starspulsate in a higher order pulsation mode. Based on data from the ESAhipparcos astrometry satellite.
| BVRI photometry of the extrinsic S star HR 1105
BVRI photometry of the extrinsic S star HR 1105 shows a stable periodiclight variability with a period of 24.76 days superimposed upon longterm changes presumably related to the orbital period. The variationsare in phase for all four magnitudes with the amplitude of thisvariability being about the same for B and V, but smaller for R and evensmaller for I. As the primary is a M3 III star, these brightness changesare mostly likely due to the pulsation of the primary star. Table 1 isonly available in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Infrared study of the two categories of S stars
Photometric observations of 20 Tc-deficient and 24 Tc-rich S stars inthe near infrared are presented in this paper. With the IRAS data,infrared two color diagrams, IRAS low-resolution spectra and energydistributions are discussed to summarize the way to segregate Tc-richstars from Tc-deficient ones.
| Insights into the formation of barium and Tc-poor S stars from an extended sample of orbital elements
The set of orbital elements available for chemically-peculiar red giant(PRG) stars has been considerably enlarged thanks to a decade-longCORAVEL radial-velocity monitoring of about 70 barium stars and 50 Sstars. When account is made for the detection biases, the observedbinary frequency among strong barium stars, mild barium stars andTc-poor S stars (respectively 35/37, 34/40 and 24/28) is compatible withthe hypothesis that they are all members of binary systems. Thesimilarity between the orbital-period, eccentricity and mass-functiondistributions of Tc-poor S stars and barium stars confirms that Tc-poorS stars are the cooler analogs of barium stars. A comparative analysisof the orbital elements of the various families of PRG stars, and of asample of chemically-normal, binary giants in open clusters, revealsseveral interesting features. The eccentricity - period diagram of PRGstars clearly bears the signature of dissipative processes associatedwith mass transfer, since the maximum eccentricity observed at a givenorbital period is much smaller than in the comparison sample of normalgiants. be held The mass function distribution is compatible with theunseen companion being a white dwarf (WD). This lends support to thescenario of formation of the PRG star by accretion of heavy-element-richmatter transferred from the former asymptotic giant branch progenitor ofthe current WD. Assuming that the WD companion has a mass in the range0.60+/-0.04 Msb ȯ, the masses of mild and strong barium starsamount to 1.9+/-0.2 and 1.5+/-0.2 Msb ȯ, respectively. Mild bariumstars are not restricted to long-period systems, contrarily to what isexpected if the smaller accretion efficiency in wider systems were thedominant factor controlling the pollution level of the PRG star. Theseresults suggest that the difference between mild and strong barium starsis mainly one of galactic population rather than of orbital separation,in agreement with their respective kinematical properties. There areindications that metallicity may be the parameter blurring the period -Ba-anomaly correlation: at a given orbital period, increasing levels ofheavy-element overabundances are found in mild barium stars, strongbarium stars, and Pop.II CH stars, corresponding to a sequence ofincreasingly older, i.e., more metal-deficient, populations. PRG starsthus seem to be produced more efficiently in low-metallicitypopulations. Conversely, normal giants in barium-like binary systems mayexist in more metal-rich populations. HD 160538 (DR Dra) may be such anexample, and its very existence indicates at least that binarity is nota sufficient condition to produce a PRG star. This paper is dedicated tothe memory of Antoine Duquennoy, who contributed many among theobservations used in this study
| The HIPPARCOS Hertzsprung-Russell diagram of S stars: probing nucleosynthesis and dredge-up
HIPPARCOS trigonometrical parallaxes make it possible to compare thelocation of Tc-rich and Tc-poor S stars in the Hertzsprung-Russell (HR)diagram: Tc-rich S stars are found to be cooler and intrinsicallybrighter than Tc-poor S stars. The comparison with the Genevaevolutionary tracks reveals that the line marking the onset of thermalpulses on the asymptotic giant branch (AGB) matches well the observedlimit between Tc-poor and Tc-rich S stars. Tc-rich S stars are, asexpected, identified with thermally-pulsing AGB stars of low andintermediate masses, whereas Tc-poor S stars comprise mostly low-massstars (with the exception of 57 Peg) located either on the red giantbranch or on the early AGB. Like barium stars, Tc-poor S stars are knownto belong exclusively to binary systems, and their location in the HRdiagram is consistent with the average mass of 1.6+/-0.2 Msb ȯderived from their orbital mass-function distribution (Jorissen et al.1997, A&A, submitted). A comparison with the S stars identified inthe Magellanic Clouds and in the Fornax dwarf elliptical galaxy revealsthat they have luminosities similar to the galactic Tc-rich S stars.However, most of the surveys of S stars in the external systems did notreach the lower luminosities at which galactic Tc-poor S stars arefound. The deep Westerlund survey of carbon stars in the SMC uncovered afamily of faint carbon stars that may be the analogues of thelow-luminosity, galactic Tc-poor S stars. Based on data from theHIPPARCOS astrometry satellite
| BVRI photometry of the S star HD 35155
Johnson BV and Cousins RI differential photometric observations of theeclipsing S star HD 35155 are reported. The four light curves are inphase. There is some evidence that the light curves are not perfectlyrepeatable with phase.
| 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.
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| Прямое восхождение: | 05h22m18.65s |
| Склонение: | -08°39'58.0" |
| Видимая звёздная величина: | 6.894 |
| Расстояние: | 757.576 парсек |
| Собственное движение RA: | 48.3 |
| Собственное движение Dec: | -4.2 |
| B-T magnitude: | 9.186 |
| V-T magnitude: | 7.084 |
Каталоги и обозначения:
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