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Random forest automated supervised classification of Hipparcos periodic variable stars
We present an evaluation of the performance of an automatedclassification of the Hipparcos periodic variable stars into 26 types.The sub-sample with the most reliable variability types available in theliterature is used to train supervised algorithms to characterize thetype dependencies on a number of attributes. The most useful attributesevaluated with the random forest methodology include, in decreasingorder of importance, the period, the amplitude, the V-I colour index,the absolute magnitude, the residual around the folded light-curvemodel, the magnitude distribution skewness and the amplitude of thesecond harmonic of the Fourier series model relative to that of thefundamental frequency. Random forests and a multi-stage scheme involvingBayesian network and Gaussian mixture methods lead to statisticallyequivalent results. In standard 10-fold cross-validation (CV)experiments, the rate of correct classification is between 90 and 100per cent, depending on the variability type. The main mis-classificationcases, up to a rate of about 10 per cent, arise due to confusion betweenSPB and ACV blue variables and between eclipsing binaries, ellipsoidalvariables and other variability types. Our training set and thepredicted types for the other Hipparcos periodic stars are availableonline.
| The evolutionary state of Miras with changing pulsation periods
Context. Miras are long-period variables thought to be in the asymptoticgiant branch (AGB) phase of evolution. In about one percent of knownMiras, the pulsation period is changing. It has been speculated thatthis changing period is the consequence of a recent thermal pulse inthese stars. Aims: We aim to clarify the evolutionary state ofthese stars, and to determine in particular whether or not they are inthe thermally-pulsing (TP-)AGB phase. Methods: One importantpiece of information that has been neglected so far when determining theevolutionary state is the presence of the radio-active s-process elementtechnetium (Tc). We obtained high-resolution, high signal-to-noise-ratiooptical spectra of a dozen prominent Mira variables with changingpulsation period to search for this indicator of TPs and dredge-up. Wealso use the spectra to measure lithium (Li) abundances. Furthermore, weestablish the evolutionary states of our sample stars by means of theirpresent-day periods and luminosities. Results: Among the twelvesample stars observed in this programme, five were found to showabsorption lines of Tc. BH Cru is found to be acarbon-star, its period increase in the past decades possibly havingstopped by now. We report a possible switch in the pulsation mode ofT UMi from Mira-like to semi-regular variability inthe past two years. R Nor, on the other hand, isprobably a fairly massive AGB star, which could be true for allmeandering Miras. Finally, we assign RU Vul to themetal-poor thick disk with properties very similar to the short-period,metal-poor Miras. Conclusions: We conclude that there is no clearcorrelation between period change class and Tc presence. The stars thatare most likely to have experienced a recent TP are BH Cru andR Hya, although their rates of period change arequite different.Based on observations made with the Mercator Telescope, operated on theisland of La Palma by the Flemish Community, at the Spanish Observatoriodel Roque de los Muchachos of the Instituto de Astrofísica deCanarias, and with the Swiss 1.2 m Euler telescope at La Silla, Chile.The spectra are only available at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/531/A88
| AKARI's infrared view on nearby stars. Using AKARI infrared camera all-sky survey, 2MASS, and Hipparcos catalogs
Context. The AKARI, a Japanese infrared space mission, has performed anAll-Sky Survey in six infrared-bands from 9 to 180 ?m with higherspatial resolutions and better sensitivities than IRAS. Aims: Weinvestigate the mid-infrared (9 and 18 ?m) point source catalog (PSC)obtained with the infrared camera (IRC) onboard AKARI, in order tounderstand the infrared nature of the known objects and to identifypreviously unknown objects. Methods: Color-color diagramsand a color-magnitude diagram were plotted with the AKARI-IRC PSCand other available all-sky survey catalogs. We combined the Hipparcosastrometric catalog and the 2MASS all-sky survey catalog with theAKARI-IRC PSC. We furthermore searched literature and SIMBADastronomical database for object types, spectral types, and luminosityclasses. We identified the locations of representative stars and objectson the color-magnitude and color-color diagram schemes. Theproperties of unclassified sources can be inferred from their locationson these diagrams. Results: We found that the (B-V) vs.(V-S9W) color-color diagram is useful for identifying thestars with infrared excess emerged from circumstellar envelopes ordisks. Be stars with infrared excess are separated well from other typesof stars in this diagram. Whereas (J-L18W) vs. (S9W-L18W)diagram is a powerful tool for classifying several object types.Carbon-rich asymptotic giant branch (AGB) stars and OH/IR stars formdistinct sequences in this color-color diagram. Young stellarobjects (YSOs), pre-main sequence (PMS) stars, post-AGB stars, andplanetary nebulae (PNe) have the largest mid-infrared color excess andcan be identified in the infrared catalog. Finally, we plot the L18W vs.(S9W-L18W) color-magnitude diagram, using the AKARI data togetherwith Hipparcos parallaxes. This diagram can be used to identify low-massYSOs and AGB stars. We found that this diagram is comparable to the [24]vs. ([8.0]-[24]) diagram of Large Magellanic Cloud sources usingthe Spitzer Space Telescope data. Our understanding of Galactic objectswill be used to interpret color-magnitude diagram of stellar populationsin the nearby galaxies that Spitzer Space Telescope observed. Conclusions: Our study of the AKARI color-color andcolor-magnitude diagrams will be used to explore properties ofunknown objects in the future. In addition, our analysis highlights afuture key project to understand stellar evolution with a circumstellarenvelope, once the forthcoming astronometrical data with GAIA areavailable.Catalog (full Tables 3 and 4) are only available in electronic form atthe CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/514/A2
| BH Crucis: Period, Magnitude, and Color Changes
The period changes of the dual maxima Mira star BH Cru and theassociated color changes are discussed. UBV measures before the changein period began are compared with those after the star had stabilized atthe new, longer, period and those made during the twelve cycles oflengthening period are summarized. A 30% increase in mean V brightnessis noted, as is a distinctly redder color in B-V. The apparentsingle maximum that has now appeared can be explained by a relativebrightening of the second maximum with the first maximum now somewhathidden by it.
| Near-infrared spectroscopy of AGB star candidates in Fornax, Sculptor, and NGC 6822
Context: The asymptotic giant branch (AGB) phase is characterised bysubstantial mass loss that is accompanied by the formation of dust. Inextreme cases this will make the star no longer visible in the optical.For a better understanding of AGB evolution it is important to identifyand characterise these very red AGB stars. Aims: The first aim ofthis article is to improve the census of red AGB stars in three LocalGroup galaxies, based on near-IR spectroscopic observations of newcandidates with red 2MASS (J-K) colours. The opportunity is taken tocompare the near-IR spectra with those of Milky Way stars. Methods: We used ISAAC on the ESO VLT to take J and H-band spectra of36 targets in Fornax, Sculptor and NGC 6822. Results: Twelve newC-stars are found in Fornax, and one is confirmed in Sculptor. AllC-stars have (J-K) > 1.6, and are brighter than -3.55 in bolometricmagnitude. Ten new oxygen-rich late-type giant stars are identified inFornax, but none is extremely red or very luminous. Five luminous O-richAGB stars are identified in NGC 6822, of which 3 show water absorption,indicative of spectral type M. Again, none is as red as Milky Way OH/IRstars, but in this galaxy the list of candidate AGB stars is biasedagainst very red objects. In some C-stars with (J-K)>2 an extremelystrong 1.53 μm absorption band is found. These stars are probably allMira variables and the feature is related to the low temperature, highdensity chemistry that is a first step towards dust formation and massloss.Based on observations collected at the European Southern Observatory,Paranal, Chile (ESO programme 75.D-0152).Figure 6 is only available in electronic form via http://www.aanda.org
| Infrared photometry and evolution of mass-losing AGB stars. II. Luminosity and colors of MS and S stars
Context: Asymptotic giant branch (AGB) phases mark the end of theevolution for low- and intermediate-mass stars. Our understanding of themechanisms through which they eject the envelope and our assessment oftheir contribution to the mass return to the interstellar medium and tothe chemical evolution of Galaxies are hampered by poor knowledge oftheir luminosities and mass loss rates, both for C-rich and for O-richsources. Aims: We plan to establish criteria permitting a morequantitative determination of luminosities (and subsequently of massloss rates) for the various types of AGB stars on the basis of infraredfluxes. In this paper, in particular, we concentrate on O-rich ands-element-rich MS, S stars and include a small sample of SC stars. Methods: We reanalyze the absolute bolometric magnitudes and colors ofMS, S, SC stars on the basis of a sample of intrinsic (single) andextrinsic (binary) long period variables. We derive bolometriccorrections as a function of near- and mid-infrared colors, adopting asreferences a group of stars for which the spectral energy distributioncould be reconstructed in detail over a large wavelength range. Wedetermine the absolute HR diagrams, and compare luminosities and colorsof S-type giants with those, previously derived, of C-rich AGB stars.Luminosity estimates are also verified on the basis of existingperiod-luminosity relations valid for O-rich Miras. Results: S starbolometric luminosities are almost indistinguishable from those ofC-rich AGB stars. On the contrary, their circumstellar envelopes arethinner and less opaque. Despite this last property the IR wavelengthsremain dominant, with the bluest stars having their maximum emission inthe H or K(short) bands. Near-to-mid infrared color differences are inany case smaller than for C stars. Based on period-luminosity relationsfor O-rich Miras and on Magnitude-color relations for the same variableswe show how approximate distances (hence intrinsic parameters) forsources of so far unknown parallax can be inferred. We argue that mostof the sources have a rather small mass (<2 Mȯ);dredge-up might then be not effective enough to let the C/O ratio exceedunity.Tables [see full textsee full textsee full textsee full textsee fulltextsee full text]-[see full textsee full textsee full textsee fulltextsee full textsee full text] are only available in electronic form athttp://www.aanda.org Tables 11 and 12 are 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/488/675
| Period Change in the Semiregular Variable RU Vulpeculae
The well-observed semiregular variable RU Vulpeculae has undergone asubstantial change in period over the past fifty-five years. Thediscovery period of ~155 days has undergone a continuous change to itscurrent value of 108 days. The amplitude and stability of the lightcurve have changed as well; the pulsations are much less regular andhave a lower amplitude now than at the time of RUVul's discovery and classification. The character ofthe period change is quantitatively similar to that of the well-studiedMira variable T Ursae Minoris, and we argue that RU Vul may be asemiregular analog of Mira variables undergoing dramatic period changes.We place RU Vul in the context of other AGB stars exhibiting similarbehavior, and discuss possible explanations for its period change.
| AGB variables and the Mira period-luminosity relation
Published data for large-amplitude asymptotic giant branch variables inthe Large Magellanic Cloud (LMC) are re-analysed to establish theconstants for an infrared (K) period-luminosity relation of the formMK = ρ[logP - 2.38] + δ. A slope of ρ = -3.51+/- 0.20 and a zero-point of δ = -7.15 +/- 0.06 are found foroxygen-rich Miras (if a distance modulus of 18.39 +/- 0.05 is used forthe LMC). Assuming this slope is applicable to Galactic Miras we discussthe zero-point for these stars using the revised Hipparcos parallaxestogether with published very long baseline interferometry (VLBI)parallaxes for OH masers and Miras in globular clusters. These result ina mean zero-point of δ = -7.25 +/- 0.07 for O-rich Galactic Miras.The zero-point for Miras in the Galactic bulge is not significantlydifferent from this value.Carbon-rich stars are also discussed and provide results that areconsistent with the above numbers, but with higher uncertainties. Withinthe uncertainties there is no evidence for a significant differencebetween the period-luminosity relation zero-points for systems withdifferent metallicity.
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| Near-infrared photometry of carbon stars
Near-infrared, JHKL, photometry of 239 Galactic C-rich variable stars ispresented and discussed. From these and published data, the stars wereclassified as Mira or non-Mira variables, and amplitudes and pulsationperiods, ranging from 222 to 948 d for the Miras, were determined formost of them. A comparison of the colour and period relations with thoseof similar stars in the Large Magellanic Cloud indicates minordifferences, which may be the consequence of sample selection effects.Apparent bolometric magnitudes were determined by combining the meanJHKL fluxes with mid-infrared photometry from IRAS and MSX. Then, usingthe Mira period luminosity relation to set the absolute magnitudes,distances were determined - to greater accuracy than has hitherto beenpossible for this type of star. Bolometric corrections to the Kmagnitude were calculated and prescriptions derived for calculatingthese from various colours. Mass-loss rates were also calculated andcompared to values in the literature.Approximately one-third of the C-rich Miras and an unknown fraction ofthe non-Miras exhibit apparently random obscuration events that arereminiscent of the phenomena exhibited by the hydrogen-deficient RCoronae Borealis stars. The underlying cause of this is unclear, but itmay be that mass loss, and consequently dust formation, is very easilytriggered from these very extended atmospheres.Based on observations made at the South African AstronomicalObservatory.E-mail: paw@saao.ac.za
| T UMi Keeps Mysterious
The well known long-period variable T UMi of Mira type has ranked amongthe most observed stars becouse of its strange behaviour. 25 years ago,the rapid decrease of period started - from original 301d long period totodays 200 - 220 days. Such behaviour can be explained as He-burning inshell surrounding the stelar nucleus. Author presents his CCD multicolorphotometry of T UMi as well.
| A Unique Dust Formation Episode in the SC-Type Star UY Centauri
We report the first detection of new dust formation in an SC star. Theprototype of the SC stars, UY Cen, underwent a decline of 2 mag in the Vband. The SC stars show pulsational variations and have 60 μmexcesses, indicating past dust formation. It has been suggested that asa star evolves from being oxygen rich to carbon rich, there is a shortperiod of time when C/O~1 during which the star appearsspectroscopically as an SC star and ceases to produce dust. The SC starBH Cru has shown large spectroscopic and pulsation period variationsover only 30 yr, indicating rapid evolution, but it has shown no sign ofnew dust formation. UY Cen has not shown any pulsation or spectroscopicvariations accompanying the onset of its dust formation. In addition, UYCen did not show emission in the resonance lines of Na I, K I, or Rb Iwhen it was at its faintest, although these lines were a feature of thecarbon stars R Lep and V Hya during similar faint phases.
| Secular Evolution in Mira Variable Pulsations
Stellar evolution theory predicts that asymptotic giant branch (AGB)stars undergo a series of short thermal pulses that significantly changetheir luminosity and mass on timescales of hundreds to thousands ofyears. These pulses are confirmed observationally by the existence ofthe short-lived radioisotope technetium in the spectra of some of thesestars, but other observational consequences of thermal pulses are subtleand may only be detected over many years of observations. Secularchanges in these stars resulting from thermal pulses can be detected asmeasurable changes in period if the star is undergoing Mira pulsations.It is known that a small fraction of Mira variables exhibit largesecular period changes, and the detection of these changes among alarger sample of stars could therefore be useful in evolutionary studiesof these stars. The American Association of Variable Star Observers(AAVSO) International Database currently contains visual data for over1500 Mira variables. Light curves for these stars span nearly a centuryin some cases, making it possible to study the secular evolution of thepulsation behavior on these timescales. In this paper we present theresults of our study of period change in 547 Mira variables using datafrom the AAVSO. We use wavelet analysis to measure the period changes inindividual Mira stars over the span of available data. By making linearfits to the period versus time measurements, we determine the averagerates of period change, dlnP/dt, for each of these stars. We findnonzero dlnP/dt at the 2 σ significance level in 57 of the 547stars, at the 3 σ level in 21 stars, and at the level of 6 σor greater in eight stars. The latter eight stars have been previouslynoted in the literature, and our derived rates of period change largelyagree with published values. The largest and most statisticallysignificant dlnP/dt are consistent with the rates of period changeexpected during thermal pulses on the AGB. A number of other starsexhibit nonmonotonic period change on decades-long timescales, the causeof which is not yet known. In the majority of stars, the periodvariations are smaller than our detection threshold, meaning theavailable data are not sufficient to unambiguously measure slowevolutionary changes in the pulsation period. It is unlikely that morestars with large period changes will be found among heretoforewell-observed Mira stars in the short term, but continued monitoring ofthese and other Mira stars may reveal new and serendipitous candidatesin the future.
| Carbon Stars in the Infrared Telescope in Space Survey
We have identified 139 cool carbon stars in the near-infraredspectrophotometric survey of the Infrared Telescope in Space (IRTS) fromthe conspicuous presence of molecular absorption bands at 1.8, 3.1, and3.8 μm. Among them, 14 are new bright (K~4.0-7.0) carbon stars. Wefind a trend relating the 3.1 μm band strength to the K-L'color index, which is known to correlate with mass-loss rate. This couldbe an effect of a relation between the depth of the 3.1 μm featureand the degree of development of the extended stellar atmosphere wheredust starts to form.
| Period and chemical evolution of SC stars
The SC and CS stars are thermal-pulsing asymptotic giant branch starswith a C/O ratio close to unity. Within this small group, the Miravariable BH Cru recently evolved from spectral type SC (showing ZrObands) to CS (showing weak C2). Wavelet analysis shows thatthe spectral evolution was accompanied by a dramatic period increase,from 420 to 540 d, indicating an expanding radius. The pulsationamplitude also increased. Old photographic plates are used to establishthat the period before 1940 was around 490 d. Chemical models indicatethat the spectral changes were caused by a decrease in stellartemperature, related to the increasing radius. There is no evidence fora change in C/O ratio. The evolution in BH Cru is unlikely to be relatedto an ongoing thermal pulse. Periods of the other SC and CS stars,including nine new periods, are determined. A second SC star, LX Cyg,also shows evidence for a large increase in period, and one further starshows a period inconsistent with a previous determination. Mira periodsmay be intrinsically unstable for C/O ~ 1; possibly because of afeedback between the molecular opacities, pulsation amplitude, andperiod. LRS spectra of 6 SC stars suggest a feature at λ > 15μm, which resembles one recently attributed to the iron-sulphidetroilite. Chemical models predict a large abundance of FeS in SC stars,in agreement with the proposed association.
| 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
| The modelling of intermediate-age stellar populations. II. Average spectra for upper AGB stars, and their use
The upper Asymptotic Giant Branch (AGB) is populated with oxygen richand carbon rich Long Period Variables (LPVs). These stars are essentialcontributors to the near-IR light of intermediate age stellarpopulations. Individual observed spectra of LPVs are so diverse thatthey cannot be used directly in the synthesis of galaxy spectra. In thispaper, the library of individual spectra of Lançon & Wood(\cite{LM00_fluct}) is used to construct averages that can beincorporated conveniently in population synthesis work. The connectionbetween such spectra and stellar evolution tracks is discussed. In orderto select a sorting criterion and to define averaging bins for the LPVspectra, correlations between their spectrophotometric properties arereexamined. While optical properties and broad baseline colours such as(I-K) are well correlated, a large dispersion is observed when theseindices are plotted against near-IR ones. This is partly due to theintrinsic width of the upper AGB, which is illustrated by locating eachof the multiple observations of individual LPVs on the HR diagram. It isargued that broad baseline colour-temperatures are the most sensiblesorting criteria. The properties of the resulting sequence of averagespectra indeed vary regularly. We further address: (i) the bolometriccorrections and temperature scales needed to associate a spectrum with agiven point on a theoretical stellar evolution track (or isochrone),(ii) the simplifying assumptions that will be implicitely made whenusing the average spectra, (iii) potential biases in the sample ofLançon & Wood and their effects, (iv) the small contributionof LPVs to the interstellar hydrogen emission lines in galaxies. It isemphasized that an a posteriori calibration of the effective temperaturescale remains necessary, until consistent models for the evolution, thepulsation and the spectral appearance of LPVs become available. Wesuggest a recipe for the use of the average spectra at variousmetallicities.
| The evolution of the Mira variable R Hydrae
The Mira variable R Hydrae is well known for its declining period, whichWood & Zarro attributed to a possible recent thermal pulse. Here weinvestigate the long-term period evolution, covering 340 years, goingback to its discovery in AD 1662. The data include photometricmonitoring by amateur and other astronomers over the last century, andrecorded dates of maximum for earlier times. Wavelets are used todetermine both the period and the semi-amplitude. We show that theperiod decreased linearly between 1770 and 1950; since 1950 the periodhas stabilized at 385d. The semi-amplitude is shown to follow the periodevolution closely. Analysis of the oldest data shows that before 1770the period was about 495d. We find no evidence for an increasing periodduring this time as found by Wood & Zarro. We discuss the mass-losshistory of R Hya: the IRAS data show that the mass loss droppeddramatically around AD 1750. The evolution of the mass loss as functionof period agrees with the mass-loss formalism from Vassiliadis &Wood; it is much larger than predicted by the Blöcker law. An outerdetached IRAS shell suggests that R Hya has experienced mass-lossinterruptions before. The period evolution can be explained by twomodels: a thermal pulse occurring around AD 1600, or a non-linearinstability leading to an internal relaxation of the stellar structure.The elapsed time between the mass-loss decline giving rise to the outerdetached shell and the recent event, of approximately 5000yr, suggeststhat only one of these events could be due to a thermal pulse. Furthermonitoring of R Hya is recommended, as both models make strongpredictions for the future period evolution. We argue that R Hya-typeevents could provide part of the explanation for the rings seen aroundsome asymptotic giant branch (AGB) and post-AGB stars. Changes in Miraproperties were already known on a cycle-to-cycle basis, and on thethermal pulse time-scale of ~104yr. R Hya shows thatsignificant evolution can also occur on intermediate time-scales of theorder of 102-103yr.
| 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
| Period Evolution in Mira Variables
We investigate a number of Mira variables which show evolution in theirperiods. Three different types of period changes are found: continuouschanges, sudden changes, and meandering periods. On the order of 1% ofMiras show evidence for period changes, but unstable periods may becommon among the longest period Miras. The case of R Hya is studied inmore detail, using archived data from AAVSO, AFOEV, BAAVSS, RASNZ, andVSOLJ, and historical records: we find that its period evolved fromalmost 500 days around its discovery (AD 1662) to about 385 days sinceAD 1950. The period change was accompanied by a dramatic change in itsmass-loss rate. Such changes in mass-loss rates, especially for theMiras with meandering periods, could be one of the causes of the ringsseen around many descendents of Mira variables, the planetary nebulae.
| 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.
| Spectra of carbon-rich asymptotic giant branch stars between 0.5 and 2.5 mu m: Theory meets observation
We present a hydrostatic analysis of five carbon rich stars, BH Cru, TCae, S Cen, RU Pup and Y Hya in the wavelength range between 0.5 and 2.5mu m. All except BH Cru, which is a Mira star, show only modestvariability. We identify the absorption features of the molecules CO, CNand C2. The overall energy distribution, which is verysensitive to the effective temperature in the investigated wavelengthrange, as well as the bands of these molecules put strict limits on thepossible values of effective temperature and C/O. We show that our modelatmospheres and corresponding synthetic spectra are able to reproducethe observed spectra quite accurately from about 0.7 to 2.5 mu m. Thediscrepancies are mainly due to uncertainties in the molecular inputdata. We discuss briefly why the variations of the molecular featuresare small and why dynamic phenomena do not play a very important role inthis wavelength range. We identify colour indices based on commonlyavailable filters and potentially suitable for the empiricaldetermination of fundamental parameters of carbon stars.
| Stars with the Largest Hipparcos Photometric Amplitudes
A list of the 2027 stars that have the largest photometric amplitudes inHipparcos Photometry shows that most variable stars are all Miras. Thepercentage of variable types change as a function of amplitude. Thiscompilation should also be of value to photometrists looking forrelatively unstudied, but large amplitude stars.
| Infrared colours for Mira-like long-period variables found in the (Mȯ<~10-7 Msolar yr-1) Hipparcos Catalogue
Near-infrared, JHKL, photometry is presented for 193 Mira andsemi-regular variables that were observed by Hipparcos; periods,bolometric magnitudes and amplitudes are derived for 92 of them. Becauseof the way in which the Hipparcos targets were selected, this group ofstars provides a useful data base of Miras with low mass-loss rates(Mȯ<~10-7Msolaryr-1).Various period-colour relationships are discussed in detail. The colour,particularly BCK = 10.86 - 38.10 K (J - K)0 +64.16(J - K)20 - 50.72(J -K)30 + 19, K-L, at a given period is found todepend on the pulsation amplitude of the star. A comparison with modelssuggests that this is a consequence of atmospheric extension, in thesense that large-amplitude pulsators have very extended atmospheres andredder Mȯ<10-7Msolaryr-1, K-L and H-K but bluerJ-H than their lower amplitude counterparts. The stars with veryextended atmospheres also have higher values of K-[12] and hence highermass-loss rates. This finding provides further evidence for the causalconnection between pulsation and mass loss. Two sequences are identifiedin the Hp-K versus logP diagram (where Hp is the Hipparcos broad-bandmagnitude) at short periods (logP<2.35). At a given period these twogroups have, on average, the same pulsation amplitude, but differentJHKL colours and spectral types. The short-period stars in the bluersequence have similar near-infrared colours to the Miras found inglobular clusters. Long-term trends in the infrared light curves arediscussed for stars that have sufficient data.
| A library of 0.5 to 2.5 mu m spectra of luminous cool stars
We present a library of 0.5-2.5 mu m digital spectra of cool, mostlyvariable, giant and supergiant stars which should be useful for spectralsynthesis applications, as well as for comparison with theoretical modelatmosphere calculations. The library includes carbon stars, GalacticBulge and Magellanic Cloud stars, and OH/IR stars. The stars observedcover a range of metallicities and masses. Most variable objects wereobserved several times, at different phases of their pulsation cycle. Wediscuss the effects of various fundamental parameters and of variabilityon the spectra. Based on period-luminosity relations and stellarevolutionary tracks, we tentatively assign initial masses to eachobject.
| 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)
| The Henize sample of S stars. II. Data
This paper presents data collected on the Henize sample of 205 S stars:(i) CORAVEL radial-velocity data; (ii) photometric data in the UBV bandsof the Geneva photometric system; (iii) photometric data in the JHKLbands of the SAAO photometric system; (iv) IRAS fluxes; (v)low-resolution spectra of 158 S stars. Close visual companions have beenfound for Hen 47, 94, 105 and 155. Spectroscopic orbital elements areprovided for Hen 2, 108, 121, 137 and 147. The analysis of these data ispresented in a companion paper. Based on observations carried out at theEuropean Southern Observatory (ESO, La Silla, Chile), at the 70~cm Swisstelescope at ESO and at the South African Astronomical Observatory.
| The Variability of R, N, and C Stars from HIPPARCOS and AAVSO Data
Not Available
| Optical and near-infrared spectrophotometric properties of Long Period Variables and other luminous red stars
Based on a new and large sample of optical and near-infrared spectraobtained at the Mount Stromlo and Siding Spring Observatories(Lançon & Wood 1998; Lançon & Wood, inpreparation), spectrophotometric properties of cool oxygen- andcarbon-rich Long Period Variables and supergiants are presented.Temperatures of oxygen-rich stars are assigned by comparison withsynthetic spectra computed from up-to-date oxygen-rich model atmospheregrids. The existence of reliable optical and near-infrared temperatureindicators is investigated. A narrow relation between the bolometriccorrection BC_I and the broad-band colour I-J is obtained foroxygen-rich cool stars. The ability of specific near-infrared indices toseparate luminosity classes, atmospheric chemistry or variabilitysubtypes is discussed. Some comments are also given on extinctioneffects, water band strengths in Long Period Variables and theevaluation of \element[][12]{CO}/\element[][13]{CO} ratio in red giants.
| "Real-time" evolution in Mira variables.
After a brief review of our current understanding of Miras and theirevolutionary status, three aspects of ``real-time'' evolution in theseand related stars are examined: # Chemical changes (O-rich to C-rich)due to third dredge-up # Period changes due to the effects of thehelium-shell flash # The existence of ``fossil'' dust and gas shells.Studies of resolved gas and dust shells are highlighted as particularlyinteresting. They will enable us to examine the mass-loss histories ofmany late-type stars over the last ten thousand years or so. Suchobservations have only recently become technically feasible and they areexpected to provide important new insights into the late stages ofstellar evolution.
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