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Binarity in Cool Asymptotic Giant Branch Stars: A GALEX Search for Ultraviolet Excesses
The search for binarity in AGB stars is of critical importance for ourunderstanding of how planetary nebulae acquire the dazzling variety ofaspherical shapes which characterizes this class. However, detectingbinary companions in such stars has been severely hampered due to theirextreme luminosities and pulsations. We have carried out a small imagingsurvey of AGB stars in ultraviolet light (using GALEX), where these coolobjects are very faint, in order to search for hotter companions. Wereport the discovery of significant far-ultraviolet excesses toward nineof these stars. The far-ultraviolet excess most likely results eitherdirectly from the presence of a hot binary companion or indirectly froma hot accretion disk around the companion.
| Proper-motion binaries in the Hipparcos catalogue. Comparison with radial velocity data
Context: .This paper is the last in a series devoted to the analysis ofthe binary content of the Hipparcos Catalogue. Aims: .Thecomparison of the proper motions constructed from positions spanning ashort (Hipparcos) or long time (Tycho-2) makes it possible to uncoverbinaries with periods of the order of or somewhat larger than the shorttime span (in this case, the 3 yr duration of the Hipparcos mission),since the unrecognised orbital motion will then add to the propermotion. Methods: .A list of candidate proper motion binaries isconstructed from a carefully designed χ2 test evaluatingthe statistical significance of the difference between the Tycho-2 andHipparcos proper motions for 103 134 stars in common between the twocatalogues (excluding components of visual systems). Since similar listsof proper-motion binaries have already been constructed, the presentpaper focuses on the evaluation of the detection efficiency ofproper-motion binaries, using different kinds of control data (mostlyradial velocities). The detection rate for entries from the NinthCatalogue of Spectroscopic Binary Orbits (S_B^9) is evaluated, as wellas for stars like barium stars, which are known to be all binaries, andfinally for spectroscopic binaries identified from radial velocity datain the Geneva-Copenhagen survey of F and G dwarfs in the solarneighbourhood. Results: .Proper motion binaries are efficientlydetected for systems with parallaxes in excess of ~20 mas, and periodsin the range 1000-30 000 d. The shortest periods in this range(1000-2000 d, i.e., once to twice the duration of the Hipparcos mission)may appear only as DMSA/G binaries (accelerated proper motion in theHipparcos Double and Multiple System Annex). Proper motion binariesdetected among S_B9 systems having periods shorter than about400 d hint at triple systems, the proper-motion binary involving acomponent with a longer orbital period. A list of 19 candidate triplesystems is provided. Binaries suspected of having low-mass(brown-dwarf-like) companions are listed as well. Among the 37 bariumstars with parallaxes larger than 5 mas, only 7 exhibit no evidence forduplicity whatsoever (be it spectroscopic or astrometric). Finally, thefraction of proper-motion binaries shows no significant variation amongthe various (regular) spectral classes, when due account is taken forthe detection biases.Full Table [see full textsee full text] 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/464/377
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| Statistical Constraints for Astrometric Binaries with Nonlinear Motion
Useful constraints on the orbits and mass ratios of astrometric binariesin the Hipparcos catalog are derived from the measured proper motiondifferences of Hipparcos and Tycho-2 (Δμ), accelerations ofproper motions (μ˙), and second derivatives of proper motions(μ̈). It is shown how, in some cases, statistical bounds can beestimated for the masses of the secondary components. Two catalogs ofastrometric binaries are generated, one of binaries with significantproper motion differences and the other of binaries with significantaccelerations of their proper motions. Mathematical relations betweenthe astrometric observables Δμ, μ˙, and μ̈ andthe orbital elements are derived in the appendices. We find a remarkabledifference between the distribution of spectral types of stars withlarge accelerations but small proper motion differences and that ofstars with large proper motion differences but insignificantaccelerations. The spectral type distribution for the former sample ofbinaries is the same as the general distribution of all stars in theHipparcos catalog, whereas the latter sample is clearly dominated bysolar-type stars, with an obvious dearth of blue stars. We point outthat the latter set includes mostly binaries with long periods (longerthan about 6 yr).
| Classification of Spectra from the Infrared Space Observatory PHT-S Database
We have classified over 1500 infrared spectra obtained with the PHT-Sspectrometer aboard the Infrared Space Observatory according to thesystem developed for the Short Wavelength Spectrometer (SWS) spectra byKraemer et al. The majority of these spectra contribute to subclassesthat are either underrepresented in the SWS spectral database or containsources that are too faint, such as M dwarfs, to have been observed byeither the SWS or the Infrared Astronomical Satellite Low ResolutionSpectrometer. There is strong overall agreement about the chemistry ofobjects observed with both instruments. Discrepancies can usually betraced to the different wavelength ranges and sensitivities of theinstruments. Finally, a large subset of the observations (~=250 spectra)exhibit a featureless, red continuum that is consistent with emissionfrom zodiacal dust and suggest directions for further analysis of thisserendipitous measurement of the zodiacal background.Based on observations with the Infrared Space Observatory (ISO), aEuropean Space Agency (ESA) project with instruments funded by ESAMember States (especially the Principle Investigator countries: France,Germany, Netherlands, and United Kingdom) and with the participation ofthe Institute of Space and Astronautical Science (ISAS) and the NationalAeronautics and Space Administration (NASA).
| Infrared Colors and Variability of Evolved Stars from COBE DIRBE Data
For a complete 12 μm flux-limited sample of 207 IRAS sources(F12>=150 Jy, |b|>=5deg), the majority ofwhich are AGB stars (~87%), we have extracted light curves in seveninfrared bands between 1.25 and 60 μm using the database of theDiffuse Infrared Background Experiment (DIRBE) instrument on the CosmicBackground Explorer (COBE) satellite. Using previous infrared surveys,we filtered these light curves to remove data points affected by nearbycompanions and obtained time-averaged flux densities and infraredcolors, as well as estimates of their variability at each wavelength. Inthe time-averaged DIRBE color-color plots, we find clear segregation ofsemiregulars, Mira variables, carbon stars, OH/IR stars, and red giantswithout circumstellar dust (i.e., V-[12]<5) and with little or novisual variation (ΔV<0.1 mag). The DIRBE 1.25-25 μm colorsbecome progressively redder and the variability in the DIRBE databaseincreases along the oxygen-rich sequence nondusty slightly varying redgiants-->SRb/Lb-->SRa-->Mira-->OH/IR and the carbon-richSRb/Lb-->Mira sequence. This supports previous assertions that theseare evolutionary sequences involving the continued production andejection of dust. The carbon stars are redder than their oxygen-richcounterparts for the same variability type, except in theF12/F25 ratio, where they are bluer. Of the 28sources in the sample not previous noted to be variable, 18 are clearlyvariable in the DIRBE data, with amplitudes of variation of ~0.9 mag at4.9 μm and ~0.6 mag at 12 μm, consistent with them being verydusty Mira-like variables. We also present individual DIRBE light curvesof a few selected stars. The DIRBE light curves of the semiregularvariable L2 Pup are particularly remarkable. The maxima at1.25, 2.2, and 3.5 μm occur 10-20 days before those at 4.9 and 12μm, and, at 4.9 and 12 μm, another maximum is seen between the twonear-infrared maxima.
| High resolution spectroscopy over lambda lambda 8500-8750 Å for GAIA. IV. Extending the cool MK stars sample
A library of high resolution spectra of MK standard and reference stars,observed in support to the GAIA mission, is presented. The aim of thispaper is to integrate the MK mapping of Paper I of this series as wellas to consider stars over a wider range of metallicities. Radialvelocities are measured for all the target stars.The spectra are available in electronic form (ASCII format) at CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/406/995 and from the webpage http://ulisse.pd.astro.it/MoreMK/, where further bibliographicalinformation for the target stars is given.
| On the Origin of Long Secondary Periods in Semiregular Variables
The presence of a long secondary period (LSP) in the light curves ofsome local semiregular variables has been known for many years.Furthermore, the LSPs have recently been found in the light curves ofapproximately 25% of the semiregular variables in the LMC. Theytypically have a length of ~500-4000 days, some 5-15 times longer thanthe primary period. Binarity, pulsation, periodic dust ejection, androtation have been suggested as the origin of the LSPs. Here we analyzeechelle spectra of a group of local semiregular variables with LSPs(hereafter LSPVs) in order to try to distinguish between thesesuggestions. In general, we find that LSPVs do not have broader spectralfeatures than semiregulars without a long secondary period (hereafternon-LSPVs). The general upper limit on the equatorial rotation velocityof 3 km s-1 rules out rotating spot and similar models. OneLSPV, V Hya, does have broader spectral lines than similar carbon stars,but it is shown here that rotation alone is not a good model forexplaining the broad lines. Mid-infrared colors of LSPs and non-LSPVsare similar and there are no LSPVs showing the large (60-25) μm IRAScolor exhibited by some R Coronae Borealis (RCB) stars. Thus, there isno evidence for periodic dust ejection from LSPVs. Finally, we find thatthe LSPVs show larger radial velocity variations than non-LSPVs, whichsuggests that LSPs are caused either by binarity or by pulsation. Asimilar conclusion was derived by Hinkle and co-workers.
| 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
| 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.
| Dust features in the 10-mu m infrared spectra of oxygen-rich evolved stars
We have analyzed the 8-13.5 mu m UKIRT CGS3 spectra of 142 M-type starsincluding 80 oxygen-rich AGB stars and 62 red supergiants, with a viewto understanding the differences and similarities between the dustfeatures of these stars. We have classified the spectra into groupsaccording to the observed appearance of the infrared features. In eachcase the normalized continuum-subtracted spectrum has been compared tothose of the other stars to find similarities and form groups. The dustfeatures of the AGB stars are classified into six groups: broad AGB,where the feature extends from 8 mu m to about 12.5 mu m with littlestructure; broad+sil AGB, which consists of a broad feature with anemerging 9.7 mu m silicate bump; and four silicate AGB groups in which a``classic'' 9.7 mu m silicate feature gets progressively narrower.Likewise, the supergiant spectra have also been classified into groups,however these do not all coincide with the AGB star groups. In thesupergiant case we again have six groups: featureless, where there islittle or no emission above the continuum; broad Super, where thefeature extends from about 9 mu m to about 13 mu m; and four silicateSuper groups, which again show a progression towards the narrowest``classic'' 9.7 mu m silicate feature. We compare the mean spectrum foreach group, which yields two main results. Firstly, while the``classic'' silicate feature is essentially identical for both AGB starsand red supergiants, the broad features observed for these two stellartypes are quite different. We suggest that the dust in these twoenvironments follows different evolutionary paths, with the dust aroundMira stars, whose broad feature spectra can be fit by a combination ofalumina (Al2O3) and magnesium silicate,progressing from this composition to dust dominated by magnesiumsilicate only, while the dust around supergiants, whose broad featurecan be fit by a combination of Ca-Al-rich silicate andAl2O3, progresses from this initial composition toone eventually also dominated by magnesium silicate. The reason for thedifference in the respective broad features is not clear as yet, butcould be influenced by lower C/O ratios and chromospheric UV radiationfields in supergiant outflow environments. The second result concernsthe 12.5 - 13.0 mu m feature discovered in IRAS LRS spectra and widelyattributed to Al2O3. This feature is seenpredominantly in the spectra of semiregular variables, sometime in Mirasand only once (so far) in supergiant spectra. We argue that it isunlikely that this feature is due to Al2O3 or, ashas more recently been suggested, spinel(MgAl2O4), but could be associated with silicondioxide or highly polymerized silicates (not pyroxenes or olivines).
| Distance Determination of Mass-Losing Stars
Based on the Principal Component Analysis on IRAS colors and the radiodata, the distances to 183 mass-losing red giant stars were determinedusing the radial velocity and Oort's galactic rotation model for azero-point calibration in the distance modulus. Also, based on therequirement of higher accuracy of the distance determination, themass-losing red giant stars were divided into two groups by means of thefirst-principal component representing an intrinsic photometric propertyof the expanding shell; then, the distances were estimated to be log{d(kpc)}=0.458 p_2+0.09+/-0.13 for group 1 and log {d(kpc)}=0.325p_2+0.45+/-0.15 for group 2, where p_2 is the principal componentcorresponding to the distance, as obtained from the IRAS flux, which wasassumed to be inversely proportional to the square of the distance.Thus,these two groups differ from each other not only by theirphotometric properties, but also by their average distances, by a factorof about 2. Systematic differences exist between the two groups in theirpopulation characteristics and in their evolutionary stages.
| The Infrared Spectral Classification of Oxygen-rich Dust Shells
This paper presents infrared spectral classifications for a flux-limitedsample of 635 optically identified oxygen-rich variables includingsupergiants and sources on the asymptotic giant branch (AGB). Severalclasses of spectra from oxygen-rich dust exist, and these can bearranged in a smoothly varying sequence of spectral shapes known as thesilicate dust sequence. Classification based on this sequence revealsseveral dependencies of the dust emission on the properties of thecentral star. Nearly all S stars show broad emission features fromalumina dust, while most of the supergiants exhibit classic featuresfrom amorphous silicate dust. Mira variables with symmetric light curvesgenerally show broad alumina emission, while those with more asymmetriclight curves show classic silicate emission. These differences may arisefrom differences in the photospheric C/O ratio.
| Circumstellar Shells of the Mass-Losing Asymptotic Giant Branch Stars: Limits for the Dust-Driven Winds
We investigated whether the radiation pressure on dust grains alone mayaccount for driving winds in semiregular, irregular and non-variable AGBstars. A simple theoretical model is employed to calculate the limitsfor the radiatively driven winds and to compare theoretical predictionswith observations. Present analysis indicates, that for most of theobjects in the studied sample of 67 oxygen-rich and 40 carbon-richmass-losing AGB stars radiation pressure on dust grains alone is noteffective enough to drive the observed circumstellar outflows.
| HIPPARCOS Astrometry of Infrared-Selected Sources and the Connection Between Optical and Infrared Reference Frames
Astrometric data from the Hipparcos satellite are reported for theoptical counterparts of 87 bright infrared sources. These sources may beuseful in defining a reference frame for infrared observations. The dataare also useful in studying the locations of circumstellar SiO masers.(SECTION: Stars)
| 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.
| A Renewed Search for Water Maser Emission from Mira Variables.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1997AJ....114.1602L&db_key=AST
| Aluminum Oxide and the Opacity of Oxygen-rich Circumstellar Dust in the 12--17 Micron Range
Amorphous alumina (Al2O3) was produced by a sol-gel technique in orderto make available its optical constants for possible astrophysicalapplications. Gradual annealing showed that the X-ray amorphousness ofalumina ended somewhere between 723 and 873 K. Above this transitionpoint, the structure changes into disordered gamma -Al2O3. At T >1273 K, crystalline alpha -Al2O3 (corundum) is formed. Mie calculationsshow that amorphous alumina exhibits a wide Al-O vibrational band,peaking at 11.5--11.8 mu m and having a steep "blue" and an extended"red" wing. It may be an important contributor to the continuous opacitybetween the silicate bands in oxygen-rich circumstellar envelopes,whereas it is ruled out for the explanation of the 13 mu m band. Anaverage 13 mu m band profile was derived from 51 IRAS low-resolutionspectra of bright Mira stars and semiregular variables. Its shape, whichis satisfactorily represented by a Lorentz profile, can be reproduced byMie calculations with the data of alpha -Al2O3, but not with those ofgamma -Al2O3. The calculations show that the 13 mu m band profile ofalpha -Al2O3 is sensitive to grain shape. If alpha -Al2O3 is theabsorber, a second band should be present at 21 mu m. A closecorrelation was found between the strengths of the 13 mu m band and the10 mu m silicate band. It suggests that the 13 mu m band carrier couldalso be somehow connected with silicate dust. Experimental argumentssupporting this attribution are presented.
| Mass-losing stars in the South Galactic CAP
Observations are presented for 162 late-type stars in the South GalacticCap (b<-30 deg) which were selected on the basisof their IRAS 25/12-μm flux ratios as high-mass-loss candidates. JHKLphotometry (over 1100 observations) was obtained for all of the stars,BV(RI)_C photometry for 78 of them and optical spectra for 51. 154 ofthese stars are non-Mira M or S stars, of which many, and possibly all,are semi-regular variables. Of the remaining eight IRAS objects, threeare T Tauri stars, three are interacting binaries and two are carbonstars. A few of the M giants and both of the carbon stars havecircumstellar envelopes of the type more normally associated with Miravariables. These include two 1612-MHz OH maser sources. It is suggestedthat such stars may have been Miras in the recent past, but arecurrently out of the instability strip owing to a recently experiencedhelium-shell flash. Alternatively, some of them could be binary stars,but there is as yet no evidence for the second star. The near-infraredcolours of the M giants are compared with those of similar stars in theBulge. They are similar to those of the inner Bulge and unlike thosefound in either the outer Bulge or the globular clusters. The kinematicsand Galactic distribution of the M giants indicate that they areprobably from a mixed population and that they could be associated withMiras with a range of periods. A comparison of the observed colours withthose derived from models indicates a range of metallicity with the bulkof stars slightly more metal-rich than the Sun. It also revealssignificant numbers of stars with colours outside the predicted range,possible due to the effects of circumstellar reddening or toinadequacies in the models. The most metal-rich examples of the M starshave high mass-loss rates for non-Miras (~10^-6 M_solar yr^-1) and thereare far fewer of them outside than inside the solar circle. This may bedue to a metallicity gradient. These stars have a scaleheight of morethan 500 pc. The two carbon stars have unusual colours and detachedshells. One of them, R Scl, is shown to vary with a period of 379dsuperimposed on a possible second period of about 2300d. The othercarbon star, which is more distant and previously unknown, may also havedouble-period variations.
| Infrared emission and dynamics of outlfows in late-type stars
The dynamical structure and infrared emission of winds around late-typestars are studied in a self-consistent model that couples the equationsof motion and radiative transfer. Thanks to its scaling properties, boththe dynamics and IR spectrum of the solution are fully characterized bytauF, the flux-averaged optical depth of the wind. Five typesof dust grains are considered: astronomical silicate, crystallineolivine, graphite, amorphous carbon and SiC, as well as mixtures.Analysis of infrared signatures provides constraints on the grainchemical composition and indications for the simultaneous existence ofsilicate and carbon grains. The abundances of crystalline olivine inSi-dominated grains and of SiC in C-dominated grains are found to belimited to less than or equal to 20%-30%. Furthermore, in carbonaceousgrains carbon is predominantly in amorphous form, rather than graphite.In mixtures, carbonaceous grains tend to dominate the dynamic behaviorwhile silicate and SiC grains dominate the IR signature. The region ofparameter space where radiation pressure can support a given mass-lossrate is identified, replacing the common misconception M nu less than orequal to L*/c, and it shows that radiatively driven windsexplain the highest mass-loss rates observed to date. A new method toderive mass-loss rates from IR data is presented, and its results agreewith other determinations. The theoretical spectra and colors are ingood agreement with observations. IRAS Low Resolution Spectrometerclasses are associated with tauF for various grain materialsand the regions of color-color diagrams expected to be populated bylate-type stars are identified. For a given grain composition, locationin the color-color diagram follows a track with position along the trackdetermined by tauF. We show that cirrus emission can severelyaffect point source measurements to the extent that their listed IRASlong-wavelength fluxes are unreliable. Whenever the listed IRAS flagcirr3 exceeds the listed 60 micrometers flux by more than a factor of 2,the 60 and 100 micrometers fluxes are no longer indicative of theunderlying point source. After accounting of cirrus contamination,essentially all IRAS point sources (95%) located in the relevant regionsof the color-color diagrams can be explained as late-type stars. Thereis no need to invoke time dependent effects, such as detached shells,for example, to explain either the colors or mass-loss rates of thesesources. Although various indications of time varying mass-loss ratesexist in numerous sources, the infrared properties of this class ofstars are well explained as a whole with steady state shows.
| Spectral evolution of the H2O maser in late-type stars
We have carried out almost simultaneous observations of H2O and SiO (J =1-0, v = 1) masers for 171 known late-type maser stars with the 34 mradio telescope at Kashima. We found a systematic change in the H2Omaser spectra related to the evolution of the stars. Typically, H2Omaser spectral profiles are singly peaked in Mira variables, but doublypeaked in IRC/AFGL objects and OH/IR stars. The expansion velocity ofH2O masers increases with decreasing IRAS color temperature. This isexplained by the shock excitation model proposed by Cooke and Elitzur(1985). The blue shifted peak in the profiles is more prominent than thered shifted peak in most of the IRC/AFGL objects and OH/IR stars. Ablocking model of the redshifted peak is introduced.
| Circumstellar dust envelopes of oxygen-rich AGB stars.
Using IRAS observational data, the best-fitting models are searched foroxygen-rich AGB stars in various evolutionary stages from opticallyvisible red giant stars to OH/IR stars with heavy mass loss. The modelinfrared spectral energy distributions of the red giant stars withcircumstellar dust envelopes are calculated with the use of a radiativetransfer code. It is found that the oxygen-rich IRAS AGB starssurrounded by circumstellar dust envelopes are divided into threegroups, which can be clearly distinguished by their mass loss rate andthe grain temperature at the inner boundary of the circumstellar dustenvelopes. One group corresponds to Mira type objects with a moderatemass loss rate and a grain formation temperature of about 500 K, thesecond to OH/IR star type objects with a large mass loss rate and a highgrain formation temperature, and the third to M stars with a very coldgrain temperature at the inner boundary, indicating that the moderatemass loss stopped a considerable time ago in these objects. The highergrain formation temperature of the OH/IR star type objects indicates agrain formation point closer to the stellar surface, suggesting aneffective acceleration of dust grains by radiation pressure. Such aneffective acceleration can play an important role in the mass lossphenomena of OH/IR stars with large mass loss rates. From the modelfitting results, it is suggested that an AGB star undergoes severaldozen phases of moderate mass loss of˙(M)~10^-7^-10^-6^Msun_/yr for a period of10^3^-10^4^years with interruptions of 10^3^-10^4^years during theordinary Mira variable phase before becoming an OH/IR star with a massloss rate exceeding 10^-5^Msun_/yr and a lifetime of about10^3^-10^4^years.
| Circumstellar CO around bright oxygen-rich semi-regulars.
We report high signal to noise millimeter wave observations of 11 nearbySemi-Regular variables, most with periods between 89 and 160 days, inthe transitions ^12^CO (J=2-1) and (J=1-0) and ^13^CO (J=2-1). The lineprofiles have been fitted by a model including molecular excitation andradiative transfer and the derived envelope properties (expansionvelocity, mass loss rate, outer radius, kinetic temperaturedistribution) are compared to the predictions of theoretical models. Themass loss properties of this sample of Semi-Regulars appear to be verysimilar with those of longer period (300<=P<400 days) Miras,observed with the same telescope. This result is consistent with theview that the Semi-Regulars are overtone pulsators while the Miras arein the fundamental pulsational mode. The pulsational mode does notstrongly affect the mass loss from the star.
| 86 GHz SiO, v=1, J=2--> 1 survey of southern IRAS point sources. II. Detection of 74 new maser sources
The detection of 74 new southern stellar SiO, v=1, J=2->1 masersassociated with IRAS point sources is reported. 57 of these were foundin an IRAS based survey of oxygen rich stellar envelopes. The detectionrate in this survey was 45%. 17 further new maser sources were detectedduring a search for strong pointing sources for the Swedish-ESOSubmillimeter Telescope (SEST). The distribution of the IRAS lowresolution spectral (LRS) classes of all the SiO masers (this paper andliterature) peaks sharply at class 15. The distribution of the LRSclasses of the maser sources from 21 to 29 is similar to thedistribution of these classes of all the point sources in the pointsource catalogue except for class 25. Only few maser sources of thisspectral class are known. This is possibly explained by a selectioneffect.
| A search for variability in the IRAS-LRS spectra of long period variables
Time-averaged IRAS-low resolution spectrometer (LRS) spectra have beenextensively used in the past for the study of mass loss in cool stars.Using the GEISHA system available at Groningen, we have extracted theraw LRS data for a sample of 40 mass losing asymptotic giant branch(AGB) stars. The selection was made on the basis of the number ofindividual spectra obtained by IRAS, the flux at 12 micrometers, an LRSclassification of 2n or 4n and a known association with an optical longperiod variable (Miras, Semiregulars). The spectra were analyzed inthree different ways, one of them being similar to the original LRSclassification scheme. Using spectra taken within 24 hours we estimatedthe internal accuracy of a single spectrum as a function of the 12micrometer flux. The spectra were then searched for variability in thesilicate and SiC dust features. Only one possible case of variabilitywas found. The results are discussed in terms of the pulsational andmass loss characteristics of our sample and other observational data oncircumstellar dust features.
| Circumstellar shells resolved in the IRAS survey data. I - Data processing procedure, results, and confidence tests
We have examined the IRAS 60 and 100 micron survey data covering 512evolved stars and young planetary nebulae for evidence of spatiallyresolved structure. A simple model, consisting of a central unresolvedsource surrounded by a resolved isothermal shell, was fitted to the datafor each star. Seventy-six stars were found to be resolved in the 60micron data. Tests have been performed to verify that the extendedstructure seen is not an artifact of the data-processing algorithm.
| The dynamics of stellar outflows dominated by interaction of dust and radiation
Wind outflow around a late-type star driven by radiation pressure ondust grains is investigated in detail. The equation of motion for theoutflow coupled with the equation of radiative transfer is solvedtreating the circumstellar envelope, which consists of gas and dust, asa two-component fluid. Because of the drift of the dust particlesthrough the gas, the dust-to-gas ratio varies with distance even ifgrain formation is a prompt process. The coupling between dust and gasweakens as the mass-loss rate decreases until finally the rate ofmomentum transfer to the gas is insufficient to overcome gravity whenthe mass-loss rate is too low. This results in a lower limit, on theorder of 10 exp -7 solar mass/yr, to the possible mass-loss rates thatcan be driven by radiation pressure on dust. Radiative transferconsiderations pose a bound on the capability of the radiation field toovercome gravity also in the opposite limit of large mass-loss rates.Due to the difference in optical properties between carbon stars andoxygen stars, these considerations produce a meaningful upper limit onthe mass-loss rate, of several times 10 exp -4 solar mass/yr, only forcarbon stars.
| Circumstellar shells resolved in IRAS survey data. II - Analysis
IRAS survey data for 512 red giant stars and young planetary nebulaewere processed using a computer program which fitted the data to anidealized model of a circumstellar shell. Seventy-six of these starswere found to have circumstellar shells resolved in the 60-micron surveydata. Forty pct of the 76 stars are carbon stars. Thirteen are Miravariables. The evolution of these shells, involving the interaction ofthe expelled material with the ISM, is modeled, and the results suggestthat the period during which Mira variables lose mass lasts forapproximately 10 exp 5 yr. Carbon stars are found to shed mass for about2 x 10 exp 5 yr. The expansion velocity of the outer shell for thelargest shells will normally be lower by a factor of 3-5 than theexpansion velocity obtained from CO observations.
| CO and HCN observations of circumstellar envelopes. A catalogue - Mass loss rates and distributions
We have searched the literature for all observations of the (C-12)O(1-0), (C-12)O (2-1), and HCN (1-0) lines in circumstellar envelopes oflate type stars published between January 1985 and September 1992. Wereport data for 1361 observations (stellar velocity, expansion velocity,peak intensity, integrated area, noise level). This CO-HCN sample nowcontains 444 sources; 184 are identified as O-rich, 205 as C-rich, andthere are 9 S stars. About 85 percent of the sources are AGB stars.There are 32 planetary nebulae and about thirty post-AGB starscandidates. Besides results of mm-observations, we also listidentifications, coordinates, IRAS data, and chemical and spectral typesfor every source. For AGB stars, we have estimated (or compiled)bolometric fluxes and distances for 349 sources, and mass loss ratesdeduced from CO results for 324 sources, taking into account theinfluence of the CO photodissociation radius. We also list mass lossrates derived from detailed models of CO emission in the literature.
| Oxygen-rich semiregular and irregular variables
All the known oxygen-rich semiregulars and irregulars of spectralclasses K and M with the absolute value of B not greater than 30 deg,Delta(m) not less than 0.5 mag, and, for the semiregulars, periods inthe range of 50 to 400 d are compiled. On the basis of theirdistributions on the sky and their brightnesses in the K band at 2.2microns, it is argued that the semiregulars with a period of 300-400 dappear to belong to the same population as the 'thin disk' Miras in thesame period range and have an exponential scale height from the Galacticplane of about 250 pc. The semiregulars with a period range of 200 to300 d belong to the population of the 'thick disk' Miras with anexponential scale height from the Galactic plane of about 500 pc. On thebasis of the similarities of their space distributions and the presenceof Tc in their atmospheres, and using the pulsational mode calculationsby Ostlie and Cox (1986), it is suggested that the semiregulars with aperiod range of 100-150 d are first and second overtone pulsations ofthe same population of AGB stars as the Miras in their fundamentalpulsational mode with periods longer than 300 d.
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Besorolás csoportokba:
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Pozíciós és asztrometriai adatok
| Csillagkép: | Eridánusz |
| Rektaszcenzió: | 04h04m18.80s |
| Deklináció: | -15°43'30.5" |
| Vizuális fényesség: | 8.597 |
| Távolság: | 219.298 parszek |
| RA sajátmozgás: | -0.6 |
| Dec sajátmozgás: | -16.9 |
| B-T magnitude: | 10.379 |
| V-T magnitude: | 8.745 |
Katalógusok és elnevezések:
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