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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.
| Reprocessing the Hipparcos data of evolved stars. III. Revised Hipparcos period-luminosity relationship for galactic long-period variable stars
We analyze the K band luminosities of a sample of galactic long-periodvariables using parallaxes measured by the Hipparcos mission. Theparallaxes are in most cases re-computed from the Hipparcos IntermediateAstrometric Data using improved astrometric fits and chromaticitycorrections. The K band magnitudes are taken from the literature andfrom measurements by COBE, and are corrected for interstellar andcircumstellar extinction. The sample contains stars of several spectraltypes: M, S and C, and of several variability classes: Mira, semiregularSRa, and SRb. We find that the distribution of stars in theperiod-luminosity plane is independent of circumstellar chemistry, butthat the different variability types have different P-L distributions.Both the Mira variables and the SRb variables have reasonablywell-defined period-luminosity relationships, but with very differentslopes. The SRa variables are distributed between the two classes,suggesting that they are a mixture of Miras and SRb, rather than aseparate class of stars. New period-luminosity relationships are derivedbased on our revised Hipparcos parallaxes. The Miras show a similarperiod-luminosity relationship to that found for Large Magellanic CloudMiras by Feast et al. (\cite{Feast-1989:a}). The maximum absolute Kmagnitude of the sample is about -8.2 for both Miras and semi-regularstars, only slightly fainter than the expected AGB limit. We show thatthe stars with the longest periods (P>400 d) have high mass lossrates and are almost all Mira variables.Based on observations from the Hipparcos astrometric satellite operatedby the European Space Agency (ESA \cite{Hipparcos}).Table \ref{Tab:data1} is only available in electronic form at the CDSvia anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/403/993
| 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
| Amateur observations - Successes and opportunities.
Not Available
| Long period variable stars: galactic populations and infrared luminosity calibrations
In this paper HIPPARCOS astrometric and kinematic data are used tocalibrate both infrared luminosities and kinematical parameters of LongPeriod Variable stars (LPVs). Individual absolute K and IRAS 12 and 25luminosities of 800 LPVs are determined and made available in electronicform. The estimated mean kinematics is analyzed in terms of galacticpopulations. LPVs are found to belong to galactic populations rangingfrom the thin disk to the extended disk. An age range and a lower limitof the initial mass is given for stars of each population. A differenceof 1.3 mag in K for the upper limit of the Asymptotic Giant Branch isfound between the disk and old disk galactic populations, confirming itsdependence on the mass in the main sequence. LPVs with a thin envelopeare distinguished using the estimated mean IRAS luminosities. The levelof attraction (in the classification sense) of each group for the usualclassifying parameters of LPVs (variability and spectral types) isexamined. Table only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/374/968 or via ASTRIDdatabase (http://astrid.graal.univ-montp2.fr).
| 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.
| Mayall II = G1 in M31: A Giant Globular Cluster with an Intrinsic Metallicity Dispersion
Our HST/WFPC2 observations of G1, the brightest globular clusterbelonging to M31, provide CMDs which reach stars fainter than V = 27mag, with a well populated red horizontal branch at about V = 25.3 mag.From model fitting, we determine a rather high mean metallicity of[Fe/H] = --0.95, somewhat similar to 47 Tucanae. Artificial starexperiments provide us with an estimate of our measurement errors andsuggest the existence of a clear color spread in the cluster red giantbranch which we attribute to an intrinsic metallicity dispersion amongthe stars of G1; this may be the consequence of self enrichment duringthe early stellar/dynamical evolutionary phases of this cluster. So far,only w Centauri, the giant Galactic globular cluster, has been known toexhibit such an intrinsic metallicity dispersion. Three mass estimates(King, Virial, and King-Michie), using HST/WFPC2 surface brightnessprofile and KECK/HIRES central velocity dispersion, provide valuesbetween 7 and 17 million solar masses, indicating that G1 is more thanthree times as massive as w Centauri, the most massive Galactic globularcluster. Such large masses, with their deep potential wells, relate tothe metallicity spreads whose origin are still unknown (eitherself-enrichement, or inhomogeneous proto-cluster cloud, or remainingcore of a dwarf galaxy). Both clusters appear on the sequences (Kormendy1985) defined by globular clusters, and definitely away from the othersequences defined by elliptical galaxies, bulges, and dwarf spheroidalgalaxies. Nothing is known about the positions, in these diagrams, ofthe nuclei of nucleated dwarf elliptical galaxies. At the moment, onlythe correlation of metallicity with age observed in w Centauri suggeststhat this cluster enriched itself over a timescale of about 3 Gyr,favoring its origin as being the remaining core of a former nucleateddwarf elliptical galaxy. Massive globular clusters may simply blur theformerly clear (or simplistic) difference between globular clusters anddward galaxies.
| Mira kinematics from Hipparcos data: a Galactic bar to beyond the Solar circle
The space motions of Mira variables are derived from radial velocities,Hipparcos proper motions and a period-luminosity relation. Thepreviously known dependence of Mira kinematics on the period ofpulsation is confirmed and refined. In addition, it is found that Miraswith periods in the range 145-200d in the general Solar neighbourhoodhave a net radial outward motion from the Galactic Centre of75+/-18kms-1. This, together with a lag behind the circularvelocity of Galactic rotation of 98+/-19kms-1, is interpretedas evidence for an elongation of their orbits, with their major axesaligned at an angle of ~17° with the Sun-Galactic Centre line,towards positive Galactic longitudes. This concentration seems to be acontinuation to the Solar circle and beyond of the bar-like structure ofthe Galactic bulge, with the orbits of some local Miras probablypenetrating into the bulge. These conclusions are not sensitive to thedistance scale adopted. A further analysis is given of the short-period(SP) red group of Miras discussed in companion papers in this series. InAppendix A the mean radial velocities and other data for 842 oxygen-richMira-like variables are tabulated. These velocities were derived frompublished optical and radio observations.
| Period-Luminosity-Colour distribution and classification of Galactic oxygen-rich LPVs. I. Luminosity calibrations
The absolute K magnitudes and kinematic parameters of about 350oxygen-rich Long-Period Variable stars are calibrated, by means of anup-to-date maximum-likelihood method, using Hipparcos parallaxes andproper motions together with radial velocities and, as additional data,periods and V-K colour indices. Four groups, differing by theirkinematics and mean magnitudes, are found. For each of them, we alsoobtain the distributions of magnitude, period and de-reddened colour ofthe base population, as well as de-biased period-luminosity-colourrelations and their two-dimensional projections. The SRa semiregulars donot seem to constitute a separate class of LPVs. The SRb appear tobelong to two populations of different ages. In a PL diagram, theyconstitute two evolutionary sequences towards the Mira stage. The Mirasof the disk appear to pulsate on a lower-order mode. The slopes of theirde-biased PL and PC relations are found to be very different from theones of the Oxygen Miras of the LMC. This suggests that a significantnumber of so-called Miras of the LMC are misclassified. This alsosuggests that the Miras of the LMC do not constitute a homogeneousgroup, but include a significant proportion of metal-deficient stars,suggesting a relatively smooth star formation history. As a consequence,one may not trivially transpose the LMC period-luminosity relation fromone galaxy to the other Based on data from the Hipparcos astrometrysatellite. Appendix B is only available in electronic form at the CDSvia anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Detection of short-term variations in Mira-type variables from HIPPARCOS photometry
The Hipparcos photometric observations carried out over 37 months havebeen investigated in detail for ~ 250 Miras. This leads to an unexpectedby-product of the mission that we already suspected from ESOC real-timereductions: the first detection from space of photometric short-termbrightness variations in Mira-type variables. Altogether, 51 events in39 M-type Miras are detected and no similar variations are found for Sand C-type Miras. Their amplitude ranges from 0.23 mag up to 1.11 magand their duration extends from 2 hours up to almost 6 days. Theseevents seem to occur preferentially in late spectral types. We suggestthat they might be related to molecular opacity effects. Based on datafrom the \HIP astrometry ESA satellite
| 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.
| Mean light curves of long-period variables and discrimination between carbon- and oxygen-rich stars
Using 75 years of AAVSO data, mean light curve parameters of a sample of355 long period M, S, and C mira and semi-regular variable stars areinvestigated. We present a classification of the light curves of LPVsinto 6 distinct groups. Combining this classification with IRAS colorsmakes it possible to distinguish oxygen-rich from carbon-rich miras.Table 2 is only available in electronic form at the CDS via anonymousftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Lumnosity attenuation and distances of red giant stars
The Mv of M red variable stars is increased by the molecularTiO bands which grow from M0 to M10 in an inherent spectral darkeningsequence. The Mv is the result of both the effective visualflux and the equivalent radius. The equivalent radius is apparentlysmaller than the empirical radius due to a molecular covering process instars later than M3. The full range of optical red giant stars forms asequence from the brightest M early spectral types (S Car, M0(max),Mv approx = -3.2 mag) to the faintest M-latest spectral types(IK Tau, M10.5 min), Mv approx. = 16.5 mag). The typicalMiras and SR stars of M-medium and M-late spectral types are betweenthese two extremes. The sequence has a range of 20 mag on the visual(HR) diagram which extends from the red giant branch (RGB) passingbeyond the Mv of red dwarf stars as far as the point where itintercepts with the prolongation of the zero-age main sequence (ZAMS) inthe latest spectral type. Typical M10-stars at 200 pc has a V approx. =20 mag. M-latest stars at larger distances are unobservable stars in thevisual band. The distances of 134 variable stars are also given. Thedistances to 86 stars were determined by using a pure photometricmethod, while preliminary distances (less than 200 pc) for the remaining48 M-latest stars were determined by the spectral-photometric method.Since the local stellar density of M stars up to 100 pc rises at least7.5 times, it is possible to discuss that the long-standing problem ofdark matter in spiral galaxies could be resolved by these very dimmassive giant stars and by the molecular covered stars at the extremeend of the attenuating sequence. Furthermore, post M-latest stars may bethe only nonvisual stellar objects that can explain the enormousquantity of faint and point infrared sources found by IRAS. These weakobjects suggest the existence of an infrared Milky Way which is moredense than the optical one.
| Emission features in IRAS LRS spectra of M Mira variables
A total of 291 M Mira variables with IRAS low-resolution spectrometer(LRS) spectra that have 8-micron fluxes greater than 15 Jy have beenanalyzed. After subtraction of a 2500 K blackbody energy distributionfrom the spectrum, the remaining difference spectra can be classifiedinto seven groups, depending on the shape of their spectral emissionfeatures around 10 microns: Sil, Sil(+) Sil(2+), S, three-component,'broad', and no feature. The spectral emission features are interpretedas being produced primarily by amorphous silicates with differingamounts of crystalline olivine. A weak broad feature at 9-13 microns ispossibly produced by aluminum oxide and/or a size distribution ofsilicate particles that favors larger grains. The 8-22-micron IR excess,defined as the fraction of energy above the 2500 K continuum, shows onlya slight tendency to correlate with period and no tendency to correlatewith mass loss rate. Maser emission from OH and H2O is much morefrequently detected in stars that show the Sil or Sil(+) emissionfeature, but SiO maser emission is detected with the same percentage inall emission feature classes with the exception of the S feature. Starsshowing the S feature appear to be closely related to the MS and Sstars.
| A study of M Mira variables based on IRAS LRS observations. I - Dust formation in the circumstellar shell
A study of low-resolution IRAS spectra for a sample of 109 M Miravariables confirms the previous suggestion that stars whose spectra showthe 9.7-micron silicate emission feature have asymmetric light curves.The observed spectra are found to be well reproduced by models ofoptically thin spherical shells containing mixtures of amorphousmagnesium silicate and aluminum oxide dust particles. The broad12-micron feature observed in the spectra of stars without the9.7-micron feature is associated with aluminum oxide particles. Modelresults imply that silicate dust condenses at low temperatures far outin the circumstellar shell, suggesting that mantle growth on preexistingaluminum oxide particles is the major process responsible for silicateformation.
| IRAS low resolution spectrograph spectral class and M and S Miras
A large sample of 177 M and S Miras, as revealed by their IRAS LRSspectral class, have been examined to determine the dependence ofsilicate emission on the visual light curve asymmetry factor, f. It isconfirmed that 9.7-micron silicate emission feature not only in M but inS Miras also occurs only when f is not greater than 0.45. However, notall stars with f of not greater than 0.45 show the silicate emission;this nondetection reveals dependence on other parameters like the meanvisual light amplitude. Though strong emission feature in M Miras mayoccur for any value of f, very weak features are absent for small valuesof f, and the strongest features tend to appear for larger values of f.Infrared excess tends to increase with the strength of the silicateemission as well as with decrease in the value of f. The probability ofdetection of silicate emission is very high for the visual light curveclasses (Ludendorff, 1928) alpha 1, alpha 2, and alpha 3, decreases foralpha 4 and gamma 1, and is negligible for the beta class.
| Classification of Mira variables based on visual light curve shape
The paper presents classifications of 368 Mira variables of M, S and Cspectral classes based on the shape of their visual light curve. Theclassification is esentially based on Ludendorff's (1928) scheme and thelight curves used are mainly from the compilation of Campbell (1955).The distribution of light curves over period, mean amplitude, lightcurve asymmetry factor, period variability, and spectral class atmaximum is discussed.
| The visible spectra of Southern Hemisphere Mira variable stars
The 483 blue classification spectrograms of 72 Southern Hemisphere Miravariables presently added to the Keenan et al. (1974) catalog indicatethat the irregular behavior of absorption features in Mira variables canbe accounted for by a second shock front that lies higher in theatmosphere than the one producing Balmer emission. Since shock velocityprobably varies from cycle to cycle, the affected lines are not expectedto maintain the same equivalent width at the same phase in differentcycles.
| Valinhos 2.2 micron survey of the southern galactic plane. II - Near-IR photometry, IRAS identifications and nature of the sources
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1987A&AS...71...39E&db_key=AST
| Optical/infrared observations of RV Tauri stars.
Not Available
| IRAS catalogues and atlases - Atlas of low-resolution spectra
Plots of all 5425 spectra in the IRAS catalogue of low-resolutionspectra are presented. The catalogue contains the average spectra ofmost IRAS poiont sources with 12 micron flux densities above 10 Jy.
| UBVRI photometry of red stars
A total of 50 Mira- and SR-type red variable stars were observed bymeans of the photoelectric photometry UBVRI Kron-Cousins system. Inaddition, 15 nearby red dwarf stars having spectral subtypes similar tothose of Mira stars at maximum were observed in order to show that theconversion of the natural system into the Landolt (1983) standard systemcan be made for stars as red as the Mira variables, in spite of theshortage of standard late M-type stars. The relationship function andspectral type-color index scale on the Johnson system was converted intothe present system. By means of VRI photometry, the spectral subtype canimmediately be determined in different phases of the light curve. SRvariables have the same color indices and spectral subclasses as Miravariables.
| Spectral and luminosity variation of long-period red variable stars
In the present analysis of visual (V) apparent magnitude observationsthat were conducted with simultaneous determination of the spectral (S)subtype of long period type-Me stars (primarily Mira variables), alinear correlation is noted for each star between V and S. Since, forany moment of observation, absolute magnitude M(V) obeys a linearrelation, it is possible to conclude that the instantaneous M(V) of anygiven Mira star depends only on those physical characteristics involvingthe instantaneous spectral subtype S. The long period semiregularvariables with Me spectrum can reach the same visual absolute magnitudesas Mira variables, since they both belong to the same sequence in thetwo-color diagram (V-R, R-I).
| Valinhos 2.2 micron survey of the Southern Galactic plane Positions and infrared photometry of 338 sources
This paper reports on JHKLM photometric measurements of 338 brightinfrared stars found in a 2.2-micron survey of a 10 x 100-deg lane ofthe Southern Galactic plane. More than 2/3 of the objects are notidentified with catalogued stars and are likely to belong-period-variable or reddened giant or supergiant stars.
| Spectral classification of southern-hemisphere Mira variables
The catalog of Keenan, Garrison and Deutsch (1974) has been extended bythe addition of 483 blue spectrograms of 72 southern-hemisphere Miravariables. About 190 direct and image-tube plates at a dispersion of 120A/mm were obtained in Chile between 1977 and 1982. Along with thespectral types, emission ratios H-delta 4101/H-gamma 4340/H-beta 4861and eye-estimated intensities of the Ca I 4226, Cr I 4254 and Sr II 4077absorption lines have been tabulated. Data for the 15 best-studied Mirasin the southern-hemisphere program are presented. In addition, spectralmontages for six stars have been prepared to illustrate changes in thevisual spectra of Mira variables through their respective cycles.
| The distance of large Amplitude Red Variables
It is pointed out that the determination of the distance for LargeAmplitude Red Variables (LARV) has presented difficulties in connectionwith problems regarding the derivation of the visual absolute magnitude(Mv) of the variables. The considered investigation provides estimatesof the distance of 43 LARV on the basis of a procedure which employs anew period-spectrum-luminosity relation to obtain Mv. The accuracy ofthe estimated values is discussed. For the relatively near stars, theaccuracy is improved more than 50 percent. The error in the reportedestimates is approximately 20 percent. For stars which do not show avery pronounced intrinsic variation from cycle to cycle, there may be anerror of 15 percent regarding the estimated distance, if the Mvdispersion is plus or minus 0.3.
| Intrinsic amplitude and molecular absorption of Mira stars
Interpretation of the luminous variation of the Mira stars results in anempirical relationship demonstrating that the visual amplitude isdetermined by the maximum magnitude variation and by the variation ofthe atmospheric molecular condensation of TiO in the time intervalrequired by a star to change from minimum to maximum magnitude. Theempirical relationship accounts for intrinsic characteristics of theMira stars, such as the period-luminosity relation noted by Clayton andFeast (1969). In addition, the amplitude relationship may be applied tothe SRa stars and probably to long-period variables in general.
| Observations of SiO masers at 43 GHz with the Parkes radio telescope
A search for stellar SiO maser emission at 43 GHz is discussed for whichthe receiving equipment was arranged to detect both the v = 1, J = 1-0and the v = 2, J = 1-0 transitions simultaneously. Ten previouslyunknown SiO stars were discovered, one other was possibly detected, andall previously detected SiO masers were also observed in order todetermine how their spectra had varied as well as to obtain v = 2, J =1-0 spectra for the complete sample of known objects. It is found thatall but one of the newly discovered sources have known H2O emission, theradial velocity of the SiO emission is usually close to the H2Ovelocity, and the profiles of many of these sources apparently vary on atime scale as short as a few days. Essentially all the previously knownsources are shown to have varied, especially NML Tau, Omicron Ceti,Orion A, R Leo, VX Sgr, VY CMa, and W Hya.
| A study of Mira variables - Implications of OH stars and galactic evolution
A maximum likelihood method has been used to study the properties oftype I OH Mira variables and the kinematical evolution of the Galaxy.The method takes into account dispersion in magnitude and employs propermotions and radial velocities. The V-I excess of type I OH stars withrespect to non OH stars is confirmed, and interpreted in terms of a hot,circumstellar disk around the OH Mira variables. The results support thenotion of a gradual flattening of the Galaxy as proposed by theories ofcollisional collapse.
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Observation and Astrometry data
| Constellation: | ケンタウルス座 |
| Right ascension: | 11h55m01.31s |
| Declination: | -59°15'13.6" |
| Apparent magnitude: | 10.466 |
| Proper motion RA: | -41.3 |
| Proper motion Dec: | 2.7 |
| B-T magnitude: | 11.171 |
| V-T magnitude: | 10.525 |
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