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Variability in red supergiant stars: pulsations, long secondary periods and convection noise
We study the brightness variations of galactic red supergiant starsusing long-term visual light curves collected by the AmericanAssociation of Variable Star Observers over the last century. The fullsample contains 48 red semiregular or irregular variable stars, with amean time-span of observations of 61 yr. We determine periods and periodvariability from analyses of power density spectra and time-frequencydistributions. We find two significant periods in 18 stars. Most ofthese periods fall into two distinct groups, ranging from a few hundredto a few thousand days. Theoretical models imply fundamental, first andpossibly second overtone mode pulsations for the shorter periods.Periods greater than 1000 d form a parallel period-luminosity relationthat is similar to the long secondary periods of the asymptotic giantbranch stars. A number of individual power spectra shows a single moderesolved into multiple peaks under a Lorentzian envelope, which weinterpret as evidence for stochastic oscillations, presumably caused bythe interplay of convection and pulsations. We find a strong 1/f noisecomponent in the power spectra that is remarkably similar in almost allstars of the sample. This behaviour fits the picture of irregularphotometric variability caused by large convection cells, analogous tothe granulation background seen in the Sun.
| The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not As Cool As We Thought
We use moderate-resolution optical spectrophotometry and the new MARCSstellar atmosphere models to determine the effective temperatures of 74Galactic red supergiants (RSGs). The stars are mostly members of OBassociations or clusters with known distances, allowing a criticalcomparison with modern stellar evolutionary tracks. We find we canachieve excellent matches between the observations and the reddenedmodel fluxes and molecular transitions, although the atomic lines Ca Iλ4226 and Ca II H and K are found to be unrealistically strong inthe models. Our new effective temperature scale is significantly warmerthan those in the literature, with the differences amounting to 400 Kfor the latest type M supergiants (i.e., M5 I). We show that the newlyderived temperatures and bolometric corrections give much betteragreement with stellar evolutionary tracks. This agreement provides acompletely independent verification of our new temperature scale. Thecombination of effective temperature and bolometric luminosities allowsus to calculate stellar radii; the coolest and most luminous stars (KWSgr, Case 75, KY Cyg, HD 206936=μ Cep) have radii of roughly 1500Rsolar (7 AU), in excellent accordance with the largeststellar radii predicted from current evolutionary theory, althoughsmaller than that found by others for the binary VV Cep and for thepeculiar star VY CMa. We find that similar results are obtained for theeffective temperatures and bolometric luminosities using only thedereddened V-K colors, providing a powerful demonstration of theself-consistency of the MARCS models.
| 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).
| Guilt by Association: The 13 Micron Dust Emission Feature and Its Correlation to Other Gas and Dust Features
A study of all full-scan spectra of optically thin oxygen-richcircumstellar dust shells in the database produced by the ShortWavelength Spectrometer on ISO reveals that the strength of severalinfrared spectral features correlates with the strength of the 13 μmdust feature. These correlated features include dust features at 19.8and 28.1 μm and the bands produced by warm carbon dioxide molecules(the strongest of which are at 13.9, 15.0, and 16.2 μm). The databasedoes not provide any evidence for a correlation of the 13 μm featurewith a dust feature at 32 μm, and it is more likely that a weakemission feature at 16.8 μm arises from carbon dioxide gas ratherthan dust. The correlated dust features at 13, 20, and 28 μm tend tobe stronger with respect to the total dust emission in semiregular andirregular variables associated with the asymptotic giant branch than inMira variables or supergiants. This family of dust features also tendsto be stronger in systems with lower infrared excesses and thus lowermass-loss rates. We hypothesize that the dust features arise fromcrystalline forms of alumina (13 μm) and silicates (20 and 28 μm).Based on observations with the ISO, a European Space Agency (ESA)project with instruments funded by ESA member states (especially thePrincipal Investigator countries: France, Germany, the Netherlands, andthe United Kingdom) and with the participation of the Institute of Spaceand Astronautical Science (ISAS) and the National Aeronautics and SpaceAdministration (NASA).
| The association of IRAS sources and 12CO emission in the outer Galaxy
We have revisited the question of the association of CO emission withIRAS sources in the outer Galaxy using data from the FCRAO Outer GalaxySurvey (OGS). The availability of a large-scale high-resolution COsurvey allows us to approach the question of IRAS-CO associations from anew direction - namely we examined all of the IRAS sources within theOGS region for associated molecular material. By investigating theassociation of molecular material with random lines of sight in the OGSregion we were able to construct a quantitative means to judge thelikelihood that any given IRAS-CO association is valid and todisentangle multiple emission components along the line of sight. Thepaper presents a list of all of the IRAS-CO associations in the OGSregion. We show that, within the OGS region, there is a significantincrease ( ~ 22%) in the number of probable star forming regions overprevious targeted CO surveys towards IRAS sources. As a demonstration ofthe utility of the IRAS-CO association table we present the results ofthree brief studies on candidate zone-of-avoidance galaxies with IRAScounterparts, far outer Galaxy CO clouds, and very bright CO clouds withno associated IRAS sources. We find that ~ 25% of such candidate ZOAGsare Galactic objects. We have discovered two new far outer Galaxystar-forming regions, and have discovered six bright molecular cloudsthat we believe are ideal targets for the investigation of the earlieststages of sequential star formation around HII regions. Finally, thispaper provides readers with the necessary data to compare othercatalogued data sets with the OGS data.Tables 1, 2 and A1 are only available in electronic form at the CDS viaanonymous ftp to\ cdsarc.u-strasbg.fr (130.79.128.5) or via\http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/399/1083
| 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
| Aufsuchkarten fur intrinsic Variable Stars in Brno.
Not Available
| 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.
| Observational investigation of mass loss of M supergiants
We present the analysis of infrared photometry and millimeterspectroscopy of a sample of 74 late-type supergiants. These observationsare particularly suitable to study the mass loss and the circumstellarenvelopes of evolved massive stars. In particular, we quantify thecircumstellar infrared excess, the relation of mass loss with stellarproperties, using the K-[12] colour index as mass-loss indicator. We donot find any clear correlation between mass loss rate and luminosity. Wealso show that the K-band magnitude is a simple luminosity indicator,because of the relative constancy of the K-band bolometric correction.Based on observations collected at the European Southern Observatory, LaSilla, Chile within program ESO 54.E-0914, and on observations collectedwith the IRAM 30m telescope. Tables A1 to A3 are only available inelectronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html
| Period-luminosity relations for red supergiant variables - I.The calibration
We present CCD photometry of red supergiant long-period variables (LPVs)in the Per OB1 association, the Large Magellanic Cloud (LMC) and M33.The photometry was obtained in the Kron-Cousins R and I bandpasses andin a narrow bandpass (λ0=8250Å, FWHM=300Å)chosen to avoid TiO bands in the spectral energy distribution of theLPVs. Because the strength of the TiO bands varies greatly withtemperature, which varies with the phase of an LPV, avoiding TiO reducesthe amplitude of the photometric variations seen in LPVs. The result isa lower dispersion and a well defined period-luminosity (PL) relation.For the LMC sample we find an rms dispersion of 0.27mag in thenarrow-band PL relation and slightly larger dispersions for the LPVs inPer OB1 and M33. This dispersion is comparable to that of the Cepheid PLrelation at similar wavelengths. Adopting a distance modulus of18.5+/-0.1mag for the LMC, we obtain distance moduli of 11.68+/-0.15magfor Per OB1 and 24.85+/-0.13mag for M33. These distances agree well withthose based on main sequence fitting for Per OB1 and the Cepheiddistance for M33. Since LPVs are ~5 times more common than Cepheids andhave a well defined PL relation, LPVs provide a promising method forestimating Galactic and extra galactic distances.
| A Mid-Infrared Galaxy Atlas (MIGA)
A mid-infrared atlas of part of the Galactic plane(75deg
| Long-Term Changes in Mira Stars. III. Multiperiodicity in Mira Stars
The maximum magnitudes of many Mira stars fluctuate from cycle to cycle.In some cases, this may be due to multiperiodicity. We have analyzed themaximum magnitudes of a large sample of bright Mira stars, using aportion of the American Association of Variable Star Observersinternational database of variable star observations: times andmagnitudes of maximum and minimum of 391 bright Mira stars over 75years. We find many whose behavior can be interpreted as due tomultiperiodicity, with either a secondary period that is an order ofmagnitude longer than the primary period or a secondary periodcomparable with the primary one. In the former case, the nature of thelong secondary period is not clear, although, in some cases, it may berelated to episodic dust emission. In the latter case, the behavior ismost consistent with the hypothesis that the primary period is the firstovertone period and the secondary period is another radial mode.
| Silicate and hydrocarbon emission from Galactic M supergiants
Following our discovery of unidentified infrared (UIR) band emission ina number of M supergiants in h and chi Per, we have obtained 10-μmspectra of a sample of 60 galactic M supergiants. Only three newsources, V1749 Cyg, UW Aql and IRC+40 427, appear to show the UIR bands;the others show the expected silicate emission or a featurelesscontinuum. The occurrence of UIR-band emission in M supergiants istherefore much higher in the h and chi Per cluster than in the Galaxy asa whole. Possible explanations for the origin and distribution of UIRbands in oxygen-rich supergiants are discussed. We use our spectra toderive mass-loss rates ranging from 10^-8 to 10^-4 M_solar yr^-1 for thenew sample, based on the power emitted in the silicate feature. Therelationship between mass-loss rate and luminosity for M supergiants isdiscussed, and correlations are explored between their mid-infraredemission properties.
| 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.
| Infrared giants vs. supergiants. II. CO observations
We report systematic observations of millimeter CO emission from asample of 109 oxygen-rich evolved stars (AGB and supergiants),colour-selected from the IRAS Point Source Catalog (0.69 200). In most cases, the observed spread in the valuesof this ratio can be explained by a large range of luminosities. Thisleads to a new criterion to identify AGB stars: an object with {cal R}< 150 must have a low mass progenitor. Here we study the correlationsbetween {cal R} and various physical properties of the sources. Mostsources with high values of {cal R} also have low galactic latitudes,small IRAS variability indices, and early spectral types (typicallyM1-M5). Conversely, there is no dependence on the IRAS colours, nor onthe intensity of silicate 10;microns emission. However, a few AGB starsexhibit large {cal R}; other factors than luminosity are required toexplain these values. Different hypotheses, such as the possiblepresence of a chromosphere, a low (12) C abundance or a variablemass-loss rate, are examined. Considering the global high OH detectionrate ( ~ 67%), we studied the correlations with CO and OH emission. Thedetection of OH seems to be a useful discriminator of mechanisms thatenhance {cal R}.
| 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.
| Identification of IRAS Sources in the Outer Disk of the Galaxy
Near infrared imaging and photometric observations at J, H and K (or K')bands were performed toward 95 IRAS sources in the outer disk of theGalaxy most of which had been searched for SiO maser emission and arecandidates for variable late-type stars with cold circumstellarenvelopes. Low resolution optical spectroscopic observations were madeto 19 stars of them for classifying the spectral types. Thirty-eight ofthem, for which counterparts were not found at I band brighter than19mag, were taken near infrared images for identification. All areidentified in the near-infrared images brighter than 16 mag at K' bandexcept two that could be in the faint phase of variation when observed.So most of the IRAS late-type stars perhaps have a near-infraredcounterpart although many have no optical counterpart. In thenear-infrared color-color diagram, the stars with O-rich and C-richcircumstellar envelopes(CSEs) are separated from each other. The starswith C-rich CSE are redder than those with O-rich CSE in general butthere are three very red stars in this sample being SiO maser sources,i.e. with O-rich CSE. By combining the near-infrared colors and IRAScolor, the two types of circumstellar envelopes are discriminated. 48percent are stars with C-rich CSE in the entire sample and the numberratios of C-rich to O-rich stars are 14:43 and 32:6 for the opticallyidentified and unidentified groups respectively. This indicates anincreasing proportion of C-rich stars with galacto-centric distance andstellar evolutionary stage. The result is applied to explain the lowdetection rate of SiO maser emission in a similar and bigger sample inthe outer disk of the Galaxy.
| Red supergiants, neutrinos and the Double Cluster
The Perseus Double Cluster is surrounded by one of the largestconcentrations of red supergiant stars in the sky. As a consequence, thedevelopment of our understanding of the structure and evolution of thesestars has been intimately connected with studies of this cluster. Thispaper traces the history of this connection from the end of the 19thcentury through to the early 1970s.
| SiO Maser Sources in the Outer Disk of the Galaxy
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996ApJS..106..463J&db_key=AST
| An Infrared Color-Magnitude Relationship
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995AJ....110.2910H&db_key=AST
| Characterization and proportion of very cold C-rich circumstellar envelopes
The paper develops a method for identification of very cold C-richcircumstellar envelopes (CSEs) in IR regions colder than region VII(i.e., larger value of IRAS flux ratio S25/S12), by reviewing thedifferent criteria and by identifying C-rich CSEs in a sample of 228bright IRAS sources. By using the results of OH surveys and catalogstogether with the results of additional HCN/CO millimeter observationsperformed on critical classes of objects, a C/O classification isproposed for 94 percent of the sources with a good probability. It isshown that the low-resolution spectra by themselves are a reasonable andeasy way to identify C-rich late AGB CSEs. For post-AGB object with coldCSEs, HCN and OH observations or visible/near IR spectroscopy arenecessary.
| Galactic OB associations in the northern Milky Way Galaxy. I - Longitudes 55 deg to 150 deg
The literature on all OB associations was reviewed, and their IRAS pointsource content was studied, between galactic longitude 55 and 150 deg.Only one third of the 24 associations listed by Ruprecht et al. (1981)have been the subject of individual studies designed to identify thebrightest stars. Distances to all of these were recomputed using themethod of cluster fitting of the B main sequence stars, which makes itpoossible to reexamine the absolute magnitude calibration of the Ostars, as well as for the red supergiant candidate stars. Also examinedwas the composite HR diagram for these associations. Associations withthe best defined main sequences, which also tend to contain very youngclusters, referred to here as OB clusters, have extremely few evolved Band A or red supergiants. Associations with poorly defined mainsequences and few OB clusters have many more evolved stars. They alsoshow an effect in the upper HR diagram referred to as a ledge byFitzpatrick and Garmany (1990) in similar data for the Large MagellanicCloud. It is suggested that the differences in the associations are notjust observational selection effects but represent real differences inage and formation history.
| A Complete Survey of OH / Infrared Objects from the IRAS LRS Sources Within a Domain of the Color Diagram
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1992A&A...254..133L&db_key=AST
| IRAS low-resolution spectral observations of the 10 and 18 micron silicate emission feature
The IRAS LRS Atlas contains 8-23 micron spectra of 1816 stars withsilicate emission features. In order to study the shapes of the silicatedust features, the 117 stars whose emission features appear to beoptically thin and which have the best signal-to-noise ratio at thelongest wavelengths were analyzed. Simple spherical dust shell modelswere calculated in both the optically thin and the slightly opticalthick approximations. From the comparison of the predicted spectra ofthe dust and stellar continuum, the emissivity function Kappa(lambda)was derived. In the different stars, the shape of the 10-micron featureis either narrow or broad and it is peaked either at about 9.7 micronsor at 10 microns. Either particle size effects (particles above 0.75microns in radius) or optical depth effects (central optical depth about1) could broaden the 10-micron feature. Chemical composition differencesno doubt are also important, particularly as regards the position of thepeak of the 10-micron feature. The stars with the peak at 10 microns aremore closely confined to the Galactic plane than the stars with the peakat 9.7 microns. The shape of the 18-micron feature is essentially thesame in all stars, and can be used to extend the interstellar extinctioncurve past 13 to 22 microns.
| Mass-losing M supergiants in the solar neighborhood
A list of the 21 mass-losing red supergiants (20 M type, one G type; Lgreater than 100,000 solar luminosities) within 2.5 kpc of the sun iscompiled. These supergiants are highly evolved descendants ofmain-sequence stars with initial masses larger than 20 solar masses. Thesurface density is between about 1 and 2/sq kpc. As found previously,these stars are much less concentrated toward the Galactic center thanW-R stars, which are also highly evolved massive stars. Although withconsiderable uncertainty, it is estimated that the mass return by the Msupergiants is somewhere between 0.00001 and 0.00003 solar mass/sq kpcyr. In the hemisphere facing the Galactic center there is much less massloss from M supergiants than from W-R stars, but, in the anticenterdirection, the M supergiants return more mass than do the W-R stars. Theduration of the M supergiant phase appears to be between 200,000 and400,000 yr. During this phase, a star of initially at least 20 solarmasses returns perhaps 3-10 solar masses into the interstellar medium.
| Statistical characteristics of the ten-micron silicate emission in M-type stars
The statistical characteristics of 10 micron silicate emission wereexamined for 1427 M-type stars in the catalog of the Two-Micron SkySurvey using the low-resolution spectra obtained by IRAS. Correlationswere examined of 10 micron silicate emission with the spectralclassification in the visual wavelength region, with near-infrared colorI - K, with a variability type, and with the period of variation. It wasfound that supergiants show silicate emission more frequently than dogiants. Silicate emission was found in stars of all three variabilitytypes: irregular, semiregular, and Mira variables. The proportion ofstars with silicate emission was found to be larger for Mira variables.Most of the Mira variables with periods of variation longer than about450 d were found to show silicate emission.
| Photoelectric photometry of G-M stars in the Vilnius system
Not Available
| Infrared circumstellar shells - Origins, and clues to the evolution of massive stars
The infrared fluxes, spatial and spectral characteristics for a sampleof 111 supergiant stars of spectral types F0 through M5 are tabulated,and correlations examined with respect to the nature of theircircumstellar envelopes. One-fourth of these objects were spatialyresolved by IRAS at 60 microns and possess extended circumstellar shellmaterial, with implied expansion ages of about 10 to the 5th yr.Inferences about the production of dust, mass loss, and the relation ofthese characteristics of the evolution of massive stars, are discussed.
| Infrared spectra and circumstellar emission of late-type stars
NIR photometry has been carried out for 63 M-type stars in eightphotometric bands. Four bands were the usual J, H, K, and L bands ofbroad-band photometry, and the other four were defined with relativelynarrow filters at 3.1, 3.3, 3.4, and 3.7 microns to measure the strengthof a stellar H2O absortion band centered at about 2.7 microns. Theeffects of circumstellar emission due to silicate dust on the energyspectra of oxygen-rich stars are extracted on the basis of the presentdata and IRAS photometric data. Peculiar carbon stars which exhibit asilicatelike emission feature at 10 microns were searched for from about1800 carbon stars. Eleven new candidate carbon stars were found.
| Circumstellar environments. III - M-supergiants
Spectra of M-supergiants in the 7-100-micron region are studied. Thecircumstellar silicate dust features at 9.7 and 18 microns are found tobe of variable width. Although most stars are shown to exhibit theclassical circumstellar silicate dust features typified by those ofAlpha Ori, some, such as VX SGr, exhibit much broader features.Mass-loss rates are given for 31 M-supergiants.
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| קבוצת-כוכבים: | פרסאוס |
| התרוממות ימנית: | 02h50m37.89s |
| סירוב: | +56°59'00.2" |
| גודל גלוי: | 9.087 |
| מרחק: | 10000000 פארסק |
| תנועה נכונה: | -2.7 |
| תנועה נכונה: | -3.7 |
| B-T magnitude: | 12.592 |
| V-T magnitude: | 9.377 |
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