J/A+A/317/503ivo://CDS.VizieR/J/A+A/317/503doi:10.26093/cds/vizier.33170503CDSGroenewegen M.A.T1997-12-09T16:49:13Z1997-12-09T17:49:05ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frinfrared-sourcesvariable-starsA spherically symmetric dust radiative transfer code is used to model the circumstellar dust shell around IRC +10 216. Compared to numerous previous models a much larger body of observational data is used as constraints; the spectral energy distribution between 0.5 and 60000{mu}m, 2-4{mu}m and 8-23{mu}m spectra, optical, far-infrared and centimeter sizes and interferometric visibility curves between 1.6 and 11.2{mu}m are used to constrain the model. The most important result is that in order to fit the visibility curve at 2.2{mu}m and the size of the shell in the optical, scattering has to be invoked.1997A&A...317..503Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/317/503CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/317/503https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/317/503http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/317/503https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/317/503https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/317/503http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/317/503GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapInfrareddefaultJ/A+A/317/503/table1Summary of existing models of IRC +10 216recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRefReference (1)meta.refcharTeffEffective temperature or lowest value if interval of the central starKphys.temperature.effectiveintn_Teff[A-] Note on Teff (2)meta.notecharTeff2? Highest effective temperature when intervalphys.temperature.effectiveintDepthOptical depthphys.absorption.opticalDepthcharRadc? Inner radius or lowest value if interval of the dust shell in stellar radiipos.distancefloatn_RadcNote on Radc (2)meta.notecharRadc2? Highest inner radius when intervalpos.distancefloatTc? Dust temperature at the inner dust radiusKphys.temperatureintn_TcNote on Tc (2)meta.notecharGrainsType of grain usedmeta.notecharDensLaw? r power number of the density lawstat.paramfloatn_DensLaw[bce] Note on DensLaw (3)meta.notecharL/D2? Luminosity versus square distancesolLum.kpc**-2phys.luminosity;em.IRintn_L/D2'?' for unknown valuemeta.notecharConstConstraints used (4)meta.notecharJ/A+A/317/503/table2Photometric data used in the modelingRemRemarksmeta.notecharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRefReferencemeta.refcharLambdaWavelengthumem.wlfloatn_Lambda'-' when intervalmeta.notecharLambda2? Highest wavelength when intervalumem.wlintFlux? Flux (see unit in X_Flux)phot.flux;arith.ratiodoublee_Flux? rms uncertainty on Fluxstat.errorfloatx_FluxUnits of flux and e_Fluxmeta.unitcharBeam? Beam sizearcsecphys.angSize;instr.beamfloatn_Beam[?x]? for unknown value; x for box beammeta.notecharBeam2? Second value when box beam (AxB)arcsecphys.angSize;instr.beamintPhase[0/1[? Phase (1)time.phasefloatn_Phase[?-] ? for unknown value; - when intervalmeta.notecharPhase2? Highest values when intervaltime.phasefloatJ/A+A/317/503/table3Visibility datarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintLambdaWavelengthumem.wlfloatRefReferencemeta.refcharPhase1[0/1[ Phase (1)time.phasefloatn_Phase1'-' when intervalmeta.notecharPhase1b[0/1.25]? Upper value when intervalmeta.codefloatPhase2[0/1[? Second values for the phasetime.phasefloatPhase3[0/1[? Third values for the phasetime.phasefloatRemRemarksmeta.notechar