J/MNRAS/469/521ivo://CDS.VizieR/J/MNRAS/469/521doi:10.26093/cds/vizier.74690521CDSKral Q.Matra L.Wyatt M.C.Kennedy G.M.2024-08-17T20:19:43Z2020-04-21T15:18:42ZCDS support team

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

cds-question@unistra.frastronomical-modelsstellar-massesco-line-emissionThis paper uses observations of dusty debris discs, including a growing number of gas detections in these systems, to test our understanding of the origin and evolution of this gaseous component. It is assumed that all debris discs with icy planetesimals create second generation CO, C and O gas at some level, and the aim of this paper is to predict that level and assess its observability. We present a new semi-analytical equivalent of the numerical model of Kral et al. (2016MNRAS.461.1614K) allowing application to large numbers of systems. That model assumes CO is produced from volatile-rich solid bodies at a rate that can be predicted from the debris discs fractional luminosity. CO photodissociates rapidly into C and O that then evolve by viscous spreading. This model provides a good qualitative explanation of all current observations, with a few exceptional systems that likely have primordial gas. The radial location of the debris and stellar luminosity explain some non-detections, e.g. close-in debris (like HD 172555) is too warm to retain CO, while high stellar luminosities (like {eta} Tel) result in short CO lifetimes. We list the most promising targets for gas detections, predicting >15 CO detections and >30 CI detections with ALMA, and tens of CII and O I detections with future far-IR missions. We find that CO, CI, CII and OI gas should be modelled in non-LTE for most stars, and that CO, CI and OI lines will be optically thick for the most gas-rich systems. Finally, we find that radiation pressure, which can blow out CI around early-type stars, can be suppressed by self-shielding.2017MNRAS.469..521Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/469/521CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/469/521https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/469/521http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/469/521https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/469/521https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/469/521http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/469/521GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/469/521/tablec1 (*Description of the 190 stars used in this study)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/469/521/tablec1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/469/521/tablec1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/469/521/tablec1?GETtext/xml+votable180.050000true86.8211986-51.06651140.0055555555555555566/765 861 934 940 1069 1603 2170 2370 2651-2652 2724 2816 4018 4042 4338 4591 4597 5311 5645 6082 6766 7763 7765 8145 8687 8717 10034 10334 10549 10812 11075 11314 11633 11844 11917 11946 12341 12592 14180 14290 16104 16543 16606 17266 17421 17425 17486 17607 17887 17952 19509 19598 20328 20530 20593 20657 21023 21043 21080 21083 21177 21285 21289 21386 21484 21703 22036 22849 23013 23140 23190 23376 24019 24924 25056 25120 26216 26975 27884 28018 28041 29348 31399 31667 31776 32466 32619 32891 33500 33508 33694 33976 34054 34147 34168 34245 34282 34508 34683 34905 34993 35474 35497 36130 36421 36664 36697 36969 37063 37175 37810 37953 38412 38687 38765 38932 38937 39501 39693 39735 40442 40692 40892 40932 41352 41607 41632 41643 41677 41710 42072 42296 42555 42601 42678 42684 42711 42714 42746 42903 43010 43017 43029 43055 43095 43150 43197 43274 43358 43369 43527 43540 43677 43804 43854 44052 44069 44106 44139 44238 44321 44368 44378 44550 44921 45412 45430 45746 45865 45927 46113 46640 46734 46939 47061 47205 47414 47464 47626 47775 48021 48274 48334 48541 48627 486513.256468315563905e-22 3.3107421909657627e-21https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/469/521?format=asciiRadiodefaultJ/MNRAS/469/521/tablec1*Description of the 190 stars used in this studySimbadNameSimbad column added by the CDSmeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar namemeta.id;meta.mainchardDistance to Earthpcpos.angDistancefloatTeffStar effective temperatureKphys.temperature.effectiveintL*Star luminositysolLumphys.luminosityfloatLIR/L*Dust fractional luminosityphys.luminosity;arith.ratiodoubleR0Location of the beltAUpos.distancefloatF60Flux at 60umJyphot.flux.density;em.IR.30-60umdoubleF160Flux at 160umJyphot.flux.density;em.mm.1500-3000GHzdoubleF610Flux at 610umJyphot.flux.density;em.mm.1500-3000GHzdouble_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainJ/MNRAS/469/521/tablec2Model predictions for the 188 stars used in this studyrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar namemeta.id;meta.maincharMCOCO masssolMassphys.massdoubleFCO1300CO flux at 1.3mmW.m**-2phot.flux.density;em.mm.200-400GHzdoubleFCO870CO flux at 870umW.m**-2phot.flux.density;em.mm.200-400GHzdoubleMCICI masssolMassphys.massdoubleFCI610CI flux at 610umW.m**-2phot.flux.density;em.mm.1500-3000GHzdoubleMCIICII masssolMassphys.massdoubleFCII158CII flux at 158umW.m**-2phot.flux.density;em.mm.1500-3000GHzdoubleMOIOI mass (with extra water, see Section 6.2)solMassphys.massdoubleFOI63OI flux at 63um (with extra water)W.m**-2phot.flux.density;em.IR.30-60umdouble