J/A+A/673/A78ivo://CDS.VizieR/J/A+A/673/A78doi:10.26093/cds/vizier.36730078CDSEmsenhuber A.Burn R.Weder J.Monsch K.Picogna G.Ercolano B.,Preibisch T.2024-11-06T20:04:10Z2023-05-10T07:40:52ZCDS support team

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

cds-question@unistra.frastronomical-modelsmultiple-starsexoplanetsWe want to find the distribution of initial conditions that best reproduces disc observations at the population level. We first run a parameter study using a 1D model that includes the viscous evolution of a gas disc, dust, and pebbles, coupled with an emission model to compute the mm flux observable with ALMA. This is used to train a machine learning surrogate model, which can compute the relevant quantity for comparison with observations in seconds. This surrogate model is used to perform parameter studies and synthetic disc populations. Performing parameter study, we find that internal photoevaporation lead to lower dependency of disc lifetimes on stellar mass than external photoevaporation. This dependence should be investigated in the future. Performing population synthesis, we find that under the combined losses of internal and external photoevaporation, discs are too short lived. To match observational constraints, future models of disc evolution need to include either or all of the following processes: infall of material to replenish the discs, shielding of the disc from internal photoevaporation due to magnetically-driven disc winds, and extinction of external high-energy radiation. Nevertheless, disc properties in low-external photoevaporation regions can be reproduced by having more massive and compact discs. Here, the optimum values of the alpha viscosity parameter lie between 3*10^-4^ and 10^-3^ and with internal photoevaporation being the main mode of disc dispersal.2023A&A...673A..78Ehttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/673/A78CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/673/A78https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/673/A78http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/673/A78https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/673/A78https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/673/A78http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/673/A78GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/673/A78/table3Training and validation datarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMstarMass of the central starsolMassphys.massfloatMdiskfGas disc-to-star initial mass ratiophys.massdoubleexpoPower-law index of the initial profilestat.fit.paramdoublePeriodOrbital period at the inner edgedtime.perioddoubleaoutCharateristic radius of the initial profileAUphys.angSize;srcdoublealphaTurbulent viscosity parameterstat.fit.paramdoublefpgInitial dust-to-gas mass ratio in the discphys.mass;arith.ratiodoubleVfragFragmentation velocitycm/sphys.velocdoublepeffPlanetesimals formation efficiencyphys.SFRdoublefdriftDrift efficiency factorstat.fit.paramdoubleLXStellar X-ray luminosity1e+23Wphys.luminosity;em.X-raydoubleUVfsAmbient UV field strength1.6e-06kg.s**-3phys.magFielddoubledltMassDisc lifetime based on mass criterion (1)yrtime.epochdoubledltNIRDisc lifetime based on near-IR criterion (2)yrtime.epochdoubleAcc1e5Stellar accretion rate at 100kyr (3)solMass/yrarith.ratedoubleMobs1e5Observable dust mass at 100kyr (3)solMassphys.massdoubler681e5Radius containing 68% of the flux at 100kyr (3)AUphys.angSize;srcdoubleAcc2e6Stellar accretion rate at 2Myr (3)solMass/yrarith.ratedoubleMobs2e6Observable dust mass at 2Myr (3)solMassphys.massdoubler68e6Radius containing 68% of the flux at 2Myr (3)AUphys.angSize;srcdoubleJ/A+A/673/A78/table4Testing datadltMassDisc lifetime based on mass criterion (1)yrtime.epochdoubledltNIRDisc lifetime based on near-IR criterion (2)yrtime.epochdoubleAcc1e5Stellar accretion rate at 100kyr (3)solMass/yrarith.ratedoubleMobs1e5Observable dust mass at 100kyr (3)solMassphys.massdoubler681e5Radius containing 68% of the flux at 100kyr (3)AUphys.angSize;srcdoubleAcc2e6Stellar accretion rate at 2Myr (3)solMass/yrarith.ratedoubleMobs2e6Observable dust mass at 2Myr (3)solMassphys.massdoubler68e6Radius containing 68% of the flux at 2Myr (3)AUphys.angSize;srcdoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMstarMass of the central starsolMassphys.massfloatMdiskfGas disc-to-star initial mass ratiophys.massdoubleexpoPower-law index of the initial profilestat.fit.paramdoublePeriodOrbital period at the inner edgedtime.perioddoubleaoutCharateristic radius of the initial profileAUphys.angSize;srcdoublealphaTurbulent viscosity parameterstat.fit.paramdoublefpgInitial dust-to-gas mass ratio in the discphys.mass;arith.ratiodoubleVfragFragmentation velocitycm/sphys.velocdoublepeffPlanetesimals formation efficiencyphys.SFRdoublefdriftDrift efficiency factorstat.fit.paramdoubleLXStellar X-ray luminosity1e+23Wphys.luminosity;em.X-raydoubleUVfsAmbient UV field strength1.6e-06kg.s**-3phys.magFielddouble