J/MNRAS/468/305ivo://CDS.VizieR/J/MNRAS/468/305doi:10.26093/cds/vizier.74680305CDSMolla M.Diaz A.I.Ascasibar Y.Gibson B.K.2024-08-17T20:18:41Z2021-10-25T09:44:15ZCDS support team

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

cds-question@unistra.frchemical-abundancesstellar-evolutionary-modelsgalaxiesIn our classical grid of multiphase chemical evolution models, star formation in the disc occurs in two steps: first, molecular gas forms, and then stars are created by cloud-cloud collisions or interactions of massive stars with the surrounding molecular clouds. The formation of both molecular clouds and stars are treated through the use of free parameters we refer to as efficiencies. In this work, we modify the formation of molecular clouds based on several new prescriptions existing in the literature, and we compare the results obtained for a chemical evolution model of the Milky Way Galaxy regarding the evolution of the Solar region, the radial structure of the Galactic disc and the ratio between the diffuse and molecular components, H I/H_2_. Our results show that the six prescriptions we have tested reproduce fairly consistent most of the observed trends, differing mostly in their predictions for the (poorly constrained) outskirts of the Milky Way and the evolution in time of its radial structure. Among them, the model proposed by Ascasibar et al. (in preparation), where the conversion of diffuse gas into molecular clouds depends on the local stellar and gas densities as well as on the gas metallicity, seems to provide the best overall match to the observed data.2017MNRAS.468..305Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/468/305CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/468/305https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/468/305http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/468/305https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/468/305https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/468/305http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/468/305GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/MNRAS/468/305/catalog*Time evolution results for the six models presented in the work.recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintModelModel: BLI, GNE, KRU, MOD, STD, ASCstat.param;meta.modelledcharTime1389 evolutionary time steps from 0 to 13.2GyrGyrtime.agedoubleRGalactocentric radius for 25 regions from R=0 to 24kpckpcpos.distance;pos.galactocentricfloatAreaArea for the considered regionkpc**2phys.angSizefloatSFRStar formation rate of each region in each timesolMass/yrphys.SFR;obs.fielddoubleSig-tSurface density of the total mass involved in the modelsolMass.pc**-2phys.densityfloatSig-dSurface density of the total mass in the discsolMass.pc**-2phys.densityfloatSig-HISurface density of the diffuse gassolMass.pc**-2phot.flux.density.sbfloatSig-H2Surface density of the molecular gassolMass.pc**-2phot.flux.density.sbfloatSig-S2Surface density of massive starssolMass.pc**-2src.densityfloatSig-S1Surface density of low-mass starssolMass.pc**-2src.densityfloatSig-remSurface density of remnantssolMass.pc**-2meta.notefloatHAbundance of H in massphys.abund.XfloatDAbundance of D in massphys.abunddoubleHe3Abundance of ^3^He in massphys.abunddoubleHe4Abundance of ^4^He in massphys.abundfloatC12Abundance of ^12^C in massphys.abundfloatC13Abundance of ^13^C in massphys.abundfloatN14Abundance of ^14^N in massphys.abundfloatOAbundance of O in massphys.abundfloatNeAbundance of Ne in massphys.abundfloatMgAbundance of Mg in massphys.abundfloatSiAbundance of Si in massphys.abundfloatSAbundance of S in massphys.abundfloatCaAbundance of Ca in massphys.abundfloatFeAbundance of Fe in massphys.abundfloatJ/MNRAS/468/305/rhalfEvolution of the effective radius for total mass and half stellar radius with the half stellar mass for each one of the six modelsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTimeEvolutionary time (1389 steps)Gyrtime.agefloatR1/2MHalf mass radius for disk masskpcphys.size.radiusfloatR1/2SBHalf stellar mass radius for BLIkpcphys.size.radiusfloatlogM1/2Blogarithm of the half stellar mass for BLIlog(solMass)phys.massfloatR1/2GHalf stellar mass radius for GNEkpcphys.size.radiusfloatlogM1/2Glogarithm of the half stellar mass for GNElog(solMass)phys.massfloatR1/2KHalf stellar mass radius for KRUkpcphys.size.radiusfloatlogM1/2Klogarithm of the half stellar mass for KRUlog(solMass)phys.massfloatR1/2SMHalf stellar mass radius for MODkpcphys.size.radiusfloatlogM1/2Mlogarithm of the half stellar mass for MODlog(solMass)phys.massfloatR1/2SHalf stellar mass radius for STDkpcphys.size.radiusfloatlogM1/2Slogarithm of the half stellar mass for STDlog(solMass)phys.massfloatR1/2AHalf stellar mass radius for ASCkpcphys.size.radiusfloatlogM1/2Alogarithm of the half stellar mass for ASClog(solMass)phys.massfloat