J/A+A/667/L2ivo://CDS.VizieR/J/A+A/667/L2doi:10.26093/cds/vizier.36679002CDSKunitomo M.Guillot T.Buldgen G.2024-11-06T20:01:27Z2022-11-03T09:10:17ZCDS support team

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

cds-question@unistra.frthe-sunstellar-evolutionary-modelschemical-abundancespre-main-sequence-starsSolar evolutionary models are thus far unable to reproduce spectroscopic, helioseismic, and neutrino constraints consistently, resulting in the so-called solar modeling problem. In parallel, planet formation models predict that the evolving composition of the protosolar disk, and thus, of the accreted gas by the proto-Sun must have been variable. We show that solar evolutionary models that include a realistic planet formation scenario lead to an increased core metallicity of up to 5%, implying that accurate neutrino flux measurements are sensitive to the initial stages of the formation of the Solar System. Models with homogeneous accretion match neutrino constraints to no better than 2.7{sigma}. In contrast, accretion with a variable composition due to planet formation processes, leading to metal-poor accretion of the last ~4% of the young Sun's total mass, yields solar models within 1.3{sigma} of all neutrino constraints. We thus demonstrate that in addition to increased opacities at the base of the convective envelope, the formation history of the Solar System constitutes a key element in resolving the current crisis of solar models.2022A&A...667L...2Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/667/L2CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/655/A51 : Solar evolutionary and structure models (Kunitomo+, 2021)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/667/L2https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/667/L2http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/667/L2https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/667/L2https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/667/L2http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/667/L2GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/667/L2/tableaResults of 33 solar modelsYsurfSurface helium abundance at 4.567Gyrphys.abund.YdoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameModel namemeta.id;meta.maincharalphaMLTMixing-length parameterstat.paramdoublefovershootOvershooting parameterstat.paramdoubleXprotoPrimordial hydrogen abundance (mass fraction)phys.abund.XdoubleYprotoPrimordial helium abundancephys.abund.YdoubleZprotoPrimordial metallicityphys.abund.ZdoubleZaccmaxMaximum accretion metallicityphys.abund.ZdoubleM1Stellar mass when Zaccretion starts to increasesolMassphys.massdoubleM2Stellar mass when Zaccretion decreases to zerosolMassphys.massdoubleA1Opacity enhancement parameter at logT=5.66stat.paramfloatA2Opacity enhancement parameter at logT=6.45stat.paramdoubleA3Opacity enhancement parameter at logT=7.18stat.paramdoubleYaccminMinimum helium abundance of accretion gasphys.abund.Y;stat.minfloattaccAccretion timescaleMyrtime.agefloatchi2Chi-square valuestat.valuedoublecsrmsRoot mean square of sound speed at 4.567Gyrstat.errordoubleZXsurfRatio of the surface metallicity to the surface hydrogen abundance at 4.567Gyrphys.abunddoubleRczLocation of the convective-radiative boundarysolRadstat.paramdoublelogLlog(bolometric luminosity) at 4.567Gyrlog(solLum)phys.luminositydoubleTeffEffective temperature at 4.567GyrKphys.temperature.effectivedoubleZcenterCentral metallicity at 4.567Gyrphys.abund.ZdoubleZsurfSurface metallicity at 4.567Gyrphys.abund.ZdoubleMXYlostMass ejected from the disk assuming M_Z,planet_=150M_{earth}_solMassphys.massdoubleMZplanetMetal mass retained by planets assuming M_XY,lost_=0(5.97236x10+24kg)phys.massdoubleTcenterCentral temperature at 4.567GyrKphys.temperaturedoublePcenterCentral pressure at 4.567Gyr (erg/cm^3^)1e-07J.cm**-3phys.pressuredoublerhocenterCentral density at 4.567Gyrg.cm**-3phys.densitydoubleXcenterCentral hydrogen abundance at 4.567Gyrphys.abund.XdoubleYcenterCentral helium abundance at 4.567Gyrphys.abund.YdoublemucenterCentral mean molecular weight at 4.567Gyrphys.atmol.weightdoublekapcenterCentral opacity at 4.567Gyrcm**2.g**-1phys.absorption.coeff;em.wl.centraldoublePhipppp neutrino flux at the Earth at 4.567Gyrcm**-2.sphot.flux;phys.particle.neutrinodoublePhipeppep neutrino flux at the Earth at 4.567Gyrcm**-2.sphot.flux;phys.particle.neutrinodoublePhi7Be7Be neutrino flux at the Earth at 4.567Gyrcm**-2.sphot.flux;phys.particle.neutrinodoublePhi8B8B neutrino flux at the Earth at 4.567Gyrcm**-2.sphot.flux;phys.particle.neutrinodoublePhiN13N13 neutrino flux at the Earth at 4.567Gyrcm**-2.sphot.flux;phys.particle.neutrinodoublePhiO15O15 neutrino flux at the Earth at 4.567Gyrcm**-2.sphot.flux;phys.particle.neutrinodoublePhiF17F17 neutrino flux at the Earth at 4.567Gyrcm**-2.sphot.flux;phys.particle.neutrinodoublePhiCNOCNO neutrino flux at the Earth at 4.567Gyrcm**-2.sphot.flux;phys.particle.neutrinodoubleP0g-mode period spacing integralstime.perioddouble