J/ApJ/743/24ivo://CDS.VizieR/J/ApJ/743/24doi:10.26093/cds/vizier.17430024CDSSerenelli A.M.Haxton W.C.Pena-Garay C.2013-06-23T12:34:06Z2013-06-05T14:11:03ZCDS support team

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

cds-question@unistra.frthe-sunastronomical-modelsWe generate new standard solar models using newly analyzed nuclear fusion cross sections and present results for helioseismic quantities and solar neutrino fluxes. The status of the solar abundance problem is discussed. We investigate whether nonstandard solar models with accretion from the protoplanetary disk might alleviate this problem. We examine a broad range of models, analyzing metal-enriched and metal-depleted accretion and three scenarios for the timing of accretion. Only partial solutions are found. For metal-rich accreted material (Z_ac_>~0.018) there exist combinations of accreted mass and metallicity that bring the depth of the convective zone into agreement with the helioseismic value. For the surface helium abundance, the helioseismic value is reproduced if metal-poor or metal-free accretion is assumed (Z_ac_<~0.09). In both cases a few percent of the solar mass must be accreted. Precise values depend on when accretion takes place. We do not find a simultaneous solution to both problems but speculate that changing the hydrogen-to-helium mass ratio in the accreted material may lead to more satisfactory solutions. We also show that, with current data, solar neutrinos are already a very competitive source of information about the solar core and can help constraining possible accretion histories. Even without helioseismic constraints, solar neutrinos rule out the possibility that more than 0.02M_{sun}_ from the protoplanetary disk were accreted after the Sun settled on the main sequence. Finally, we discuss how measurements of neutrinos from the CN cycle could shed light on the interaction between the early Sun and its protoplanetary disk.2011ApJ...743...24Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/743/24CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/743/24https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/743/24http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/743/24https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/743/24https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/743/24http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/743/24GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/ApJ/743/24/table5Main properties of solar models including accretionrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintModelModel (E1 to L95) (1)meta.notechartauaccTime when accretion begins (5, 15 or 30)Myrtime.epochintMaccAccreted masssolMassphys.massdoubleZacc[0/1] Metallicity of accreted matterphys.abund.ZfloatYacc[0/1] Helium mass fraction of accreted matterphys.abund.YfloatZini[0/1] Initial metallicityphys.abund.ZfloatYini[0/1] Initial helium mass fractionphys.abund.YfloataMLTMixing Length Parameter {alpha}_MLT_stat.paramfloatZs[0/1] Final surface metallicityphys.abund.ZfloatYs[0/1] Final surface helium mass fractionphys.abund.YfloatRczDepth of convective envelopesolRadstat.paramfloat<dc/c>Average rms of relative sound speed difference <{delta}c/c>phot.flux;meta.modelledfloatZc[0/1] Central metallicity Z_c_phys.abund.ZfloatYc[0/1] Central helium mass fraction Y_c_phys.abund.YfloatTcCentral temperature T_c_MKphys.temperaturefloatrho.cCentral density {rho}_c_g.cm**-3phys.densityfloatppneutrino flux from pp reaction1e+10cm**-2.s**-1phot.flux;meta.modelledfloatpepneutrino flux from pep reaction1e+08cm**-2.s**-1phot.flux;meta.modelledfloatBe7neutrino flux from ^7^Be1e+09cm**-2.s**-1phot.flux;meta.modelledfloatB8neutrino flux from ^8^B1e+08cm**-2.s**-1phot.flux;meta.modelledfloatN13neutrino flux from ^13^N1e+08cm**-2.s**-1phot.flux;meta.modelledfloatO15neutrino flux from ^15^O1e+08cm**-2.s**-1phot.flux;meta.modelledfloatchi2Global {chi}^2^ for neutrino fluxesstat.fit.chi2float