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We have computed accurate 1-D solar models including both a macroscopicmixing process in the solar tachocline as well as up-to-date microscopicphysical ingredients. Using sound speed and density profiles inferred throughprimary inversion of the solar oscillation frequencies coupled with theequation of thermal equilibrium, we have extracted the temperature and hydrogenabundance profiles. These inferred quantities place strong constraints on ourtheoretical models in terms of the extent and strength of our macroscopicmixing, on the photospheric heavy elements abundance, on the nuclear reactionrates such as $S_{11}$ and $S_{34}$ and on the efficiency of the microscopicdiffusion. We find a good overall agreement between the seismic Sun and ourmodels if we introduce a macroscopic mixing in the tachocline and allow forvariation within their uncertainties of the main physical ingredients. From ourstudy we deduce that the solar hydrogen abundance at the solar age is $X_{\rminv}=0.732\pm 0.001$ and that based on the $^9$Be photospheric depletion, themaximum extent of mixing in the tachocline is 5% of the solar radius. Thenuclear reaction rate for the fundamental $pp$ reaction is found to be$S_{11}(0)=4.06\pm 0.07$ $10^{-25}$ MeV barns, i.e., 1.5% higher than thepresent theoretical determination. The predicted solar neutrino fluxes arediscussed in the light of the new SNO/SuperKamiokande results.Comment: 16 pages, 12 figures, A&A in press (1) JILA, University of Colorado,  Boulder, CO 80309-0440, USA, (2) LUTH, Observatoire de Paris-Meudon, 92195  Meudon, France, (3) Tata Institute of Fundamental Research, Homi Bhabha road,  Mumbai 400005, India, (4) Department of Physics, University of Mumbai, Mumbai  400098, Indi

Seismic tests for solar models with tachocline mixing