We construct updated solar models with different sets of solar abundances , including the most recent determinations by Asplund et al .
( 8 ) .
The latter work predicts a larger ( \sim 10 \% ) solar metallicity compared to previous measurements by the same authors but significantly lower ( \sim 25 \% ) than the recommended value from a decade ago by Grevesse & Sauval ( 29 ) .
We compare the results of our models with determinations of the solar structure inferred through helioseismology measurements .
The model that uses the most recent solar abundance determinations predicts the base of the solar convective envelope to be located at R _ { CZ } = 0.724 { R _ { \odot } } and a surface helium mass fraction of Y _ { surf } = 0.231 .
These results are in conflict with helioseismology data ( R _ { CZ } = 0.713 \pm 0.001 { R _ { \odot } } and Y _ { surf } = 0.2485 \pm 0.0035 ) at 5 - \sigma and 11 - \sigma levels respectively .
Using the new solar abundances , we calculate the magnitude by which radiative opacities should be modified in order to restore agreement with helioseismology .
We find that a maximum change of \sim 15 \% at the base of the convective zone is required with a smooth decrease towards the core , where the change needed is \sim 5 \% .
The required change at the base of the convective envelope is about half the value estimated previously .
We also present the solar neutrino fluxes predicted by the new models .
The most important changes brought about by the new solar abundances are the increase by \sim 10 \% in the predicted ^ { 13 } N and ^ { 15 } O fluxes that arise mostly due to the increase in the C and N abundances in the newly determined solar composition .