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Solar models using the new lower abundances of Asplund et al. (2005, 2009) orCaffau et al. (2008, 2009) do not agree as well with helioseismic inferences asmodels that use the higher Grevesse & Noels (1993) or Grevesse & Sauval (1998)abundances. Adopting the new abundances leads to models with sound speeddiscrepancies of up to 1.4$%$ below the base of the convection zone (comparedto discrepancies of less than 0.4$%$ with the old abundances), a convectionzone that is too shallow, and a convection zone helium abundance that is toolow. Here we review briefly recent attempts to restore agreement, and weevaluate three changes to the models: early mass loss, accretion of low-Zmaterial, and convective overshoot. One goal of these attempts is to exploremodels that could preserve the structure in the interior obtained with the oldabundances while accommodating the new abundances at the surface. Although themass-losing and accretion models show some improvement in agreement withseismic constraints, a satisfactory resolution to the solar abundance problemremains to be found. In addition, we perform a preliminary analysis of modelswith the Caffau et al. (2008, 2009) abundances that shows that the sound speeddiscrepancy is reduced to only about 0.6$%$ at the convection zone base,compared to 1.4$%$ for the Asplund et al. (2005) abundances and 0.4$%$ for theGrevesse & Noels (1993) abundances. Furthermore, including mass loss in modelswith the Caffau et al. (2008, 2009) abundances may improve sound speedagreement and help resolve the solar lithium problem.

Exploring mass loss, low-Z accretion, and convective overshoot in solar models to mitigate the solar abundance problem