  Stellar seismology appears more and more as a powerful tool for a better
determination of the fundamental properties of solar-type stars. However the
particular case of Sun is still challenging. The helioseismic sound speed
determination continues to disagree with the Standard Solar Model (SSM)
prediction for about a decade, questioning the reliability of this model. One
of the sources of uncertainty could be in the treatment of the transport of
radiation from the solar core to the surface. In this letter, we use the new
OPAS opacity tables, recently available for solar modelling, to address this
issue. We discuss first the peculiarities of these tables, then we quantify
their impact on the solar sound speed and density profiles using the reduced
OPAS tables taken on the grids of the OPAL ones. We use the two evolution codes
MESA and CLES that led to similar conclusions in the solar radiative zone. In
comparison to commonly used OPAL opacity tables, the new solar models computed,
for the most recent photospheric composition, with OPAS tables present
improvements in the location of the base of the convective zone and in the
description of the solar radiative zone in comparison to the helioseismic
observations, even if the differences in the Rosseland mean opacity do not
exceed 6 %. We finally carry out a comparison to a solar model computed with
the OP opacity tables.
