  Utilizing multi-wavelength dust emission maps acquired with $Herschel$, we
reconstruct local volume density and dust temperature profiles for the
prestellar cores B68 and L1689B using inverse-Abel transform based technique.
We present intrinsic radial dust temperature profiles of starless cores
directly from dust continuum emission maps disentangling the effect of
temperature variations along the line of sight which was previously limited to
the radiative transfer calculations. The reconstructed dust temperature
profiles show a significant drop in core center, a flat inner part, and a
rising outward trend until the background cloud temperature is reached. The
central beam-averaged dust temperatures obtained for B68 and L1689B are 9.3
$\pm$ 0.5 K and 9.8 $\pm$0.5 K, respectively, which are lower than the
temperatures of 11.3 K and 11.6 K obtained from direct SED fitting. The best
mass estimates derived by integrating the volume density profiles of B68 and
L1689B are 1.6 M_sol and 11 M_sol, respectively. Comparing our results for B68
with the near-infrared extinction studies, we find that the dust opacity law
adopted by the HGBS project, $\kappa_{\lambda} =0.1(\lambda/300 \mu m)^{-2}$,
agrees to within 50% with the dust extinction constraints
