  Various remote sensing observations have been used so far to probe the
turbulent properties of the solar wind. Using the recently reported density
modulation indices that are derived using angular broadening observations of
Crab Nebula during 1952 - 2013, we measured the solar wind proton heating using
the kinetic $\rm Alfv\acute{e}n$ wave dispersion equation. The estimated
heating rates vary from $\approx 1.58 \times 10^{-14}$ to $1.01 \times 10^{-8}
~\rm erg~ cm^{-3}~ s^{-1}$ in the heliocentric distance range 5 - 45 $\rm
R_{\odot}$. Further, we found that heating rates vary with the solar cycle in
correlation with density modulation indices. The models derived using in-situ
measurements (for example, electron/proton density, temperature, and magnetic
field) that the recently launched Parker Solar Probe observes (planned closest
perihelia $\rm 9.86~ R_{\odot}$ from the center of the Sun) are useful in the
estimation of the turbulent heating rate precisely. Further, we compared our
heating rate estimates with the one derived using previously reported remote
sensing and in-situ observations.
