  We present the results of the multi-frequency scatter time measurements for
ten radio pulsars that were relatively less studied in this regard. The
observations were performed using the Giant Meterwave Radio Telescope at the
observing frequencies of 150, 235, 325, 610 and 1060~MHz. The data we
collected, in conjunction with the results from other frequencies published
earlier, allowed us to estimate the scatter time frequency scaling indices for
eight of these sources. For PSR J1852$-$0635 it occurred that its profile
undergoes a strong evolution with frequency, which makes the scatter time
measurements difficult to perform, and for PSR J1835$-$1020 we were able to
obtain reliable pulse broadening estimates at only two frequencies. We used the
eight frequency scaling indices to estimate both: the electron density
fluctuation strengths along the respective lines-of-sight, and the standardized
amount of scattering at the frequency of 1 GHz. Combining the new data with the
results published earlier by Lewandowski et al., we revisited the scaling index
versus the dispersion measure (DM) relation, and similarly to some of the
earlier studies we show that the average value of the scaling index deviates
from the theoretical predictions for large DM pulsars, however it reaches the
magnitude claimed by L\"ohmer et al. only for pulsars with very large DMs
($>$650 pc cm$^{-3}$). We also investigated the dependence of the scattering
strength indicators on the pulsar distance, DM, and the position of the source
in the Milky Way Galaxy.
