  We developed a generic formalism to estimate the event rate and the redshift
distribution of Fast Radio Bursts (FRBs) in our previous publication (Bera et
al. 2016), considering FRBs are of an extragalactic origin. In this paper we
present (a) the predicted pulse widths of FRBs by considering two different
scattering models, (b) the minimum total energy required to detect events, (c)
the redshift distribution and (d) the detection rates of FRBs for the Ooty Wide
Field Array (OWFA). The energy spectrum of FRBs is modelled as a power law with
an exponent $-\alpha$ and our analysis spans a range $-3\leq \alpha \leq 5$. We
find that OWFA will be capable of detecting FRBs with $\alpha\geq 0$. The
redshift distribution and the event rates of FRBs are estimated by assuming two
different energy distribution functions; a Delta function and a Schechter
luminosity function with an exponent $-2\le \gamma \le 2$. We consider an
empirical scattering model based on pulsar observations (model I) as well as a
theoretical model (model II) expected for the intergalactic medium. The
redshift distributions peak at a particular redshift $z_p$ for a fixed value of
$\alpha$, which lie in the range $0.3\leq z_p \leq 1$ for the scattering model
I and remain flat and extend up to high redshifts ($z\lesssim 5$) for the
scattering model II.
