  Future research studies of cosmic microwave background polarization seems
likely to provide a more improved upper bound of $r \le 0.03$ on the
tensor-to-scalar ratio(r). In our work, we have done the reheating study of
mutated hilltop inflation(MHI), a model falling in the broad category of small
field inflation. We have parameterized reheating in terms of various parameters
like reheating duration $N_{\text{rh}}$, reheating temperature $T_{\text{rh}}$
and effective equation of state $\overline{\omega }_{\text{rh}}$ using
observationally viable values of scalar power spectrum amplitude $A_{\text{s}}$
and scalar spectral index $n_{\text{s}}$. In our study, working over a range of
$\overline{\omega }_{\text{rh}}$, we found that the MHI potential is well
consistent with combined Planck and BK18 observations for $\overline{\omega
}_{\text{rh}} > 0$ within a particular range of model's parameter space and the
lower values of the model parameter in MHI generate considerably smaller r
compared to normal hilltop potential without any incompatibility of $n_s$ with
observational data, making MHI a better choice in accordance to recent and
future studies.
