decreases. $n_{s}$ varies from 0.98 to 0.93 in the given range of $\beta$. The tensor-to-scalar ratio decreases from $7.4 \times 10^{-3}$ to $4.4 \times 10^{-4}$ when $\beta$ changes from -0.02 to 0.05. The magnitude of the running of the spectral index is maximum around Starobinsky model. The amplitude of the scalar primordial curvature perturbation increases as $\beta$ increases.

  -------- ------- ------- -------------- ----------------------- ------------------- ------- -------------
                                $r$        $\epsilon_{\text{V}}$   $\eta_{\text{V}}$              $A_s$
                            $(10^{-3}) $        $(10^{-4})$          $(10^{-4}) $       $$     $(10^{-9})$
   $ -20$   75.19   0.980       7.41               4.63                  0.76          -5.22      0.78
   $-10$    54.37   0.973       4.76               2.98                  1.53          -5.45      1.14
   $ -1$    42.42   0.968       3.25               2.03                  2.42          -5.51      1.61
     0      41.36   0.967       3.12               1.95                  2.54          -5.51      1.67
    $1$     40.33   0.966       2.99               1.87                  2.65          -5.51      1.73
    $10$    32.70   0.960       2.07               1.29                  3.79          -5.45      2.42
   $20 $    26.65   0.953       1.39               0.87                  5.31          -5.30      3.48
   $ 50$    16.43   0.932       0.44               0.28                  11.4          -4.49      10.0
  -------- ------- ------- -------------- ----------------------- ------------------- ------- -------------

  : These are the cosmological parameters predicted from the models when one chooses $N_{\text{e-foldings}} = 60$.[]{data-label="tab-1"}

The table.\[tab-2\] shows the viable cosmological parameters when the e-folding number is 50. The $\bphi_{i}$ varies from 57.5 to 15.3 when $\beta$ changes from -0.02 to 0.05. $\epsilon_{\text{V}}$ decreases from $5.8 