f'''(R)\big]}{\big[f(R) - 6(\dot{H} + H^2)f'(R) + 36(4H^2\dot{H} + H\ddot{H})f''(R)\big]} ~~.\end{aligned}$$ In $f(R)$ gravity theories usually we encounter three types of scale factors for accelerating and inflationary cosmological solutions. We will follow the details of [@f95; @f]. Here we will study phantom, quintessence and deSitter scale factors which are given by $$\label{mGB2}
a=\left\{
\begin{array}{ll} a_0~(t_s - t)^{-h}, ~~~~~~~~~~~~ t\leq t_s,~~~~~ h>0~~~~~~~~~~ \mbox{(phantom)} \\\\
a_0 ~t^h,~~~~~~~~~~~~~~~~~~~~~~ h>0~~~~~~~~~~~~~~~~~~~~~~~~ \mbox{(quintessence)} \\\\
a_0 ~e^{Ht},~~~~~~~~~~~~~~~~ H=\mbox{constant~~~~~~~~~~~~~~~~~~(deSitter)}
\end{array} \right.$$ With the phantom scale factor and eqn.(\[eqR\]) we get $$H = \left[\frac{h}{6(2h+1)}R\right]^{\frac{1}{2}}$$ and also $$\dot{H} = \frac{H^2}{2} ~~.$$ Recent observations constrain the value of $h$ for the phantom scale factor to be $-\infty > h \geq 7.81$ [@obser]. Similarly with the quintessence scale factor and eqn.(\[eqR\]) we get $$\label{quin1}
H = \left[\frac{h}{6(2h-1)}R\right]^{\frac{1}{2}}$$ and also $$\label{quin2}
\dot{H} = -\frac{H^2}{2} ~~.$$ For this quintessence scale factor the value of $h$ is very close to unity [@obser]. For deSitter solution we have $H=$ constant. This scale factor is used describe the early inflationary scenario. For this case we get $$\label{conh}
H = \left(\frac{R}{12}\right)^{\frac{1}{2}} ~~.$$ Now we will try to evaluate the form of $f(R)$ for each of the scale factor mentioned above in the light of the generalized uncertainty principle (GUP). 