  We investigate how to derive an isotropic stellar model in the framework of
mimetic gravitational theory. Recently, this theory has gained big interest due
to its difference from Einstein's general relativity (GR), especially in the
domain non-vacuum solutions. In this regard, we apply the field equation of
mimetic gravitational theory to a spherically symmetric ansatz and obtain an
over determined system of non-linear differential equations in which
differential equations are less than the unknown functions. To overcome the
over determined system we suppose a specific form of the temporal component of
the metric potential, $g_{tt}$, and assume the vanishing of the anisotropic
condition to derive the form of the spatial component of the metric, $g_{rr}$.
In this regard, we discuss the possibility to derive a stellar isotropic model
that is in agreement with observed pulsars. To examine the stability of the
isotropic model we use the Tolman-Oppenheimer-Volkoff equation and the
adiabatic index. Furthermore, we assess the model's validity by evaluating its
compatibility with a broad range of observed pulsar masses and radii. We
demonstrate that the model provides a good fit to these observations.
