  Gravastars are considered as one of the prime exotic type compact objects
which may be found at the end state of gravitational collapse of massive stars
with a view to resolve the complexities that are pertinent in case of a black
hole \cite{Mazur}-\cite{Mazur2}. In this paper, we analyse the role of charge
on the possible formation of isotropic spherically symmetric gravastar
configuration in the framework of Rastall gravity. Gravastar contains three
distinct layers {\it viz.} i) Interior region, ii) Thin shell and iii) Exterior
region. The interior region is characterised by the equation of state $p=-\rho$
that defines the repulsive outward pressure in radial direction at all points
on the thin shell. The thin shell, contains ultra-relativistic stiff fluid
which is denoted by the equation of state $p=\rho$ following Zel'dovich's
criteria \cite{Zeldovich,Zeldovich1} for cold baryonic universe, can withstand
the repulsive pressure exerted by the interior region. The exterior region is
the vacuum space-time represented by the Reissner-Nordstr$\ddot{o}$m solution.
In view of the above specifications, we construct and analyse a charged
gravastar model in Rastall theory of gravity which represents several salient
features. The basic physical attributes, {\it viz.} proper length, energy,
entropy and equation of state parameter of the shell are investigated. In this
model, it is interesting to note that for large value of the radius of
hyper-surface (R) the EoS parameter of the thin shell corresponds to dark
energy EoS with $\mathcal{W}(R)\rightarrow-1$. However, for small value of $R$
the EoS parameter $\mathcal{W}(R)\rightarrow0$, defines a dust shell. The
stability of the model is ensured through the study of gravitational surface
redshift and maximisation of shell entropy within the framework of Rastall
theory of gravity.
