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Magnetars are neutron stars born with short periods of $\sim$ 1 ms, which allow them to support an efficient $\alpha-\Omega$ dynamo, resulting in magnetic dipole fields of $10^4-10^5 \rm \ G$. This field strength is higher than that of normal neutron stars by a factor of $\sim 10^2$. They were  first proposed by \citep{Duncan_1992} \cite{Duncan_1992} to explain Soft Gamma Repeaters (SGRs). A magnetar of mass $1.4 M_{\odot}$, $R = 10 \ \rm km$, and $P = 1 \ \rm s$ has a rotational energy of   \begin{equation}  E_{\rm rot} = I \omega^2 /2 = \dfrac{1}{5}MR^2 \left(\dfrac{2\pi}{P}\right)^2 \simeq 4.4 \times 10^{51} \ \rm erg  \end{equation}  assuming a solid sphere moment of inertia as an approximation. The magnetic stresses and torques damped the rotation and release a large fraction of $E_{\rm rot}$ on the time scale of $\tau \simeq 0.6 B_{15}^{-2} (P/1 \ {\rm ms})^2$ \cite{Duncan_1992}. This amount of energy is similar to that released in the most energetic cosmic explosion like $\gamma$-ray bursts and superluminous supernovae (SLSNe), thus making magnetar an attractive candidate for the central engine that power these explosions. In the past two decades, a connection has been made between supernovae and at least some subclass of long-duration $\gamma$-ray bursts, supporting the case that they are powered by the same mechanism.