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The nonlinear dynamics of outflows driven by magnetic explosion on thesurface of a compact star is investigated through special relativisticmagnetohydrodynamic simulations. We adopt, as the initial equilibrium state, aspherical stellar object embedded in hydrostatic plasma which has a density$\rho(r) \propto r^{- \alpha}$ and is threaded by a dipole magnetic field. Theinjection of magnetic energy at the surface of compact star breaks theequilibrium and triggers a two-component outflow. At the early evolutionarystage, the magnetic pressure increases rapidly around the stellar surface,initiating a magnetically driven outflow. A strong forward shock driven outflowis then excited. The expansion velocity of the magnetically driven outflow ischaracterized by the Alfv\'en velocity on the stellar surface, and follows asimple scaling relation $v_{\rm mag} \propto {v_{\rm A}}^{1/2}$. When theinitial density profile declines steeply with radius, the strong shock isaccelerated self-similarly to relativistic velocity ahead of the magneticallydriven component. We find that it evolves according to a self-similar relation$\Gamma_{\rm sh} \propto r_{\rm sh}$, where $\Gamma_{\rm sh}$ is the Lorentzfactor of the plasma measured at the shock surface $r_{\rm sh}$. Purelyhydrodynamic process would be responsible for the acceleration mechanism of theshock driven outflow. Our two-component outflow model, which is the naturaloutcome of the magnetic explosion, can provide a better understanding of themagnetic active phenomena on various magnetized compact stars.

Special Relativistic Magnetohydrodynamic Simulation of Two-Component Outflow Powered by Magnetic Explosion on Compact Stars