We explore the impact of a magnetar giant flare (GF) on the neutron star (NS) crust, and the associated baryon mass ejection. We consider that sudden magnetic energy dissipation creates a thin high-pressure shell above a portion of the NS surface, which drives a relativistic shockwave into the crust, heating a fraction of these layers sufficiently to become unbound along directions unconfined by the magnetic field. We explore this process using spherically-symmetric relativistic hydrodynamical simulations. For an initial shell pressure $P_{ \rm GF}$ we find the total unbound ejecta mass roughly obeys the relation $M_{ \rm{ ej}}\sim4-9\times10^{ 24}\:\rm{ g}\:(P_{ \rm GF}/10^{ 30}\:\rm{ ergs}\:\rm{ cm}^{ -3})^{ 1.43}$. For $P_{ \rm{ GF}}\sim10^{ 30}-10^{ 31}\:\rm{ ergs}\:\rm{ cm}^{ -3}$ corresponding to the dissipation of a magnetic field of strength $\sim10^{ 15.5}-10^{ 16}\:\rm{ G}$, we find $M_{ \rm{ ej}}\sim10^{ 25}-10^{ 26}\:\rm{ g}$ with asymptotic velocities $v_{ \rm{ ej}}/c\sim0.3-0.6$ compatible with the ejecta properties inferred from the afterglow of the December 2004 GF from SGR 1806-20. Because the flare excavates crustal material to a depth characterized by an electron fraction $Y_e\approx0.40-0.46$, and is ejected with high entropy and rapid expansion timescale, the conditions are met for heavy element $r$-process nucleosynthesis via the alpha-rich freeze-out mechanism. Given an energetic GF rate of roughly once per century in the Milky Way, we find that magnetar GFs could be an appreciable heavy $r$-process source that tracks star formation. We predict that GFs are accompanied by short $\sim$minutes long, luminous $\sim10^{ 39}\:\rm{ ergs}\:\rm{ s}^{ -1}$ optical transients powered by $r$-process decay ("nova brevis"), akin to scaled-down kilonovae. Our findings also have implications for the synchrotron nebulae surrounding some repeating fast radio burst sources.
Categories: astro-ph.HE astro-ph.SR