Blowouts of Nascent Wind Bubbles in Pulsar-driven Supernovae

Abstract Formation of a rapidly spinning, strongly magnetized neutron star (NS) may occur in various classes of core-collapse events. If the NS injects an amount of energy comparable to the explosion energy of the accompanying supernova (SN) before the SN ejecta becomes transparent, the nascent NS wind bubble can overtake the outer ejecta and undergo a blowout driven by hydrodynamic instabilities. Based on multidimensional numerical studies, we construct a minimal semi-analytic framework to follow the post-blowout dynamics and radiative evolution, map the blowout conditions by scanning the ejecta and NS parameters, and compute survey-ready multiband light curves. For stripped-envelope SNe with an ejecta mass of M ej ∼ 10 M ⊙ and an explosion energy of E sn ∼ 1 0 51 erg , blowout occurs for NSs with magnetic field strengths of B dip ≳ 10 13 G and spin periods of P NS ≲ a few ms. Relatively weak-field cases with B dip ≲ 10 14 G produce luminous double-peaked UV/optical light curves, as observed in the superluminous SN LSQ14bdq, while stronger-field cases with B dip ≳ 10 14 G result in hypernovae preceded by X-ray blowout precursors. We also examine weaker and lower-mass SN explosions representing ultra-stripped SNe and accretion- or merger-induced collapse events, in which blowout is more readily achieved over a broader range of NS parameters, producing fast X-ray transients with durations of 10 2–4 s and peak luminosities of 10 42–48 erg s −1 . Our results encourage coordinated UV, optical, and X-ray observations that constrain the formation of the most energetic NSs in the Universe.