科研之友
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摘要
Fast-spinning strongly magnetized newborn neutron stars (NSs), including nascent magnetars, are popularly implemented as the engine of luminous stellar explosions. Here, we consider the scenario that they power various stripped-envelope (SE) supernovae (SNe), not only superluminous SNe Ic but also broad-line (BL) SNe Ibc and possibly some ordinary SNe Ibc. This scenario is also motivated by the hypothesis that Galactic magnetars largely originate from fast-spinning NSs as remnants of SE SNe. By consistently modeling the energy injection from magnetized wind and Ni-56 decay, we show that proto-NSs with greater than or similar to 10 ms rotation and a poloidal magnetic field of B-dip greater than or similar to 5 x 10(14) G can be harbored in ordinary SNe Ibc. On the other hand, millisecond proto-NSs can solely power BL SNe Ibc if they are born with B-dip greater than or similar to 5 x 10(14) G and superluminous SNe Ic with B-dip greater than or similar to 10(13) G. Then, we study how multi-messenger emission can be used to discriminate such pulsar-driven SN models from other competitive scenarios. First, high-energy X-ray and gamma-ray emission from embryonic pulsar wind nebulae can probe the underlying newborn pulsar. Follow-up observations of SE SNe using NuSTAR similar to 50-100 days after the explosion are strongly encouraged for nearby objects. We also discuss possible effects of gravitational waves (GWs) on the spin-down of proto-NSs. If millisecond proto-NSs with B-dip < a few x 10(13) G emit GWs through, e.g., non-axisymmetric rotation deformed by the inner toroidal fields of B-t greater than or similar to 10(16) G, the GW signal can be detectable from ordinary SNe Ibc in the Virgo cluster by Advanced LIGO, Advanced Virgo, and KAGRA.
- 出版日期2016-2-10
