Multi-messenger tests for fast-spinning newborn pulsars embedded in stripped-envelope supernovae
- Department of Astronomy, Department of Physics, Theoretical Astrophysics Center, University of California, Berkeley, Berkeley, CA 94720 (United States)
- School of Natural Sciences, Institute for Advanced Study, 1 Einstein Dr., Princeton NJ 08540 (United States)
- Department of Physics, Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027 (United States)
- Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto, 606-8502 (Japan)
- Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138 (United States)
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 {sup 56}Ni decay, we show that proto-NSs with ≳10 ms rotation and a poloidal magnetic field of B{sub dip}≳5×10{sup 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{sub dip}≳5×10{sup 14} G and superluminous SNe Ic with B{sub dip}≳10{sup 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 ∼ 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{sub dip}
- OSTI ID:
- 22887031
- Journal Information:
- Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 818; ISSN ASJOAB; ISSN 0004-637X
- Country of Publication:
- United Kingdom
- Language:
- English
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