Bumpy Superluminous Supernovae Powered by Magnetar-star Binary Engine
arxiv(2024)
摘要
Wolf-Rayet stars in close binary systems can be tidally spun up by their
companions, potentially leaving behind fast-spinning highly-magnetized neutron
stars, known as “magnetars", after core collapse. These newborn magnetars can
transfer rotational energy into heating and accelerating the ejecta, producing
hydrogen-poor superluminous supernovae (SLSNe). In this Letter, we
propose that the magnetar wind of the newborn magnetar could significantly
evaporate its companion star, typically a main-sequence or helium star, if the
binary system is not disrupted by the SN kick. The subsequent heating and
acceleration of the evaporated star material along with the SN ejecta by the
magnetar wind can produce a post-peak bump in the SLSN lightcurve. Our model
can reproduce the primary peaks and post-peak bumps of four example observed
multiband SLSN lightcurves, revealing that the mass of the evaporated material
could be ∼0.4-0.6 M_⊙ if the material is hydrogen-rich. We suggest
that the magnetar could induce strongly enhanced evaporation from its companion
star near the pericenter if the orbit of the post-SN binary is highly
eccentric, ultimately generating multiple post-peak bumps in the SLSN
lightcurves. This “magnetar-star binary engine" model offers a possible
explanation for the evolution of polarization, along with the origin and
velocity broadening of late-time hydrogen or helium broad spectral features
observed in some bumpy SLSNe. The diversity in the lightcurves and spectra of
SLSNe may be attributed to the wide variety of companion stars and post-SN
binary systems.
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