SN2018kzr: a rapidly declining transient from the destruction of a white dwarf
2019
We present SN2018kzr, the fastest declining supernova-like transient, second only to the
kilonova, AT2017gfo. SN2018kzr is characterized by a peak magnitude of $M_r = -17.98$, peak bolometric luminosity of ${\sim} 1.4 \times 10^{43}$erg s$^{\mathrm{-1}}$ and a rapid decline rate of $0.48 \pm 0.03$ mag d$^{\textrm{-1}}$ in the $r$ band. The bolometric luminosity evolves too quickly to be explained by pure $^{\mathrm{56}}$Ni heating, necessitating the inclusion of an alternative powering source. Incorporating the spin-down of a magnetized
neutron staradequately describes the lightcurve and we estimate a small
ejectamass of $M_\mathrm{ej} = 0.10 \pm 0.05$ $\textrm{M}_{\odot}$. Our spectral modelling suggests the
ejectais composed of intermediate mass elements including O, Si and Mg and trace amounts of Fe-peak elements, which disfavours a binary
neutron starmerger. We discuss three explosion scenarios for SN2018kzr, given the low
ejectamass, intermediate mass element composition and the high likelihood of additional powering - core collapse of an ultra-stripped progenitor, the accretion induced collapse of a
white dwarfand the merger of a
white dwarfand
neutron star. The requirement for an alternative input energy source favours either the accretion induced collapse with
magnetarpowering or a
white dwarf-
neutron starmerger with energy from disk wind shocks.
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