Late Jets, Early Sparks: Illuminating the Premaximum Bumps in Superluminous Supernovae

TL;DR

This paper uses 3D relativistic hydrodynamical simulations to show how jets from central engines in superluminous supernovae can produce early bumps in their light curves, matching observed features and suggesting a jet-driven origin.

Contribution

It demonstrates that relativistic jets can break through supernova ejecta and produce observable early bumps in SLSN light curves, providing a new explanation for these features.

Findings

Jet successfully breaks through ejecta and powers UV/optical emission

Cocoon emission matches observed SLSN bumps in luminosity and temperature

High radiative efficiency due to low optical depths in expanded ejecta

Abstract

Superluminous supernovae (SLSNe) radiate $\gtrsim 10-100$ times more energy than ordinary stellar explosions, implicating a novel power source behind these enigmatic events. One frequently discussed source, particularly for hydrogen-poor (Type I) SLSNe, is a central engine such as a millisecond magnetar or accreting black hole. Both black hole and magnetar engines are expected to channel a fraction of their luminosity into a collimated relativistic jet. Using 3D relativistic hydrodynamical simulations, we explore the interaction of a relativistic jet, endowed with a luminosity $L_{\rm j}\approx10^{45.5}\,{\rm erg\,s^{-1}}$ and duration $t_{\rm eng} \approx 10\,{\rm days}$ compatible with those needed to power SLSNe, launched into the envelope of the exploding star. The jet successfully breaks through the expanding ejecta, and its shocked cocoon powers ultraviolet/optical emission lasting several days after the explosion and reaching a peak luminosity $\gtrsim 10^{44}\,{\rm erg\,s^{-1}} $, corresponding to a sizable fraction of $L_{\rm j}$. This high radiative efficiency is the result of the modest adiabatic losses the cocoon experiences owing to the low optical depths of the enlarged ejecta at these late times, e.g., compared to the more compact stars in gamma-ray bursts. The luminosity and temperature of the cocoon emission match those of the ``bumps'' in SLSN light curves observed weeks prior to the optical maximum in many SLSNe. Confirmation of jet breakout signatures by future observations (e.g., days-long to weeks-long internal X-ray emission from the jet for on-axis observers, spectroscopy confirming large photosphere velocities $v/c \gtrsim 0.1$, or detection of a radio afterglow) would offer strong evidence for central engines powering SLSNe.