# Emission peaks in the light curve of core collapse supernovae by late jets

## TL;DR

This paper proposes a toy model where late-time jets launched by the central object in core collapse supernovae can produce emission peaks in their light curves, explaining peculiar features like those observed in iPTF14hls.

## Contribution

The study introduces a novel toy model demonstrating how late jets can create observable peaks in supernova light curves, fitting peculiar supernova data.

## Key findings

- Late jets produce stronger emission peaks than early jets.
- Jets with about 1-2% of the supernova's kinetic energy can generate significant peaks.
- The model successfully fits the light curve of iPTF14hls with specific jet parameters.

## Abstract

We build a toy model where the central object, i.e., a newly born neutron star or a black hole, launches jets at late times and show that these jets might account for peaks in the light curve of some peculiar (i.e., having unusual light curves) core collapse supernovae (CCSNe) when the jets interact with the CCSN ejecta. We assume that the central object accretes fallback material and launches two short-lived opposite jets weeks to months after the explosion. We model each jet-ejecta interaction as a spherically symmetric `mini explosion' that takes place inside the ejecta. We assume that each `mini explosion' adds emission that is symmetric in time around the late peak, and with a rise in emission power that has the same slope as that of the main CCSN light curve. In total we use 12 parameters in the toy model. In our toy model late jets form stronger emission peaks than early jets. Late jets with a kinetic energy of only about one percent of the kinetic energy of the CCSN itself might form strong emission peaks. We apply our toy model to the brightest peak of the enigmatic CCSN iPTF14hls that has several extra peaks in its light curve. We can fit this emission peak with our toy model when we take the kinetic energy of the jets to be about one to two percent of the CCSN energy, and the shocked ejecta mass to be about three percent of the ejecta mass.