Observational signatures of stellar explosions driven by relativistic jets

TL;DR

This paper investigates the observational signatures of stellar explosions driven by relativistic jets, revealing a universal flat velocity distribution and implications for energy distribution between supernovae and gamma-ray bursts.

Contribution

It introduces the concept of a universal flat energy distribution in jet-driven explosions and compares observational signatures to data, challenging the idea that jets alone cause SN/GRB events.

Findings

Jet-driven explosions produce a flat energy distribution across proper velocities.

The velocity range for typical GRB parameters is approximately 0.03-3 in Lorentz factor units.

SN/GRB events involve two energy channels: a quasi-spherical component and a collimated jet component.

Abstract

The role of relativistic jets in unbinding the stellar envelope during a supernova (SN) associated with a gamma-ray burst (GRB) is unclear. To study that, we explore observational signatures of stellar explosions that are driven by jets. We focus on the final velocity distribution of the outflow in such explosions and compare its observational imprints to SN/GRB data. We find that jet driven explosions produce an outflow with a flat distribution of energy per logarithmic scale of proper velocity. The flat distribution seems to be universal as it is independent of the jet and the progenitor properties that we explored. The velocity range of the flat distribution for typical GRB parameters is $\gamma\beta \approx 0.03-3$, where $\gamma$ is the outflow Lorentz factor and $\beta$ is its dimensionless velocity. A flat distribution is seen also for collimated choked jets where the highest outflow velocity decreases with the depth at which the jet is choked. Comparison to observations of SN/GRBs rules out jets as the sole explosion source in these events. Instead, in SN/GRB the collapsing star must deposit its energy into two channels - a quasi-spherical (or wide angle) channel and a narrowly collimated one. The former carries most of the energy and is responsible for the SN sub-relativistic ejecta while the latter carries 0.01-0.1 of the total outflow energy and is the source of the GRB. Intriguingly, the same two channels, with a similar energy ratio, were seen in the binary neutron star merger GW170817, suggesting that similar engines are at work in both phenomena.