The jet-shaped pipe morphology in planetary nebulae and core-collapse supernova remnants

TL;DR

This paper compares the morphologies of planetary nebulae and supernova remnants, using simulations to argue that jets shape these structures, supporting the jittering jets explosion mechanism for core-collapse supernovae.

Contribution

It demonstrates that jet activity can produce pipe-shaped features in nebulae and supernova remnants, reinforcing the jittering jets explosion mechanism hypothesis.

Findings

Jets shape pipe-like structures in planetary nebulae and supernova remnants.

Hydrodynamic simulations reproduce observed jet-shaped morphologies.

Merging of lobes can form pipe-like features in nebulae.

Abstract

We compare images of core-collapse supernova (CCSN) remnants (CCSNRs) and jet-shaped planetary nebulae (PNe) that have a narrow, faint zone extending from side to side, termed a pipe, with a hydrodynamical numerical simulation exploding a massive star with three pairs of jets in the framework of the jittering jets explosion mechanism (JJEM), and conclude that jets shaped the pipes in these CCSNRs and PNe. We present two jet-shaped PNe with a pipe and three PNe with two opposite narrow jet-shaped lobes, and argue that in some cases the two opposite narrow lobes might merge to form one long, faint zone extending from side to side of the PN, namely, a pipe. From the qualitative similarity of the pipe morphology of the two CCSNRs we analyze with the pipe of the PNe, we suggest that jets also shaped the pipe of these CCSNRs. We strengthen this conclusion with a three-dimensional hydrodynamic simulation that reproduces two opposite narrow lobes, similar to those observed in PNe with lobes. These lobes can merge later to form a pipe. This paper is another in a series that strengthen the case for the JJEM as the primary explosion mechanism of CCSNe by comparing CCSNR morphologies with those of jet-shaped PNe.