Postexplosion Positive Jet-feedback Activity in Inner Ejecta of Core Collapse Supernovae

Abstract

We conduct three-dimensional hydrodynamical simulations of weak jets that we launch into a core collapse supernova (CCSN) ejecta half an hour after the explosion and find that the interaction of the fast jets with the CCSN ejecta creates high-pressure zones that induce a backflow that results in mass accretion onto the newly born neutron star. In cases of weak jets, with a total power of ≈1045–1046 erg, the backflow mass accretion might power them up to more energetic jets by an order of magnitude. In total, the jets of the two postexplosion jet-launching episodes have enough energy to influence the morphology of the very inner ejecta, with a mass of ≈0.1 M ⊙. Our results imply that in some, probably a minority of, CCSN remnants the very inner regions might display a bipolar structure that results from postexplosion weak jets. The regions outside this part might display the morphology of jittering jets.

Pre-explosion, explosion, and post-explosion jets in supernova SN 2019zrk

“…I concluded that late (post-explosion) jets are the most likely explanation for the bump. Late sources of accreted mass that might lead to late jet-launching include fallback after the explosion (e.g., Della Valle et al 2006;Moriya et al 2010;Akashi & Soker 2022;Pellegrino et al 2022), feeding the young NS (or BH) by an inflated main sequence companion (e.g., Ogata, Hirai, & Hijikawa 2021;Hober, Bear, & Soker 2022), and the feeding of a pre-existing NS/BH by the CCSN ejecta (e.g., Fryer, Rueda, & Ruffini 2014;Becerra et al 2015Becerra et al , 2019Akashi & Soker 2020). At this time I leave all possibilities open for SN 2019zrk, as it is not clear whether it was a CCSN event or a CEJSN event.…”