Minutes-delayed Jets from a Neutron Star Companion in Core-collapse Supernovae

Noam Soker

doi:10.3847/1538-4357/abb809

Minutes-delayed Jets from a Neutron Star Companion in Core-collapse Supernovae

Noam Soker^*

^*Corresponding author for this work

Physics

Research output: Contribution to journal › Article › peer-review

Abstract

This paper presents cases in which a neutron star (NS; or a black hole) companion to a type-Ib or type-Ic (stripped-envelope) core-collapse supernova (CCSN) accretes mass from the explosion ejecta and launches jets minutes to hours after explosion. The NS orbits at a pre-explosion radius of a ≃ 1-5 R o˙. When the ejecta velocity drops to , the ejecta gas that the NS accretes possesses sufficient specific angular momentum to form an accretion disk around the NS. The NS accretes a fraction of of the ejecta mass through an accretion disk over a time period of 10 minutes-few hr. If the jets carry about 10% of the accretion energy, then their total energy is a fraction of about 0.003-0.03 of the kinetic energy of the ejecta. The implications of these jets from an NS (or a black hole) companion to a CCSN are the shaping of the inner ejecta to have a bipolar morphology, energizing the light curve of the CCSN, and in some cases the possible enrichment of the inner ejecta with r-process elements.

Original language	English
Article number	130
Journal	Astrophysical Journal
Volume	902
Issue number	2
DOIs	https://doi.org/10.3847/1538-4357/abb809
State	Published - 20 Oct 2020

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abstract = "This paper presents cases in which a neutron star (NS; or a black hole) companion to a type-Ib or type-Ic (stripped-envelope) core-collapse supernova (CCSN) accretes mass from the explosion ejecta and launches jets minutes to hours after explosion. The NS orbits at a pre-explosion radius of a ≃ 1-5 R o˙. When the ejecta velocity drops to , the ejecta gas that the NS accretes possesses sufficient specific angular momentum to form an accretion disk around the NS. The NS accretes a fraction of of the ejecta mass through an accretion disk over a time period of 10 minutes-few hr. If the jets carry about 10% of the accretion energy, then their total energy is a fraction of about 0.003-0.03 of the kinetic energy of the ejecta. The implications of these jets from an NS (or a black hole) companion to a CCSN are the shaping of the inner ejecta to have a bipolar morphology, energizing the light curve of the CCSN, and in some cases the possible enrichment of the inner ejecta with r-process elements.",

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Minutes-delayed Jets from a Neutron Star Companion in Core-collapse Supernovae

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