TY - JOUR
T1 - Minutes-delayed Jets from a Neutron Star Companion in Core-collapse Supernovae
AU - Soker, Noam
N1 - Publisher Copyright:
© 2020. The American Astronomical Society. All rights reserved..
Copyright:
Copyright 2020 Elsevier B.V., All rights reserved.
PY - 2020/10/20
Y1 - 2020/10/20
N2 - 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.
AB - 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.
UR - http://www.scopus.com/inward/record.url?scp=85094561340&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/abb809
DO - 10.3847/1538-4357/abb809
M3 - 文章
AN - SCOPUS:85094561340
VL - 902
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
M1 - 130
ER -