TY - JOUR
T1 - Reviving the stalled shock by jittering jets in core collapse supernovae
T2 - Jets from the standing accretion shock instability
AU - Soker, Noam
N1 - Publisher Copyright:
© 2019 National Astronomical Observatories, CAS and IOP Publishing Ltd.
PY - 2019
Y1 - 2019
N2 - I present a scenario by which an accretion flow with alternating angular momentum on to a newly born neutron star in a core collapse supernova (CCSN) efficiently amplifies magnetic fields and by that launches jets. The accretion flow of a collapsing core on to the newly born neutron star suffers spiral standing accretion shock instability (SASI). This instability leads to a stochastically variable angular momentum of the accreted gas, which in turn forms an accretion flow with alternating directions of the angular momentum, and hence alternating shear, at any given time. I study the shear in this alternating-shear sub-Keplerian inflow in published simulations, and present a new comparison with Keplerian accretion disks. From that comparison I argue that it might be as efficient as Keplerian accretion disks in amplifying magnetic fields by a dynamo. I suggest that although the average specific angular momentum of the accretion flow is small, namely, sub-Keplerian, this alternating-shear accretion flow can launch jets with varying directions, namely, jittering jets. Neutrino heating is an important ingredient in further energizing the jets. The jittering jets locally revive the stalled accretion shock in the momentarily polar directions, and by that they explode the star. I repeat again my call for a paradigm shift from a neutrino-driven explosion of CCSNe to a jet-driven explosion mechanism that is aided by neutrino heating.
AB - I present a scenario by which an accretion flow with alternating angular momentum on to a newly born neutron star in a core collapse supernova (CCSN) efficiently amplifies magnetic fields and by that launches jets. The accretion flow of a collapsing core on to the newly born neutron star suffers spiral standing accretion shock instability (SASI). This instability leads to a stochastically variable angular momentum of the accreted gas, which in turn forms an accretion flow with alternating directions of the angular momentum, and hence alternating shear, at any given time. I study the shear in this alternating-shear sub-Keplerian inflow in published simulations, and present a new comparison with Keplerian accretion disks. From that comparison I argue that it might be as efficient as Keplerian accretion disks in amplifying magnetic fields by a dynamo. I suggest that although the average specific angular momentum of the accretion flow is small, namely, sub-Keplerian, this alternating-shear accretion flow can launch jets with varying directions, namely, jittering jets. Neutrino heating is an important ingredient in further energizing the jets. The jittering jets locally revive the stalled accretion shock in the momentarily polar directions, and by that they explode the star. I repeat again my call for a paradigm shift from a neutrino-driven explosion of CCSNe to a jet-driven explosion mechanism that is aided by neutrino heating.
KW - stars: jets
KW - stars: massive
KW - supernovae: general
UR - http://www.scopus.com/inward/record.url?scp=85072519002&partnerID=8YFLogxK
U2 - 10.1088/1674-4527/19/7/95
DO - 10.1088/1674-4527/19/7/95
M3 - 文章
AN - SCOPUS:85072519002
VL - 19
JO - Research in Astronomy and Astrophysics
JF - Research in Astronomy and Astrophysics
SN - 1674-4527
IS - 7
M1 - 95
ER -