Simulating jets from a neutron star companion hours after a core collapse supernova

Abstract

We conduct three-dimensional hydrodynamical simulations to explore the interaction of jets that a neutron star (NS) companion to a type Ic or type Ib core collapse supernova (CCSN) launches few hours after explosion with the ejecta of the CCSN. We assume that a NS companion at 5Ro from the exploding star accretes mass from the slower inner ejecta through an accretion disk, and that the disk launches two opposite jets. Although the energy of the jets is only about one per cent of the total energy of the ejecta, it is comparable to the energy of the slower inner part of the ejecta. We find that the jets inflate one low-density hot bubble to one side of the ejecta, and that this bubble expands to influence ejecta gas up to expansion velocities of v=3500 km/s. The post-shock jets' material develops a large meridional flow and small vortexes. The boundary between the ejecta and jets' post-shock gases is unstable. The instabilities and vortexes mix jets' gas with the ejecta. We expect such a hot bubble to contribute to the light curve of CCSNe that are progenitors of binary NS systems, in particular to observers on the side of the bubble.

Accepted for publication in the ApJ

References in corpus (9)

• Formation of Double Neutron Star Systems
• Three-dimensional Models of Core-collapse Supernovae From Low-mass Progenitors With Implications for Crab
• Hypercritical Accretion, Induced Gravitational Collapse, and Binary-Driven Hypernovae
• Explaining iPTF14hls as a common envelope jets supernova
• Disk formation and jet inclination effects in Common Envelopes
• On the possible observational manifestation of supernova shock impact on the neutron star magnetosphere
• Type Ic Supernova of a 22 ${\text{M}}_{\odot }$ Progenitor
• Spectral evidence of an accretion disk in wind-fed X-ray pulsar Vela X-1 during an unusual spin-up period
• A numerical investigation of wind accretion in persistent Supergiant X-ray Binaries I - Structure of the flow at the orbital scale