  I study cases where 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=1-5Ro. I find that when the ejecta
velocity drops to be <1000-1500km/s 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 3e-5 to 3e-4 of the ejecta mass through
an accretion disk over a time period of 10min to few hours. If the jets carry
about ten per cent 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 a NS (or a black hole) companion to a CCSN are
the shaping the inner ejecta to have a bipolar morphology, energising the light
curve of the CCSN, and in some cases the possible enrichment of the inner
ejecta with r-process elements.
