Emission peaks in the light curve of core collapse supernovae by late jets. (arXiv:1907.05051v1 [astro-ph.HE])

Emission peaks in the light curve of core collapse supernovae by late jets. (arXiv:1907.05051v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kaplan_N/0/1/0/all/0/1">Noa Kaplan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soker_N/0/1/0/all/0/1">Noam Soker</a> (Technion, Israel)

We build a toy model where the central object, i.e., a newly born neutron
star or a black hole, launches jets at late times and show that these jets
might account for peaks in the light curve of some peculiar core collapse
supernovae (CCSNe) when the jets interact with the CCSN ejecta. We assume that
the central object accretes fall back material and launches two short-lived
opposite jets weeks to months after the explosion. We model each jet-ejecta
interaction as a spherically symmetric `mini explosion’ that takes place inside
the ejecta. In our toy model late jets form stronger emission peaks than early
jets. Late jets with a kinetic energy of only about one percent of the kinetic
energy of the CCSN itself might form strong emission peaks. We apply our toy
model to the brightest peak of the enigmatic CCSN iPTF14hls that has several
extra peaks in its light curve. We can fit this emission peak with our toy
model when we take the kinetic energy of the jets to be about one percent of
the CCSN energy, and the shocked ejecta mass to be about one percent of the
ejecta mass.

We build a toy model where the central object, i.e., a newly born neutron
star or a black hole, launches jets at late times and show that these jets
might account for peaks in the light curve of some peculiar core collapse
supernovae (CCSNe) when the jets interact with the CCSN ejecta. We assume that
the central object accretes fall back material and launches two short-lived
opposite jets weeks to months after the explosion. We model each jet-ejecta
interaction as a spherically symmetric `mini explosion’ that takes place inside
the ejecta. In our toy model late jets form stronger emission peaks than early
jets. Late jets with a kinetic energy of only about one percent of the kinetic
energy of the CCSN itself might form strong emission peaks. We apply our toy
model to the brightest peak of the enigmatic CCSN iPTF14hls that has several
extra peaks in its light curve. We can fit this emission peak with our toy
model when we take the kinetic energy of the jets to be about one percent of
the CCSN energy, and the shocked ejecta mass to be about one percent of the
ejecta mass.

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