Modelling light curves of bipolar core collapse supernovae from the equatorial plane. (arXiv:2007.14021v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Soker_N/0/1/0/all/0/1">Noam Soker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kaplan_N/0/1/0/all/0/1">Noa Kaplan</a> (Technion, Israel)
We use the two-components bipolar toy model of core collapse supernova (CCSN)
ejecta to fit the rapid decline from maximum luminosity in the light curve of
the type IIb CCSN SN2018gk. In this toy model we use a template light curve
from a different CCSN that is similar to SN2018gk, but that has no rapid drop
in its light curve. The bipolar morphology that we model with a polar ejecta
and an equatorial ejecta increases the maximum luminosity and causes a steeper
decline for an equatorial observer, relative to a similar spherical explosion.
The total energy and mass of our toy model for SN2018gk are E=5e51 erg and
M=2.7Mo. This explosion energy is more than what a neutrino-driven explosion
mechanism can supply, implying that jets exploded SN2018gk. These energetic
jets likely shaped the ejecta to a bipolar morphology, as our toy model
requires. We crudely estimate that f=2-5% of all CCSNe show this behavior, most
being hydrogen deficient (stripped-envelope) CCSNe, as we observe them from the
equatorail plane. We estimate the overall fraction of CCSNe that have a
pronounced bipolar morphology to be 5-15% of all CCSNe.
We use the two-components bipolar toy model of core collapse supernova (CCSN)
ejecta to fit the rapid decline from maximum luminosity in the light curve of
the type IIb CCSN SN2018gk. In this toy model we use a template light curve
from a different CCSN that is similar to SN2018gk, but that has no rapid drop
in its light curve. The bipolar morphology that we model with a polar ejecta
and an equatorial ejecta increases the maximum luminosity and causes a steeper
decline for an equatorial observer, relative to a similar spherical explosion.
The total energy and mass of our toy model for SN2018gk are E=5e51 erg and
M=2.7Mo. This explosion energy is more than what a neutrino-driven explosion
mechanism can supply, implying that jets exploded SN2018gk. These energetic
jets likely shaped the ejecta to a bipolar morphology, as our toy model
requires. We crudely estimate that f=2-5% of all CCSNe show this behavior, most
being hydrogen deficient (stripped-envelope) CCSNe, as we observe them from the
equatorail plane. We estimate the overall fraction of CCSNe that have a
pronounced bipolar morphology to be 5-15% of all CCSNe.
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