Models for fast-evolving supernova KSN 2015K: light curves of explosions of Super-AGB progentors. (arXiv:1811.09139v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Tolstov_A/0/1/0/all/0/1">Alexey Tolstov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nomoto_K/0/1/0/all/0/1">Ken'ichi Nomoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sorokina_E/0/1/0/all/0/1">Elena Sorokina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blinnikov_S/0/1/0/all/0/1">Sergei Blinnikov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tominaga_N/0/1/0/all/0/1">Nozomu Tominaga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Taniguchi_Y/0/1/0/all/0/1">Yoshiaki Taniguchi</a>
Recent supernova searches revealed a number of fast-evolving luminous
transients. We perform radiation hydrodynamical simulations of light curves of
several models of supernova from super–asymptotic giant branch (super-AGB,
SAGB) stars with low mass envelopes ($M_{rm env}$ $sim$ $0.05-1.25$
$M_{odot}$). The differences in the light curves found among the models are
used to link the observed events to the most appropriate models. In particular,
we propose that KSN 2015K is an electron-capture supernova with a faint tail
that might be influenced by the spin-down luminosity of a newborn Crab-like
pulsar. Our fits indicate an ejecta mass of $0.02-0.05$ $M_{odot}$, a
circumstellar medium (CSM) mass of $0.10-0.12$ $M_{odot}$, a radius of the CSM
photosphere $sim$ 10$^{14}$ cm, a kinetic energy of $sim$ 3 $times$
10$^{50}$ erg, a photospheric velocity $v_{rm ph} gtrsim 10,000$ km s$^{-1}$
and a pulsar total spin energy ($2.5-4$) $times$ 10$^{49}$ erg.
Recent supernova searches revealed a number of fast-evolving luminous
transients. We perform radiation hydrodynamical simulations of light curves of
several models of supernova from super–asymptotic giant branch (super-AGB,
SAGB) stars with low mass envelopes ($M_{rm env}$ $sim$ $0.05-1.25$
$M_{odot}$). The differences in the light curves found among the models are
used to link the observed events to the most appropriate models. In particular,
we propose that KSN 2015K is an electron-capture supernova with a faint tail
that might be influenced by the spin-down luminosity of a newborn Crab-like
pulsar. Our fits indicate an ejecta mass of $0.02-0.05$ $M_{odot}$, a
circumstellar medium (CSM) mass of $0.10-0.12$ $M_{odot}$, a radius of the CSM
photosphere $sim$ 10$^{14}$ cm, a kinetic energy of $sim$ 3 $times$
10$^{50}$ erg, a photospheric velocity $v_{rm ph} gtrsim 10,000$ km s$^{-1}$
and a pulsar total spin energy ($2.5-4$) $times$ 10$^{49}$ erg.
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