Double common envelope jets supernovae (CEJSNe) by triple-star systems. (arXiv:2103.03168v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Soker_N/0/1/0/all/0/1">Noam Soker</a> (Technion, Israel)
I propose a new type of common envelope jets supernova (CEJSN) events where
instead of a single neutron star (NS; or a black hole; BH) a tight binary
system of a NS and a main sequence star enters a common envelope evolution
(CEE) with a red supergiant. The NS and the main sequence star of the tight
binary system merge inside the red supergiant envelope and enter a CEE of their
own. The NS accretes some mass through an accretion disk and launches jets that
explodes the main sequence star. I estimate that the two jets that the NS
launches at this phase carry an energy of ~10^{52} erg, about the same order of
magnitude as the energy that the jets will carry when the NS or its BH remnant
will enter the core in a later phase. For that, I term the entire event a
double CEJSN. The outcome of the double CEJSN is a very long, months to years,
and very energetic event, a total energy of ~10^{52} – 10^{53} erg, that will
be observationally classified as a peculiar super-energetic event. I crudely
estimate that new transient surveys should detect about one CEJSN event from a
triple star system per year. I end by listing some other types of CEJSN events
in triple star systems.
I propose a new type of common envelope jets supernova (CEJSN) events where
instead of a single neutron star (NS; or a black hole; BH) a tight binary
system of a NS and a main sequence star enters a common envelope evolution
(CEE) with a red supergiant. The NS and the main sequence star of the tight
binary system merge inside the red supergiant envelope and enter a CEE of their
own. The NS accretes some mass through an accretion disk and launches jets that
explodes the main sequence star. I estimate that the two jets that the NS
launches at this phase carry an energy of ~10^{52} erg, about the same order of
magnitude as the energy that the jets will carry when the NS or its BH remnant
will enter the core in a later phase. For that, I term the entire event a
double CEJSN. The outcome of the double CEJSN is a very long, months to years,
and very energetic event, a total energy of ~10^{52} – 10^{53} erg, that will
be observationally classified as a peculiar super-energetic event. I crudely
estimate that new transient surveys should detect about one CEJSN event from a
triple star system per year. I end by listing some other types of CEJSN events
in triple star systems.
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