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Abstract:
In this paper we propose a new plausible mechanism of supernova explosions specific to close
binary systems. The starting point is the common envelope phase in the evolution of a binary
consisting of a red super giant and a neutron star. As the neutron star spirals towards the center of
its companion it spins up via disk accretion. Depending on the specific angular momentum of gas
captured by the neutron star via the Bondi-Hoyle mechanism, it may reach millisecond periods
either when it is still inside the common envelope or after it has merged with the companion core.
The high accretion rate may result in strong differential rotation of the neutron star and generation
of the magnetar-strength magnetic field. The magnetar wind can blow away the common envelope
if its magnetic field is as strong as 1015 G, and can destroy the entire companion if it is as strong
as 1016 G. The total explosion energy can be comparable to the rotational energy of a millisecond
pulsar and reach 1052 erg. However, only a small amount of 56Ni is expected to be produced this
way. The result is an unusual type-II supernova with very high luminosity during the plateau
phase, followed by a sharp drop in brightness and a steep light-curve tail. The remnant is either
a solitary magnetar or a close binary involving a Wolf-Rayet star and a magnetar. When this
Wolf-Rayet star explodes this will be a third supernovae explosion in the same binary.
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