The Signature of a Windy Radio Supernova Progenitor in a Binary System. (arXiv:1811.11193v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Yalinewich_A/0/1/0/all/0/1">Almog Yalinewich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zwart_S/0/1/0/all/0/1">Simon Portegies Zwart</a>
Type II supernova progenitors are expected to emit copious amounts of mass in
a dense stellar wind prior to the explosion. When the progenitor is a member of
a binary, the orbital motion modulates the density of this wind. When the
progenitor explodes, the high-velocity ejecta collides with the modulated wind,
which in turn produces a modulated radio signal. In this work we derive general
analytic relations between the parameters of the radio signal modulations and
binary parameter in the limit of large member mass ratio. We use these
relations to infer the semi major axis of SN1979c and a lower bound for the
mass of the companion. We also perform numerical simulations using the AMUSE
framework of the progenitor binary system including the wind and the
gravitational effect of a companion star. The simulation output is compared to
the observed radio signal in supernova SN1979C. We find that it must have been
a binary with an orbital period of about 2000 years. If the exploding star
evolved from a $sim 18 M_{odot}$ zero-age main-sequence at solar metallicity,
we derive a companion mass of $5$ to $12 M_{odot}$ in a roughly circular
orbit.
Type II supernova progenitors are expected to emit copious amounts of mass in
a dense stellar wind prior to the explosion. When the progenitor is a member of
a binary, the orbital motion modulates the density of this wind. When the
progenitor explodes, the high-velocity ejecta collides with the modulated wind,
which in turn produces a modulated radio signal. In this work we derive general
analytic relations between the parameters of the radio signal modulations and
binary parameter in the limit of large member mass ratio. We use these
relations to infer the semi major axis of SN1979c and a lower bound for the
mass of the companion. We also perform numerical simulations using the AMUSE
framework of the progenitor binary system including the wind and the
gravitational effect of a companion star. The simulation output is compared to
the observed radio signal in supernova SN1979C. We find that it must have been
a binary with an orbital period of about 2000 years. If the exploding star
evolved from a $sim 18 M_{odot}$ zero-age main-sequence at solar metallicity,
we derive a companion mass of $5$ to $12 M_{odot}$ in a roughly circular
orbit.
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