Gravitational Waves from Supernova Mass Loss and Natal Kicks in Close Binaries. (arXiv:1909.07384v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Holgado_A/0/1/0/all/0/1">A. Miguel Holgado</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricker_P/0/1/0/all/0/1">Paul M. Ricker</a>
Some fraction of compact binaries that merge within a Hubble time may have
formed from two massive stars in isolation. For this isolated-binary formation
channel, binaries need to survive two supernova (SN) explosions in addition to
surviving common-envelope evolution. For the SN explosions, both the mass loss
and natal kicks change the orbital characteristics, producing either a bound or
unbound binary. We show that gravitational waves (GWs) may be produced not only
from the core-collapse SN process, but also from the SN mass loss and SN natal
kick during the pre-SN to post-SN binary transition. We model the dynamical
evolution of a binary at the time of the second SN explosion with an equation
of motion that accounts for the finite timescales of the SN mass loss and the
SN natal kick. From the dynamical evolution of the binary, we calculate the GW
burst signals associated with the SN natal kicks. We find that such GW bursts
may be of interest to future mid-band GW detectors like DECIGO. We also find
that the energy radiated away from the GWs emitted due to the SN mass loss and
natal kick may be a significant fraction, ${gtrsim}10%$, of the post-SN
binary’s orbital energy. For unbound post-SN binaries, the energy radiated away
in GWs tends to be higher than that of bound binaries.
Some fraction of compact binaries that merge within a Hubble time may have
formed from two massive stars in isolation. For this isolated-binary formation
channel, binaries need to survive two supernova (SN) explosions in addition to
surviving common-envelope evolution. For the SN explosions, both the mass loss
and natal kicks change the orbital characteristics, producing either a bound or
unbound binary. We show that gravitational waves (GWs) may be produced not only
from the core-collapse SN process, but also from the SN mass loss and SN natal
kick during the pre-SN to post-SN binary transition. We model the dynamical
evolution of a binary at the time of the second SN explosion with an equation
of motion that accounts for the finite timescales of the SN mass loss and the
SN natal kick. From the dynamical evolution of the binary, we calculate the GW
burst signals associated with the SN natal kicks. We find that such GW bursts
may be of interest to future mid-band GW detectors like DECIGO. We also find
that the energy radiated away from the GWs emitted due to the SN mass loss and
natal kick may be a significant fraction, ${gtrsim}10%$, of the post-SN
binary’s orbital energy. For unbound post-SN binaries, the energy radiated away
in GWs tends to be higher than that of bound binaries.
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