Probe for Type Ia supernova progenitor in decihertz gravitational wave astronomy. (arXiv:1910.01063v1 [astro-ph.HE])

Probe for Type Ia supernova progenitor in decihertz gravitational wave astronomy. (arXiv:1910.01063v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kinugawa_T/0/1/0/all/0/1">Tomoya Kinugawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takeda_H/0/1/0/all/0/1">Hiroki Takeda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yamaguchi_H/0/1/0/all/0/1">Hiroya Yamaguchi</a>

It is generally believed that Type Ia supernovae are thermonuclear explosions
of carbon-oxygen white dwarfs (WDs). However, there is currently no consensus
regarding the events leading to the explosion. A binary WD (WD-WD) merger is a
possible progenitor of Type Ia supernovae. Space-based gravitational wave (GW)
detectors with great sensitivity in the decihertz range like DECIGO can observe
WD-WD mergers directly. Therefore, access to the deci-Hz band of GWs would
enable multi-messenger observations of Type Ia supernovae to constrain their
progenitor and explosion mechanism. In this paper, we consider the event rate
of WD-WD mergers and minimum detection range to observe one WD-WD merger per
year, using nearby galaxy catalog and the relation between the Ia supernova and
the host galaxy. Furthermore, we calculate the DECIGO’s ability to localize
WD-WD mergers and to determine the masses of binary mergers. We estimate that
if the deci-Hz GW observatory can detect the GW whose amplitude is
$hsim10^{-20}[rm Hz^{-1/2}]$ at 0.1 Hz, 1000 times higher than the detection
limit of DECIGO. In fact, DECIGO is expected to detect WD-WD
($1M_{odot}-1M_{odot}$) mergers within $z=0.115$,corresponding to the
detection rate of $sim20000,rm yr^{-1}$, and identify the host galaxy of
WD-WD mergers for $sim8000$ WD-WDs only by the GW detection.

It is generally believed that Type Ia supernovae are thermonuclear explosions
of carbon-oxygen white dwarfs (WDs). However, there is currently no consensus
regarding the events leading to the explosion. A binary WD (WD-WD) merger is a
possible progenitor of Type Ia supernovae. Space-based gravitational wave (GW)
detectors with great sensitivity in the decihertz range like DECIGO can observe
WD-WD mergers directly. Therefore, access to the deci-Hz band of GWs would
enable multi-messenger observations of Type Ia supernovae to constrain their
progenitor and explosion mechanism. In this paper, we consider the event rate
of WD-WD mergers and minimum detection range to observe one WD-WD merger per
year, using nearby galaxy catalog and the relation between the Ia supernova and
the host galaxy. Furthermore, we calculate the DECIGO’s ability to localize
WD-WD mergers and to determine the masses of binary mergers. We estimate that
if the deci-Hz GW observatory can detect the GW whose amplitude is
$hsim10^{-20}[rm Hz^{-1/2}]$ at 0.1 Hz, 1000 times higher than the detection
limit of DECIGO. In fact, DECIGO is expected to detect WD-WD
($1M_{odot}-1M_{odot}$) mergers within $z=0.115$,corresponding to the
detection rate of $sim20000,rm yr^{-1}$, and identify the host galaxy of
WD-WD mergers for $sim8000$ WD-WDs only by the GW detection.

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