Gravitational Waves from Stellar Mass Black Holes Around SgrA*. (arXiv:1903.02579v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Emami_R/0/1/0/all/0/1">Razieh Emami</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loeb_A/0/1/0/all/0/1">Abraham Loeb</a> (Harvard University)
We consider the detectability of the gravitational wave (GW) signal from an
orbiting stellar-mass black hole (BH) with a mass of order 40 $M_{odot}$
around Sgr A* at the center of the Milky Way galaxy. We simulate the sinking
BHs to the center through dynamical friction and GW emission. We predict that
LISA will detect of order 10 BHs at any given time with a signal-to-noise ratio
$S/N > 10$.
We consider the detectability of the gravitational wave (GW) signal from an
orbiting stellar-mass black hole (BH) with a mass of order 40 $M_{odot}$
around Sgr A* at the center of the Milky Way galaxy. We simulate the sinking
BHs to the center through dynamical friction and GW emission. We predict that
LISA will detect of order 10 BHs at any given time with a signal-to-noise ratio
$S/N > 10$.
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