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$N-$body dynamics of Intermediate mass-ratio inspirals in globular clusters | | Carl-Johan Haster
; Fabio Antonini
; Vicky Kalogera
; Ilya Mandel
; | | Date: |
22 Jun 2016 | | Abstract: | The intermediate mass-ratio inspiral of a stellar compact remnant into an
intermediate mass black hole (IMBH) can produce a gravitational wave (GW)
signal that is potentially detectable by current ground-based GW detectors
(e.g., Advanced LIGO) as well as by planned space-based interferometers (e.g.,
eLISA). Here, we present results from a direct integration of the
post-Newtonian $N$-body equations of motion describing stellar clusters
containing an IMBH and a population of stellar-mass black holes (BHs) and solar
mass stars. We take particular care to simulate the dynamics closest to the
IMBH, including post-Newtonian effects up to order $2.5$. Our simulations show
that the IMBH readily forms a binary with a BH companion. This binary is
gradually hardened by transient 3-body or 4-body encounters, leading to
frequent substitutions of the BH companion, while the binary’s eccentricity
experiences large amplitude oscillations due to the Lidov-Kozai resonance. We
also demonstrate suppression of these resonances by the relativistic precession
of the binary orbit. We find an intermediate mass-ratio inspiral in one of the
12 cluster models we evolved for $sim 100$ Myr. This cluster hosts a $100
M_odot$ IMBH embedded in a population of 32 $10M_odot$ BH and 32,000
$1M_odot$ stars. At the end of the simulation, after $sim 100$ Myr of
evolution, the IMBH merges with a BH companion. The IMBH--BH binary inspiral
starts in the eLISA frequency window ($gtrsim 1
m mHz$) when the binary
reaches an eccentricity $1-esimeq 10^{-3}$. After $simeq 10^5$ years the
binary moves into the LIGO frequency band with a negligible eccentricity. We
comment on the implications for GW searches, with a possible detection within
the next decade. | | Source: | arXiv, 1606.7097 | | Services: | Forum | Review | PDF | Favorites | |
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