scholarly journals Self-force gravitational waveforms for extreme- and intermediate-mass-ratio inspirals

2012 ◽  
Vol 86 (8) ◽  
Author(s):  
Kristen A. Lackeos ◽  
Lior M. Burko
Keyword(s):  
Mass Ratio ◽  
Intermediate Mass ◽  
Self Force

scholarly journals Dark Matter: An Efficient Catalyst for Intermediate-mass-ratio-inspiral Events

2019 ◽  
Vol 874 (1) ◽  
pp. 34 ◽  
Author(s):  
Xiao-Jun Yue ◽  
Wen-Biao Han ◽  
Xian Chen
Keyword(s):  
Dark Matter ◽  
Mass Ratio ◽  
Intermediate Mass ◽  
Efficient Catalyst

scholarly journals Probing gas disc physics with LISA: simulations of an intermediate mass ratio inspiral in an accretion disc

2019 ◽  
Vol 486 (2) ◽  
pp. 2754-2765 ◽  
Author(s):  
A M Derdzinski ◽  
D D’Orazio ◽  
P Duffell ◽  
Z Haiman ◽  
A MacFadyen
Keyword(s):  
Small Deviation ◽  
Compact Object ◽  
Accretion Disc ◽  
Mass Ratio ◽  
Intermediate Mass ◽  
Laser Interferometer Space Antenna ◽  
Total Phase ◽  
Accretion Rates ◽  
Hydrodynamical Simulations ◽  
And Migration

Abstract The coalescence of a compact object with a $10^{4}\hbox{--}10^{7}\, {\rm M_\odot }$ supermassive black hole (SMBH) produces mHz gravitational waves (GWs) detectable by the future Laser Interferometer Space Antenna (LISA). If such an inspiral occurs in the accretion disc of an active galactic nucleus (AGN), the gas torques imprint a small deviation in the GW waveform. Here, we present two-dimensional hydrodynamical simulations with the moving-mesh code disco of a BH inspiraling at the GW rate in a binary system with a mass ratio q = M2/M1 = 10−3, embedded in an accretion disc. We assume a locally isothermal equation of state for the gas (with Mach number $\mathcal {M}=20$) and implement a standard α-prescription for its viscosity (with α = 0.03). We find disc torques on the binary that are weaker than in previous semi-analytic toy models, and are in the opposite direction: the gas disc slows down, rather than speeds up the inspiral. We compute the resulting deviations in the GW waveform, which scale linearly with the mass of the disc. The SNR of these deviations accumulates mostly at high frequencies, and becomes detectable in a 5 yr LISA observation if the total phase shift exceeds a few radians. We find that this occurs if the disc surface density exceeds $\Sigma _0 \gtrsim 10^{2-3}\rm g\, cm^{-2}$, as may be the case in thin discs with near-Eddington accretion rates. Since the characteristic imprint on the GW signal is strongly dependent on disc parameters, a LISA detection of an intermediate mass ratio inspiral would probe the physics of AGN discs and migration.

scholarly journals Prospects for Detection of Gravitational Waves from Intermediate-Mass-Ratio Inspirals

2007 ◽  
Vol 99 (20) ◽  
Author(s):  
Duncan A. Brown ◽  
Jeandrew Brink ◽  
Hua Fang ◽  
Jonathan R. Gair ◽  
Chao Li ◽  
...  
Keyword(s):  
Gravitational Waves ◽  
Mass Ratio ◽  
Intermediate Mass
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