
 Real extreme/intermediate mass ratio inspiral(E/IMRI) systems are likely to contain large accretion disks which could be as massive as the central supermassive black hole. Therefore, contrary to its ideal model, a real E/IMRI system contains a third important component: the accretion disk. We study the influence of these disks on the emitted GW profile and its detectability through proposed LISA observation. We use a semi-relativistic formalism in the Kerr background for the case of transonic accretion flow which is a potential candidate to describe the accretion flows around AGN. The hydrodynamic drag of the disks modified the motion of the companion as a result the emitted wave changes in amplitude and phase. We found that these changes are detectable through the last few years of observation by LISA (in some cases as small as six months) for EMRIs residing within redshift z = 1 from the detector and for the accretion rate of the primary black hole of the order of $\dot{M}=1 \dot{M}_{Edd}$. These choices of parameter values are consistent with real systems. The drag effect and hence the detectability of the emitted GW is sensitive to the hydrodynamical model of the disk. Therefore we vary the disk parameters, accretion rate and duration of observation of E/IMRIs, and find that in comparison with other disk models, transonic solution offers relatively better observable signatures in detecting the gas-riched E/IMRI’s within the LISA band. Such observations will help one to probe the nature of the accretion flow and verify various paradigms of accretion physics.

Detectability of gas-riched E/IMRI’s in LISA band: Observable signature of transonic accretion flow.

We give here a brief review of the works studying the signatures of accretion disks on the gravitational wave signals generated by extreme mass ratio binary systems of compact objects. An example of such a system is a stellar mass compact star (typically a neutron star or a black hole) orbiting a central super-massive black hole embedded in a massive accretion disk. We particularly focus on the effects produced by hydrodynamic drag of the disk on the orbiting companion and find that the drag effects produced by the disk matter are indeed capable of modifying the companion’s motion and, hence, the gravitational wave signal emitted from the system. The nature and significance of the effect depends crucially on the flow parameters of the disk, e.g. velocity, density profiles of the flow. Therefore, on one hand, one needs to incorporate these effects while theoretically modelling the gravitational wave signal emitted from such systems. On the other hand, by studying the emitted gravitational wave signals profile, one could infer about the nature of the accretion disk, which has been, till date, done only by observing the electro-magnetic signals coming from it. This multi-messenger astronomy was for the first time conceived and worked out during our research work.

Gravitational Wave Emission from Binary Mergers: Ideal Versus Real Picture

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Gravitational Wave Emission from Binary Mergers: Ideal Versus Real Picture