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 (Gair & Glampedakis 2006; Barausse & Rezzolla 2008) 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 3 GPc from the detector and for the accretion rate of the primary black
hole of the order of M˙=1M˙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 such observations will help one to identify the nature of the
accretion flow and verify various paradigms of accretion physics.Comment: 17 pages, 17 figure