Abstract
In this article we investigate the possible effects of the presence of the massive accretion disks on the gravitational wave emission properties of the extreme or intermediate mass ratio inspiralling black hole binaries. We chose a system in which a massive black hole (M = 105 M⊙) is orbiting a central super massive black hole (M = 108 M⊙) endowed with an accretion disk. We show that the drag exerted on the companion by the disk is sufficient to reduce the coalescence time of the binary. We find that the effect of the disk will be significant in reducing the coalescence time and this has to be incorporated to interprete gravitational wave signals emitted from such systems. Same effects should be seen for smaller mass companion also albeit at a smaller scale.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
