Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Quick Search
My eDoc
Session History
Support Wiki
Direct access to
document ID:

          Institute: MPI für Gravitationsphysik     Collection: Astrophysical Relativity     Display Documents

ID: 318888.0, MPI für Gravitationsphysik / Astrophysical Relativity
Intermediate-mass black holes in colliding clusters: Implications for lower-frequency gravitational-wave astronomy
Authors:Amaro-Seoane, Pau; Freitag, Marc
Date of Publication (YYYY-MM-DD):2006-12-10
Title of Journal:Astrophysical Journal
Issue / Number:1
Start Page:L53
End Page:L56
Review Status:not specified
Audience:Not Specified
Abstract / Description:Observations suggest that star clusters often form in binaries or larger bound groups. Therefore, mergers between two clusters are likely to occur. If these clusters both harbor an intermediate-mass black hole (IMBH; 10^{2-4} Msun) in their center, they can become a strong source of gravitational waves when the black holes merge with each other. In order to understand the dynamical processes that operate in such a scenario, one has to study the evolution of the merger of two such young massive star clusters, and more specifically, their respective IMBHs. We employ the direct-summation Nbody4 numerical tool on special-purpose GRAPE6 hardware to simulate a merger of two stellar clusters each containing 63,000 particles and a central IMBH. This allows us to study accurately the orbital evolution of the colliding clusters and the embedded massive black holes. Within ~7 Myr the clusters have merged and the IMBHs constitute a hard binary. The final coalescence happens in ~10^8 yrs. The implication of our analysis is that intermediate-mass black holes merging as the result of coalescence of young dense clusters could provide a source for the Laser Interferometer Space Antenna (LISA) space-based gravitational wave detector mission. We find that interactions with stars increase the eccentricity of the IMBH binary to about 0.8. Although the binary later circularizes by emission of gravitational waves, the residual eccentricity can be detectable through its influence on the phase of the waves if the last few years of inspiral are observed.
External Publication Status:published
Document Type:Article
Communicated by:Bernhard F. Schutz
Affiliations:MPI für Gravitationsphysik/Astrophysical Relativity
MPI für Gravitationsphysik/Quantum Gravity and Unified Theories
Full Text:
You have privileges to view the following file(s):
eDoc318888arxiv.pdf  [260,00 Kb] [Comment:ArXiv]  
eDoc318888web.pdf  [231,00 Kb] [Comment:Online Journal]  
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.