Help Privacy Policy Disclaimer
  Advanced SearchBrowse




Journal Article

Gravitational-wave background from compact objects embedded in AGN accretion disks


Buonanno,  Alessandra
Physics Department, University of Maryland;
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

External Resource
No external resources are shared
Fulltext (restricted access)
There are currently no full texts shared for your IP range.
Fulltext (public)

(Preprint), 474KB

(Any fulltext), 563KB

Supplementary Material (public)
There is no public supplementary material available

Sigl, G., Schnittman, J., & Buonanno, A. (2007). Gravitational-wave background from compact objects embedded in AGN accretion disks. Physical Review D, 75: 024034. doi:10.1103/PhysRevD.75.024034.

Cite as: https://hdl.handle.net/11858/00-001M-0000-0018-D7A8-8
We consider a model in which massive stars form in a self-gravitating accretion disk around an active galactic nucleus (AGN). These stars may evolve and collapse to form compact objects on a time scale shorter than the accretion time, thus producing an important family of sources for LISA. Assuming the compact object formation/inspiral rate is proportional to the steady-state gas accretion rate, we use the intrinsic hard X-ray AGN luminosity function to estimate expected event rates and signal strengths. We find that these sources will produce a continuous low-frequency (<~ mHz) background detectable by LISA if more than 1% of the accreted matter is in the form of compact objects. For compact objects with masses >~ 10 solar masses the last stages of the inspiral events should be resolvable above a few mHz, with rates as high as a few hundred per year.