Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:0809.3412)
· References in the article
· Citations to the Article (11) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Gravitational waves from resolvable massive black hole binary systems and observations with Pulsar Timing Arrays
Authors:
Sesana, A.; Vecchio, A.; Volonteri, M.
Affiliation:
AA(Center for Gravitational Wave Physics, The Pennsylvania State University, University Park, PA 16802, USA), AB(School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT), AC(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 394, Issue 4, pp. 2255-2265. (MNRAS Homepage)
Publication Date:
04/2009
Origin:
MNRAS
MNRAS Keywords:
black hole physics , gravitational waves , pulsars: general , cosmology: theory
DOI:
10.1111/j.1365-2966.2009.14499.x
Bibliographic Code:
2009MNRAS.394.2255S

Abstract

Massive black holes are key components of the assembly and evolution of cosmic structures, and a number of surveys are currently on going or planned to probe the demographics of these objects and to gain insight into the relevant physical processes. Pulsar Timing Arrays (PTAs) currently provide the only means to observe gravitational radiation from massive black hole binary systems with masses >~107Msolar. The whole cosmic population produces a stochastic background that could be detectable with upcoming PTAs. Sources sufficiently close and/or massive generate gravitational radiation that significantly exceeds the level of the background and could be individually resolved. We consider a wide range of massive black hole binary assembly scenarios, investigate the distribution of the main physical parameters of the sources, such as masses and redshift, and explore the consequences for PTAs observations. Depending on the specific massive black hole population model, we estimate that on average at least one resolvable source produces timing residuals in the range ~5-50ns. PTAs, and in particular the future Square Kilometre Array, can plausibly detect these unique systems, although the events are likely to be rare. These observations would naturally complement on the high-mass end of the massive black hole distribution function future surveys carried out by the Laser Interferometer Space Antenna.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints