Event Rate for Extreme Mass Ratio Burst Signals in the Laser Interferometer Space Antenna Band

Details Event Rate for Extreme Mass Ratio Burst Signals in the Laser Interferometer Space Antenna Band Event Rate for Extreme Mass Ratio Burst Signals in the Laser Interferometer Space Antenna Band

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006apj...649l..25r&link_type=abstract

The Astrophysical Journal, Volume 649, Issue 1, pp. L25-L28.

Physics

10

Black Hole Physics, Galaxy: Nucleus, Gravitational Waves, Stellar Dynamics

Scientific paper

Stellar mass compact objects in short-period (P<~103 s) orbits about a 104.5-107.5 Msolar massive black hole (MBH) are thought to be a significant continuous-wave source of gravitational radiation for the ESA/NASA Laser Interferometer Space Antenna (LISA) gravitational wave detector. These extreme mass ratio inspiral sources began in long-period, nearly parabolic orbits that have multiple close encounters with the MBH. The gravitational radiation emitted during the close encounters may be detectable by LISA as a gravitational wave burst if the characteristic passage timescale is less than 105 s. Scaling a static, spherical model to the size and mass of the Milky Way bulge, we estimate an event rate of ~15 yr-1 for such burst signals, detectable by LISA with signal-to-noise ratio greater than 5, originating in our Galaxy. When extended to include Virgo Cluster galaxies, our estimate increases to a gravitational wave burst rate of ~18 yr-1. We conclude that these extreme mass ratio burst sources may be a steady and significant source of gravitational radiation in the LISA data streams.

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