Detecting gravity waves from binary black holes

Details Detecting gravity waves from binary black holes Detecting gravity waves from binary black holes

Aug 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989nascp3046...14w&link_type=abstract

In NASA, Relativistic Gravitational Experiments in Space p 14-17 (SEE N90-19940 12-90)

Astronomy and Astrophysics

Astronomy

1

Black Holes (Astronomy), Gravitational Waves, Radiation Measurement, Radiation Sources, X Ray Binaries, Galactic Nuclei, Gravity Waves, Neutron Stars, Polarization (Waves), Signal To Noise Ratios, White Dwarf Stars

Scientific paper

One of the most attractive possible sources of strong gravitational waves would be a binary system comprising massive black holes (BH). The gravitational radiation from a binary is an elliptically polarized, periodic wave which could be observed continuously - or at intervals whenever a detector was available. This continuity of the signal is certainly appealing compared to waiting for individual pulses from infrequent random events. It also has the advantage over pulses that continued observation can increase the signal-to-noise ratio almost indefinitely. Furthermore, this system is dynamically simple; the theory of the generation of the radiation is unambiguous; all characteristics of the signal can be precisely related to the dynamical parameters of the source. The current situation is that while there is no observational evidence as yet for the existence of massive binary BH, their formation is theoretically plausible, and within certain coupled constraints of mass and location, their existence cannot be observationally excluded. Detecting gravitational waves from these objects might be the first observational proof of their existence.

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