Gravitational-Wave Signature of an Inspiral into a Boson Star

Details Gravitational-Wave Signature of an Inspiral into a Boson Star Gravitational-Wave Signature of an Inspiral into a Boson Star

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...20514904k&link_type=abstract

American Astronomical Society Meeting 205, #149.04; Bulletin of the American Astronomical Society, Vol. 37, p.375

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Observations suggest that massive compact objects lie at the center of most galaxies. While these objects are commonly presumed to be supermassive black holes, alternative candidates such as boson stars (BS) have yet to be excluded. The inspiral of stellar-mass compact objects (COs) into these central objects will produce gravitational waves (GWs) and provide a major source for LISA, the proposed space-based GW detector. If the scalar field of which the BS is composed interacts only gravitationally with normal matter, stable orbits will exist not just outside the Scwarzschild radius but within the surface of the BS as well. Geodesics within the BS surface will exhibit extreme pericentre precession and other features making the emitted GWs readily distinguishable from those emitted during an inspiral into a black hole. Here we solve for the metric in the interior of a fairly generic class of BS, and evolve the trajectory of an inspiraling CO from the Schwarzschild exterior through the plunge into the exotic BS interior. We calculate the waveform for GWs emitted during this inspiral, and suggest several signatures by which such waveforms can be distinguished from those produced by inspirals into black holes.

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