Pulsar timing and the detection of black hole binary systems in globular clusters

Details Pulsar timing and the detection of black hole binary systems in globular clusters Pulsar timing and the detection of black hole binary systems in globular clusters

2005-05-29

arxiv.org/abs/astro-ph/0505585v1

Astrophys.J. 627 (2005) L125-L128

Astronomy and Astrophysics

Astrophysics

Accepted into ApJ Letters. This is a slightly augmented version containing one extra figure

Scientific paper

10.1086/431949

The possible existence of intermediate mass binary black holes (IMBBHs) in globular clusters (GCs) offers a unique geometry in which to detect space-time oscillations. For certain pulsar-IMBBH configurations possible within a GC, the usual far-field plane wave approximation for the IMBBH metric perturbation severely underestimates the magnitude of the induced pulsar pulse time-of-arrival (TOA) fluctuations. In this letter, the expected TOA fluctuations induced by an IMBBH lying close to the line-of-sight between a pulsar and the Earth are calculated for the first time. For an IMBBH consisting of 10 Msolar and 10^3 Msolar components, a 10 year orbital period, and located 0.1 lyr from the Earth-Pulsar line of sight, the induced pulsar timing residual amplitude will be of order 5 to 500 ns.

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