Authors: Abdul H. Mroué, Harald P. Pfeiffer, Lawrence E. Kidder, Saul A. Teukolsky
Date: 27 Apr 2010
Abstract: We compare different methods of computing the orbital eccentricity of quasi-circular binary black hole systems using the orbital variables and gravitational wave phase and frequency. For eccentricities of about a per cent, most methods work satisfactorily. For small eccentricity, however, the gravitational wave phase allows a particularly clean and reliable measurement of the eccentricity. Furthermore, we measure the decay of the orbital eccentricity during the inspiral and find reasonable agreement with post-Newtonian results. Finally, we measure the periastron advance of non-spinning binary black holes, and we compare them to post-Newtonian approximations. With the low uncertainty in the measurement of the periastron advance, we positively detect deviations between fully numerical simulations and post-Newtonian calculations.
© M. Vallisneri 2012 — last modified on 2010/01/29
Tantum in modicis, quantum in maximis