Comparison of eccentric numerical relativity simulations to small mass-ratio perturbation theory

          @misc{ pirsa_PIRSA:21060027,
            doi = {10.48660/21060027},
            url = {https://pirsa.org/21060027},
            author = {Ramos-Buades, Antoni},
            keywords = {Other},
            language = {en},
            title = {Comparison of eccentric numerical relativity simulations to small mass-ratio perturbation theory},
            publisher = {Perimeter Institute},
            year = {2021},
            month = {jun},
            note = {PIRSA:21060027 see, \url{https://pirsa.org}}
          }
          

Abstract

In this work we compare two approaches to modeling binary black holes (BBHs): 1) small mass-ratio (SMR) perturbation theory, and 2) numerical relativity (NR). We extend recent work on combining information from quasicircular nonspinning NR simulations of BBHs with results from SMR perturbation theory to nonspinning eccentric BBHs. We produce a dataset of long and accurate eccentric nonspinning NR simulations with the Spectral Einstein Code (SpEC) from mass ratios 1 to 10, and eccentricities up to 0.7. We analyze these NR simulations, compute gauge invariant quantities from the gravitational radiation, and develop tools to map points in parameter space between eccentric NR and SMR waveforms. Finally, we discuss discrepancies between SMR and NR predictions for the energy and angular momentum fluxes due to eccentricity, and limitations of such comparisons due to the limited parameter space in mass ratio covered by the NR simulations.