TY - JOUR

T1 - Accurate and efficient waveforms for compact binaries on eccentric orbits

AU - Huerta, E. A.

AU - Kumar, Prayush

AU - McWilliams, Sean T.

AU - O'Shaughnessy, Richard

AU - Yunes, Nicolás

N1 - Publisher Copyright:
© 2014 American Physical Society.

PY - 2014/10/10

Y1 - 2014/10/10

N2 - Compact binaries that emit gravitational waves in the sensitivity band of ground-based detectors can have non-negligible eccentricities just prior to merger, depending on the formation scenario. We develop a purely analytic, frequency-domain model for gravitational waves emitted by compact binaries on orbits with small eccentricity, which reduces to the quasicircular post-Newtonian approximant TaylorF2 at zero eccentricity and to the postcircular approximation of Yunes et al. [Phys. Rev. D 80, 084001 (2009)] at small eccentricity. Our model uses a spectral approximation to the (post-Newtonian) Kepler problem to model the orbital phase as a function of frequency, accounting for eccentricity effects up to O(e8) at each post-Newtonian order. Our approach accurately reproduces an alternative time-domain eccentric waveform model for e∈[0,0.4] and binaries with total mass ≲12M ". As an application, we evaluate the signal amplitude that eccentric binaries produce in different networks of existing and forthcoming gravitational waves detectors. Assuming a population of eccentric systems containing black holes and neutron stars that is uniformly distributed in comoving volume, we estimate that second-generation detectors like Advanced LIGO could detect approximately 0.1-10 events per year out to redshift z∼0.2, while an array of Einstein Telescope detectors could detect hundreds of events per year to redshift z∼2.3.

AB - Compact binaries that emit gravitational waves in the sensitivity band of ground-based detectors can have non-negligible eccentricities just prior to merger, depending on the formation scenario. We develop a purely analytic, frequency-domain model for gravitational waves emitted by compact binaries on orbits with small eccentricity, which reduces to the quasicircular post-Newtonian approximant TaylorF2 at zero eccentricity and to the postcircular approximation of Yunes et al. [Phys. Rev. D 80, 084001 (2009)] at small eccentricity. Our model uses a spectral approximation to the (post-Newtonian) Kepler problem to model the orbital phase as a function of frequency, accounting for eccentricity effects up to O(e8) at each post-Newtonian order. Our approach accurately reproduces an alternative time-domain eccentric waveform model for e∈[0,0.4] and binaries with total mass ≲12M ". As an application, we evaluate the signal amplitude that eccentric binaries produce in different networks of existing and forthcoming gravitational waves detectors. Assuming a population of eccentric systems containing black holes and neutron stars that is uniformly distributed in comoving volume, we estimate that second-generation detectors like Advanced LIGO could detect approximately 0.1-10 events per year out to redshift z∼0.2, while an array of Einstein Telescope detectors could detect hundreds of events per year to redshift z∼2.3.

UR - http://www.scopus.com/inward/record.url?scp=84908236470&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84908236470&partnerID=8YFLogxK

U2 - 10.1103/PhysRevD.90.084016

DO - 10.1103/PhysRevD.90.084016

M3 - Article

AN - SCOPUS:84908236470

VL - 90

JO - Physical Review D - Particles, Fields, Gravitation and Cosmology

JF - Physical Review D - Particles, Fields, Gravitation and Cosmology

SN - 1550-7998

IS - 8

M1 - 084016

ER -