Matter effects on binary neutron star waveforms
Abstract
Using an extended set of equations of state and a multiplegroup multiplecode collaborative effort to generate waveforms, we improve numericalrelativitybased dataanalysis estimates of the measurability of matter effects in neutronstar binaries. We vary two parameters of a parametrized piecewisepolytropic equation of state (EOS) to analyze the measurability of EOS properties, via a parameter Λ that characterizes the quadrupole deformability of an isolated neutron star. We find that, to within the accuracy of the simulations, the departure of the waveform from pointparticle (or spinless double blackhole binary) inspiral increases monotonically with Λ and changes in the EOS that did not change Λ are not measurable. We estimate with two methods the minimal and expected measurability of Λ in second and thirdgeneration gravitationalwave detectors. The first estimate using numerical waveforms alone shows that two EOSs which vary in radius by 1.3 km are distinguishable in mergers at 100 Mpc. The second estimate relies on the construction of hybrid waveforms by matching to postNewtonian inspiral and estimates that the same EOSs are distinguishable in mergers at 300 Mpc. We calculate systematic errors arising from numerical uncertainties and hybrid construction, and we estimate the frequency at which such effects would interfere with templatebased searches.
 Publication:

Physical Review D
 Pub Date:
 August 2013
 DOI:
 10.1103/PhysRevD.88.044042
 arXiv:
 arXiv:1306.4065
 Bibcode:
 2013PhRvD..88d4042R
 Keywords:

 04.30.w;
 97.60.Jd;
 04.25.D;
 26.60.c;
 Gravitational waves: theory;
 Neutron stars;
 Numerical relativity;
 Nuclear matter aspects of neutron stars;
 General Relativity and Quantum Cosmology;
 Astrophysics  High Energy Astrophysical Phenomena
 EPrint:
 21 pages, 13 figures