Matter effects on binary neutron star waveforms

By J. Read, Luca Baiotti, Jolien D. E. Creighton, J. Friedman, B. Giacomazzo, K. Kyutoku, Charalampos Markakis, Luciano Rezzolla, M. Shibata, K. Taniguchi. 2013

176 citations recorded by the source corpus.

Using an extended set of equations of state and a multiple-group multiple-code collaborative effort to generate waveforms, we improve numerical-relativity-based data-analysis estimates of the measurability of matter effects in neutron-star binaries. We vary two parameters of a parameterized piecewise-polytropic equation of state (EOS) to analyze the measurability of EOS properties, via a parameter {\Lambda} 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 point-particle (or spinless double black-hole binary) inspiral increases monotonically with {\Lambda}, and changes in the EOS that did not change {\Lambda} are not measurable. We estimate with two methods the minimal and expected measurability of {\Lambda} in second- and third- generation gravitational-wave detectors. The first estimate, using numerical waveforms alone, shows two EOS which vary in radius by 1.3km are distinguishable in mergers at 100Mpc. The second estimate relies on the construction of hybrid waveforms by matching to post-Newtonian inspiral, and estimates that the same EOS are distinguishable in mergers at 300Mpc. We calculate systematic errors arising from numerical uncertainties and hybrid construction, and we estimate the frequency at which such effects would interfere with template-based searches.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/ecc201d5504789f32b72ae0fb1a27252765a5dfb

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Citations in the corpus

Constraining the Maximum Mass of Neutron Stars from Multi-messenger Observations of GW170817 (2017, background): “H E ] 8 N ov 2 01 7 2 et al. 2012; Favata 2014; Read et al. 2013; Del Pozzo et al. 2013; Agathos et al. 2015; Lackey & Wade 2015; Chatziioannou et al. 2015) and for quasi-periodic oscillations of the post-merger remnant (e.g. Bauswein & Janka 2012; Bauswein et al. 2012; Clark et al. 2014; Bauswein…”
Science case for the Einstein telescope (2019, background): “From [42] (figure courtesy of Jocelyn Read, based on results presented in [43]).”
Beyond second-order convergence in simulations of binary neutron stars in full general-relativity (2013, methodology): “…and as already mentioned above, this high order of convergence is obtained without any manipulation of the waveforms, which is a procedure hardly justified from a mathematical point of view, although used by some of us (Baiotti et al. 2009; Read et al. 2013) and in (Hotokezaka et al. 2013).”
Neutron-star Radius Constraints from GW170817 and Future Detections (2017, background): “…can be obtained from the GW signal either from finite-size effects during the late inspiral phase (e.g. Faber et al. 2002; Flanagan & Hinderer 2008; Read et al. 2013; Del Pozzo et al. 2013; Abbott et al. 2017) or through the characteristic oscillations of the postmerger remnant (Bauswein & Janka…”
Using Gravitational-wave Observations and Quasi-universal Relations to Constrain the Maximum Mass of Neutron Stars (2017, background): “This imprint, such as the one associated with the GW frequency at maximum amplitude (Read et al. 2013; Bernuzzi et al. 2014; Takami et al. 2015), can even be quasi-universal in the sense that it depends only weakly on the EOS.”
Tidal Deformability from GW170817 as a Direct Probe of the Neutron Star Radius (2018, background): “The degree of the deviation depends on the underlying EOS and, as a result, could be used to differentiate between EOS that differ in radius by only ∼1 km (Read et al. 2009b, 2013; Lackey & Wade 2015).”
Maximum mass, moment of inertia and compactness of relativistic stars (2016, background): “With the exception of those works that have looked at the existence of universality in merging systems of neutron-star binaries (Read et al. 2013; Maselli et al. 2013; Takami et al. 2014, 2015; Bernuzzi et al. 2014), all of the work done so far on universal relations in isolated relativistic stars…”
GW170817: Joint Constraint on the Neutron Star Equation of State from Multimessenger Observations (2017, background): “…signal during the inspiral (Flanagan & Hinderer 2008; Damour & Nagar 2010; Hinderer et al. 2010, 2016; Damour et al. 2012; Del Pozzo et al. 2013; Read et al. 2013; Favata 2014; Wade et al. 2014; Bernuzzi et al. 2015b; Lackey & Wade 2015; Hotokezaka et al. 2016; Lackey et al. 2017; Dietrich et…”
Unequal mass binary neutron star mergers and multimessenger signals (2016, unknown): “[63], see also [64–66]) using the ‘zero detuned, high power’ and the ‘no SRM’ noise curves in aLIGO [67].”
Prospects for Observing and Localizing Gravitational-Wave Transients with Advanced LIGO and Advanced Virgo (2013, methodology): “The gravitational waveform from a BNS coalescence is well modeled and matched filtering can be used to search for signals and measure the system parameters [74, 35, 34, 90].”