English
 
Help Privacy Policy Disclaimer
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT

Released

Journal Article

Matter effects on binary neutron star waveforms

MPS-Authors
/persons/resource/persons4291

Read,  Jocelyn
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

/persons/resource/persons20657

Giacomazzo,  B.
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

/persons/resource/persons20670

Rezzolla,  Luciano
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

External Resource
No external resources are shared
Fulltext (restricted access)
There are currently no full texts shared for your IP range.
Fulltext (public)

1306.4065.pdf
(Preprint), 7MB

PRD88_044042.pdf
(Any fulltext), 5MB

Supplementary Material (public)
There is no public supplementary material available
Citation

Read, J., Baiotti, L., Creighton, J. D. E., Friedman, J. L., Giacomazzo, B., Kyutoku, K., et al. (2013). Matter effects on binary neutron star waveforms. Physical Review D, 88: 044042. doi:10.1103/PhysRevD.88.044042.


Cite as: https://hdl.handle.net/11858/00-001M-0000-0015-13B6-D
Abstract
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.