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  Gravitational waveforms for neutron star binaries from binary black hole simulations

Barkett, K., Scheel, M. A., Haas, R., Ott, C. D., Bernuzzi, S., Brown, D. A., et al. (2016). Gravitational waveforms for neutron star binaries from binary black hole simulations. Physical Review D, 93: 044064. doi:10.1103/PhysRevD.93.044064.

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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-002B-26EF-4 Version Permalink: http://hdl.handle.net/11858/00-001M-0000-002B-26F0-F
Genre: Journal Article

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1509.05782.pdf (Preprint), 1012KB
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 Creators:
Barkett, Kevin, Author
Scheel, Mark A., Author
Haas, R.1, Author              
Ott, Christian D., Author
Bernuzzi, Sebastiano, Author
Brown, Duncan A., Author
Szilágyi, Béla, Author
Kaplan, Jeffrey D., Author
Lippuner, Jonas, Author
Muhlberger, Curran D., Author
Foucart, Francois, Author
Duez, Matthew D., Author
Affiliations:
1Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, escidoc:1933290              

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Free keywords: General Relativity and Quantum Cosmology, gr-qc
 Abstract: Gravitational waves from binary neutron star (BNS) and black hole/neutron star (BHNS) inspirals are primary sources for detection by the Advanced Laser Interferometer Gravitational-Wave Observatory. The tidal forces acting on the neutron stars induce changes in the phase evolution of the gravitational waveform, and these changes can be used to constrain the nuclear equation of state. Current methods of generating BNS and BHNS waveforms rely on either computationally challenging full 3D hydrodynamical simulations or approximate analytic solutions. We introduce a new method for computing inspiral waveforms for BNS/BHNS systems by adding the post-Newtonian (PN) tidal effects to full numerical simulations of binary black holes (BBHs), effectively replacing the nontidal terms in the PN expansion with BBH results. Comparing a waveform generated with this method against a full hydrodynamical simulation of a BNS inspiral yields a phase difference of $<1$ radian over $\sim 15$ orbits. The numerical phase accuracy required of BNS simulations to measure the accuracy of the method we present here is estimated as a function of the tidal deformability parameter ${\lambda}$.

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 Dates: 2015-09-182016-02-252016
 Publication Status: Published in print
 Pages: 7 pages, 3 figures; updated acknowledgements; published PRD version
 Publishing info: -
 Table of Contents: -
 Rev. Method: -
 Identifiers: arXiv: 1509.05782
DOI: 10.1103/PhysRevD.93.044064
URI: http://arxiv.org/abs/1509.05782
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Title: Physical Review D
  Other : Phys. Rev. D.
Source Genre: Journal
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Publ. Info: Lancaster, Pa. : American Physical Society
Pages: - Volume / Issue: 93 Sequence Number: 044064 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: http://pubman.mpdl.mpg.de/cone/journals/resource/111088197762258