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  Comprehensive numerical relativity -- effective-one-body comparison to inform improvements in waveform models for binary neutron star systems

Dietrich, T., & Hinderer, T. (2017). Comprehensive numerical relativity -- effective-one-body comparison to inform improvements in waveform models for binary neutron star systems. Physical Review D, 95(12): 124006. doi:10.1103/PhysRevD.95.124006.

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Datensatz-Permalink: http://hdl.handle.net/11858/00-001M-0000-002C-A983-2 Versions-Permalink: http://hdl.handle.net/11858/00-001M-0000-002E-07C5-4
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 Urheber:
Dietrich, Tim1, Autor              
Hinderer, Tanja1, Autor              
Affiliations:
1Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, escidoc:1933290              

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Schlagwörter: General Relativity and Quantum Cosmology, gr-qc, Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE
 Zusammenfassung: We present a detailed comparison between tidal effective-one-body (EOB) models and new state-of-the-art numerical relativity simulations for non-spinning binary neutron star systems. This comparison is the most extensive one to date, covering a wide range in the parameter space and encompassing the energetics of the binary, the periastron advance, the time and frequency evolution of the gravitational wave phase for the dominant mode, and several subdominant modes. We consider different EOB models with tidal effects that have been proposed, including the model with dynamical tides of [Phys.Rev.Lett. 116 (2016) no.18, 181101] and the gravitational self-force (GSF) inspired tidal EOB model of [Phys.Rev.Lett. 114 (2015) no.16, 161103]. The EOB model with dynamical tides leads to the best representation of the systems considered here, however, the differences to the GSF-inspired model are small. A common feature is that for systems where matter effects are large, i.e. stiff equations of state or small total masses, all EOB models underestimate the tidal effects and differences to the results from numerical relativity simulations become noticeable near the merger. We analyze this regime to diagnose the shortcomings of the models in the late inspiral, where the two neutron stars are no longer isolated bodies moving in vacuum. Our work will serve to guide further advances in modeling these systems.

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 Datum: 2017-02-072017
 Publikationsstatus: Im Druck publiziert
 Seiten: 22 pages, 13 figures
 Ort, Verlag, Ausgabe: -
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 Identifikatoren: arXiv: 1702.02053
URI: http://arxiv.org/abs/1702.02053
DOI: 10.1103/PhysRevD.95.124006
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Titel: Physical Review D
  Andere : Phys. Rev. D.
Genre der Quelle: Zeitschrift
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Ort, Verlag, Ausgabe: Lancaster, Pa. : American Physical Society
Seiten: - Band / Heft: 95 (12) Artikelnummer: 124006 Start- / Endseite: - Identifikator: ISSN: 0556-2821
CoNE: http://pubman.mpdl.mpg.de/cone/journals/resource/111088197762258