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  Matter imprints in waveform models for neutron star binaries: tidal and self-spin effects

Dietrich, T., Khan, S., Dudi, R., Kapadia, S. J., Kumar, P., Nagar, A., et al. (2019). Matter imprints in waveform models for neutron star binaries: tidal and self-spin effects. Physical Review D, 99: 024029. doi:10.1103/PhysRevD.99.024029.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0001-402F-3 Version Permalink: http://hdl.handle.net/21.11116/0000-0002-E9BA-6
Genre: Journal Article

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 Creators:
Dietrich , Tim1, Author
Khan, Sebastian, Author
Dudi, Reetika, Author
Kapadia, Shasvath J., Author
Kumar, Prayush, Author
Nagar, Alessandro, Author
Ohme, Frank, Author
Pannarale, Francesco, Author
Samajdar, Anuradha, Author
Bernuzzi, Sebastiano, Author
Carullo, Gregorio, Author
Del Pozzo, Walter, Author
Haney, Maria, Author
Markakis, Charalampos, Author
Puerrer, Michael1, Author              
Riemenschneider, Gunnar, Author
Setyawati, Yoshinta Eka, Author
Tsang, Ka Wa, Author
Broeck, Chris Van Den, Author
Affiliations:
1Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290              

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Free keywords: General Relativity and Quantum Cosmology, gr-qc, Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE
 Abstract: The combined observation of gravitational and electromagnetic waves from the coalescence of two neutron stars marks the beginning of multi-messenger astronomy with gravitational waves (GWs). The development of accurate gravitational waveform models is a crucial prerequisite to extract information about the properties of the binary system that generated a detected GW signal. In binary neutron star systems (BNS), tidal effects also need to be incorporated in the modeling for an accurate waveform representation. Building on previous work [Phys.Rev.D96 121501], we explore the performance of inspiral-merger waveform models that are obtained by adding a numerical relativity (NR) based approximant for the tidal part of the phasing (NRTidal) to existing models for nonprecessing and precessing binary black hole systems (SEOBNRv4, PhenomD and PhenomPv2), as implemented in the LSC Algorithm Library Suite. The resulting BNS waveforms are compared and contrasted to target waveforms hybridizing NR waveforms, covering the last approx. 10 orbits up to merger and extending through the postmerger phase, with inspiral waveforms calculated from 30Hz obtained with TEOBResumS. The latter is a state-of-the-art effective-one-body waveform model that blends together tidal and spin effects. We probe that the combination of the PN-based self-spin terms and of the NRTidal description is necessary to obtain minimal mismatches (< 0.01) and phase differences (< 1 rad) with respect to the target waveforms. However, we also discuss possible improvements and drawbacks of the NRTidal approximant in its current form, since we find that it tends to overestimate the tidal interaction with respect to the TEOBResumS model during the inspiral.

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 Dates: 2018-04-0620182019
 Publication Status: Published in print
 Pages: -
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 Table of Contents: -
 Rev. Method: -
 Identifiers: arXiv: 1804.02235
URI: http://arxiv.org/abs/1804.02235
DOI: 10.1103/PhysRevD.99.024029
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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: 99 Sequence Number: 024029 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: https://pure.mpg.de/cone/journals/resource/111088197762258