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Beyond second-order convergence in simulations of binary neutron stars in full general relativity

Radice, David and Rezzolla, Luciano and Galeazzi, Filippo (2014) Beyond second-order convergence in simulations of binary neutron stars in full general relativity. Monthly Notices of the Royal Astronomical Society, 437 (1). L46-L50. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20140117-113254579

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Abstract

Despite the recent rapid progress in numerical relativity, a convergence order less than the second has so far plagued codes solving the Einstein–Euler system of equations. We report simulations of the inspiral of binary neutron stars in quasi-circular orbits computed with a new code employing high-order, high-resolution shock-capturing, finite-differencing schemes that, for the first time, go beyond the second-order barrier. In particular, without any tuning or alignment, we measure a convergence order above three both in the phase and in the amplitude of the gravitational waves. Because the new code is already able to calculate waveforms with very small phase errors at modest resolutions, we are able to obtain accurate estimates of tidal effects in the inspiral that are essentially free from the large numerical viscosity typical of lower order methods, and even for the challenging large compactness and small-deformability binary considered here. We find a remarkable agreement between our Richardson-extrapolated waveform and the one from the tidally corrected post-Newtonian (PN) Taylor-T4 model, with a de-phasing smaller than 0.4 rad during the seven orbits of the inspiral and up to the contact point. Because our results can be used reliably to assess the validity of the PN or other approximations at frequencies significantly larger than those considered so far in the literature, at these compactnesses, they seem to exclude significant tidal amplifications from next to next-to-leading-order terms in the PN expansion.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1093/mnrasl/slt137DOIArticle
http://mnrasl.oxfordjournals.org/content/437/1/L46PublisherArticle
http://arxiv.org/abs/1306.6052arXivDiscussion Paper
Additional Information:© 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2013 September 30. Received 2013 September 27; in original form 2013 September 2. First published online: October 28, 2013. It is a pleasure to acknowledge W. Kastaun for kindly providing the primitive recovery routine and F. Pannarale for providing the PN waveforms.We also thank D. Alic and K. Takami for numerous useful discussions. Partial support comes from the VESF grant (EGO-DIR-69-2010), the DFG grant SFB/Transregio 7 and by ‘Compstar’, a Research Networking Programme of the European Science Foundation. The calculations were performed on the SuperMUC cluster at the LRZ, on the Datura cluster at the AEI and on the LOEWE cluster in Frankfurt.
Funders:
Funding AgencyGrant Number
VESFEGO-DIR- 69-2010
DFG Grant SFB/Transregio 7UNSPECIFIED
European Science Foundation Research Networking ProgrammeUNSPECIFIED
Subject Keywords:gravitational waves stars: neutron
Record Number:CaltechAUTHORS:20140117-113254579
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20140117-113254579
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:43431
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:22 Jan 2014 16:04
Last Modified:22 Jan 2014 16:04

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