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Equation-of-state insensitive relations after GW170817

Carson, Zack and Chatziioannou, Katerina and Haster, Carl-Johan and Yagi, Kent and Yunes, Nicolás (2019) Equation-of-state insensitive relations after GW170817. Physical Review D, 99 (8). Art. No. 083016. ISSN 2470-0010. https://resolver.caltech.edu/CaltechAUTHORS:20200804-125059299

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Abstract

The thermodynamic relation between pressure and density (i.e., the equation of state) of cold supranuclear matter is critical in describing neutron stars, yet it remains one of the largest uncertainties in nuclear physics. The extraction of tidal deformabilities from the gravitational waves emitted in the coalescence of neutron star binaries, such as GW170817, is a promising tool to probe this thermodynamic relation. Equation-of-state insensitive relations between symmetric and antisymmetric combinations of individual tidal deformabilities, the so-called “binary Love relations”, have proven important to infer the radius of neutron stars, and thus constrain the equation of state, from such gravitational waves. A similar set of relations between the moment of inertia, the tidal deformability, the quadrupole moment, and the compactness of neutron stars, the so-called “I-Love-Q” and “C-Love” relations, allow for future tests of General Relativity in the extreme gravity regime. But even the most insensitive of such relations still presents some degree of equation-of-state variability that could introduce systematic uncertainties in parameter extraction and in model selection. We here reduce this variability by more than 50% by imposing a prior on the allowed set of equations of state, derived from the posteriors generated from the analysis of GW170817. The resulting increase in insensitivity reduces systematic uncertainties in the extraction of the tidal deformability from future gravitational wave observations, although statistical uncertainties currently dominate the error budget, and will continue to do so until the era of Voyager-class detectors.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1103/physrevd.99.083016DOIArticle
https://arxiv.org/abs/1903.03909arXivDiscussion Paper
ORCID:
AuthorORCID
Chatziioannou, Katerina0000-0002-5833-413X
Yunes, Nicolás0000-0001-6147-1736
Additional Information:© 2019 American Physical Society. Received 8 March 2019; published 30 April 2019. K. Y. acknowledges support from NSF Grant No. PHY-1806776. K. Y. would like to also acknowledge networking support by the COST Action GWverse CA16104. N. Y. acknowledges support from NSF Grant No. PHY-1759615 and NASA Grants No. NNX16AB98G and No. 0NSSC17M0041. This research has made use of data, software and/or web tools obtained from the Gravitational Wave Open Science Center (https://www.gw-openscience.org), a service of LIGO Laboratory, the LIGO Scientific Collaboration, and the Virgo Collaboration. LIGO is funded by the U.S. National Science Foundation. Virgo is funded by the French Centre National de Recherche Scientifique (CNRS), the Italian Istituto Nazionale della Fisica Nucleare (INFN), and the Dutch Nikhef, with contributions by Polish and Hungarian institutes. The authors are grateful for computational resources provided by the LIGO Laboratory and supported by National Science Foundation Grants No. PHY-0757058 and No. PHY-0823459.
Funders:
Funding AgencyGrant Number
NSFPHY-1806776
European Cooperation in Science and Technology (COST)CA16104
NSFPHY-1759615
NASANNX16AB98G
NASA0NSSC17M0041
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Istituto Nazionale di Fisica Nucleare (INFN)UNSPECIFIED
NikhefUNSPECIFIED
NSFPHY-0757058
NSFPHY-0823459
Issue or Number:8
Record Number:CaltechAUTHORS:20200804-125059299
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20200804-125059299
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:104731
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:05 Aug 2020 19:32
Last Modified:05 Aug 2020 19:32

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