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Probing Extreme-density Matter with Gravitational-wave Observations of Binary Neutron Star Merger Remnants

Radice, David and Bernuzzi, Sebastiano and Del Pozzo, Walter and Roberts, Luke F. and Ott, Christian D. (2017) Probing Extreme-density Matter with Gravitational-wave Observations of Binary Neutron Star Merger Remnants. Astrophysical Journal Letters, 842 (2). Art. No. L10. ISSN 2041-8213. https://resolver.caltech.edu/CaltechAUTHORS:20170616-100047138

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Abstract

We present a proof-of-concept study, based on numerical-relativity simulations, of how gravitational waves (GWs) from neutron star merger remnants can probe the nature of matter at extreme densities. Phase transitions and extra degrees of freedom can emerge at densities beyond those reached during the inspiral, and typically result in a softening of the equation of state (EOS). We show that such physical effects change the qualitative dynamics of the remnant evolution, but they are not identifiable as a signature in the GW frequency, with the exception of possible black hole formation effects. The EOS softening is, instead, encoded in the GW luminosity and phase and is in principle detectable up to distances of the order of several megaparsecs with advanced detectors and up to hundreds of megaparsecs with third-generation detectors. Probing extreme-density matter will require going beyond the current paradigm and developing a more holistic strategy for modeling and analyzing postmerger GW signals.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/2041-8213/aa775fDOIArticle
http://iopscience.iop.org/article/10.3847/2041-8213/aa775f/metaPublisherArticle
https://arxiv.org/abs/1612.06429arXivDiscussion Paper
ORCID:
AuthorORCID
Roberts, Luke F.0000-0001-7364-7946
Ott, Christian D.0000-0003-4993-2055
Additional Information:© 2017 The American Astronomical Society. Received 2017 May 4; revised 2017 May 24; accepted 2017 June 2; published 2017 June 14. We thank S. Hild for the ET-D noise curve data and the anonymous referee for useful comments, and we acknowledge useful discussions with A. Burrows, T. Dietrich, S. Marka, L. Rezzolla, B. S. Sathyaprakash, and K. Takami. D.R. gratefully acknowledges support from the Schmidt Fellowship, the Sherman Fairchild Foundation and the Max-Planck/Princeton Center (MPPC) for Plasma Physics (NSF PHY-1523261). C.D.O. was partially supported by NSF awards CAREER PHY-1151197, PHY-1404569, and TCAN AST-1333520, and by the Sherman Fairchild Foundation. The simulations were performed on NSF XSEDE (TG-PHY160025), and on NSF/NCSA Blue Waters (NSF PRAC ACI-1440083).
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funders:
Funding AgencyGrant Number
Schmidt FellowshipUNSPECIFIED
Sherman Fairchild FoundationUNSPECIFIED
NSFPHY-1523261
NSFPHY-1151197
NSFPHY-1404569
NSFAST-1333520
NSFTG-PHY160025
NSFACI-1440083
Subject Keywords:gravitational waves – stars: neutron
Issue or Number:2
Record Number:CaltechAUTHORS:20170616-100047138
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170616-100047138
Official Citation:David Radice et al 2017 ApJL 842 L10
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:78267
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:16 Jun 2017 19:19
Last Modified:03 Oct 2019 18:07

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