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Constraining the Gravitational-Wave Afterglow From a Binary Neutron Star Coalescence

Banagiri, Sharan and Coughlin, Michael W. and Clark, James and Lasky, Paul D. and Bizouard, M. A. and Talbot, Colm and Thrane, Eric and Mandic, Vuk (2019) Constraining the Gravitational-Wave Afterglow From a Binary Neutron Star Coalescence. . (Unpublished) https://resolver.caltech.edu/CaltechAUTHORS:20190906-112627297

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Abstract

Binary neutron star mergers are rich laboratories for physics, accessible with ground-based interferometric gravitational-wave detectors such as Advanced LIGO and Advanced Virgo. If a neutron star remnant survives the merger, it can emit gravitational waves that might be detectable with the current or next generation detectors. The physics of the long-lived post-merger phase is not well understood and makes modeling difficult. In particular the phase of the gravitational-wave signal is not well modeled. In this paper, we explore methods for using long duration post-merger gravitational-wave signals to constrain the parameters and the properties of the remnant. We develop a phase-agnostic likelihood model which uses only the spectral content for parameter estimation and demonstrate the calculation of a Bayesian upper limit in the absence of a signal. With the millisecond magnetar model, we show that for an event like GW170817, the ellipticity of a long-lived remnant can be constrained to less than about 0.5 in the parameter space used.


Item Type:Report or Paper (Discussion Paper)
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1909.01934arXivDiscussion Paper
ORCID:
AuthorORCID
Coughlin, Michael W.0000-0002-8262-2924
Lasky, Paul D.0000-0003-3763-1386
Thrane, Eric0000-0002-4418-3895
Additional Information:We are grateful to Ling Sun, Joe Romano, David Keitel and Paul Schale and for useful discussion and comments. SB acknowledges support by the Hoff Lu Fellowship at the university of Minnesota, and by NSF grant PHY-1806630. MC is supported by the David and Ellen Lee Postdoctoral Fellowship at the California Institute of Technology. PDL is supported by ARC Future Fellowship FT160100112 and ARC Discovery Project DP180103155. ET and CT are supported by CE170100004. ET is supported by FT150100281. The authors are thankful for the computing resources provided by LIGO Laboratory. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation and operates under cooperative agreement PHY-0757058. All posterior corner plots were made with ChainConsumer (Hinton 2016). The code for the analysis in this paper is available upon request. A public release is being planned for the near future. This paper has been assigned document number LIGO-P1900107.
Group:LIGO
Funders:
Funding AgencyGrant Number
University of MinnesotaUNSPECIFIED
NSFPHY-1806630
David and Ellen Lee Postdoctoral ScholarshipUNSPECIFIED
Australian Research CouncilFT160100112
Australian Research CouncilDP180103155
Australian Research CouncilCE170100004
Australian Research CouncilFT150100281
NSFPHY-0757058
Subject Keywords:gravitational waves, stars: neutron, methods: statistical
Other Numbering System:
Other Numbering System NameOther Numbering System ID
LIGO DocumentP1900107
Record Number:CaltechAUTHORS:20190906-112627297
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190906-112627297
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:98486
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:06 Sep 2019 20:38
Last Modified:03 Oct 2019 21:41

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