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Annual Review of Nuclear and Particle Science

Volume 70, 2020

The Dynamics of Binary Neutron Star Mergers and GW170817

Abstract

With the first observation of a binary neutron star merger through gravitational waves and light, GW170817, compact binary mergers have now taken the center stage in nuclear astrophysics. They are thought to be one of the main astrophysical sites of production of r-process elements, and merger observations have become a fundamental tool to constrain the properties of matter. Here, we review our current understanding of the dynamics of neutron star mergers in general and of GW170817 in particular. We discuss the physical processes governing the inspiral, merger, and postmerger evolution, and we highlight the connections between these processes, the dynamics, and the multimessenger observables. Finally, we discuss open questions and issues in the field and the need to address them through a combination of better theoretical models and new observations.

Keyword(s): gravitational wave generation, gravitational wave sources, multimessenger astrophysics, neutron stars
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2020-10-19
2024-10-12
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The Dynamics of Binary Neutron Star Mergers and GW170817
Annual Review of Nuclear and Particle Science 70, 95 (2020); https://doi.org/10.1146/annurev-nucl-013120-114541
/content/journals/10.1146/annurev-nucl-013120-114541
/content/journals/10.1146/annurev-nucl-013120-114541
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Supplementary Data

  • Supplemental Figure 1: The top panels show rest mass density (top left) and temperature (top right) on the orbital plane for a binary neutron star system with MA = MB = 1.35M⊙ simulated with the SFHo equation of state (Steiner et al. 2012). The bottom panels show temperature–density (bottom left) and entropy–density (bottom right) histograms computed from the full-3D data. From this figure it is possible to appreciate the thermodynamic conditions achieved in the merger remnant as it evolves toward gravitational collapse and black hole formation. Reference: Steiner AW, et al. Astrophys J. 774:17 (2013)

    Supplemental Figure 2: The top panels show rest mass density (top left) and temperature (top right) on the orbital plane for a binary neutron star system with MA = MB = 1.35M⊙ simulated with the SFHo equation of state (Steiner et al. 2012). The bottom panels show histograms of log temperature versus log density and entropy versus log density. From this figure it is possible to better appreciate the thermodynamic conditions in the low-density disk and in the ejecta. Reference: Steiner AW, et al. Astrophys J. 774:17 (2013)

  • Article Type: Review Article

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