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Simulating binary neutron stars: Dynamics and gravitational waves

Matthew Anderson1, Eric W. Hirschmann2, Luis Lehner1, Steven L. Liebling3, Patrick M. Motl1, David Neilsen2, Carlos Palenzuela1, and Joel E. Tohline1

  • 1Department of Physics and Astronomy, Louisiana State University, Baton Rouge, Louisiana 70803-4001, USA
  • 2Department of Physics and Astronomy, Brigham Young University, Provo, Utah 84602, USA
  • 3Department of Physics, Long Island University–C.W. Post Campus, Brookville, New York 11548, USA

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Phys. Rev. D 77, 024006 – Published 7 January, 2008

DOI: https://doi.org/10.1103/PhysRevD.77.024006

Abstract

We model two mergers of orbiting binary neutron stars, the first forming a black hole and the second a differentially rotating neutron star. We extract gravitational waveforms in the wave zone. Comparisons to a post-Newtonian analysis allow us to compute the orbital kinematics, including trajectories and orbital eccentricities. We verify our code by evolving single stars and extracting radial perturbative modes, which compare very well to results from perturbation theory. The Einstein equations are solved in a first-order reduction of the generalized harmonic formulation, and the fluid equations are solved using a modified convex essentially non-oscillatory method. All calculations are done in three spatial dimensions without symmetry assumptions. We use the had computational infrastructure for distributed adaptive mesh refinement.

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Phys. Rev. D 77, 024006– Published 7 January, 2008
  • Received 20 August 2007

© 2008 American Physical Society

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