Modeling the Electromagnetic and Gravitational Radiation from Neutron Stars

ORAL

Abstract

The dynamics of magnetized neutron stars both in binaries and in isolation are modeled with a novel numerical approach able to capture the dynamics of the star(s) and of the surrounding plasma. The stellar dynamics incorporate ideal MHD which appropriately models the regime in which the fluid pressure dominates that of the magnetic field, while the stellar exterior is modeled within the force free approach (magnetic pressure largely dominates that of the fluid). The approach is shown to approach certain known solutions. An intense electromagnetic outburst is observed for the collapsing, rotating star. The approach is also applied to the coalescence of a neutron star binary.

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Authors

  • Steven Liebling

    • Department of Physics, Long Island University, New York
    • Long Island University

  • Matthew Anderson

    • Department of Physics and Astronomy, Louisiana State University, Baton Rouge
    • Indiana University Bloomington

  • Eric Hirschmann

    • Brigham Young University

  • David Neilsen

    • Brigham Young University

  • Chad Hanna

    • Perimeter Institute for Theoretical Physics

  • Luis Lehner

    • Perimeter Institute for the Theoretical Physics, Waterloo - Department of Physics, University of Guelph, Guelph
    • Perimeter Institute for Theoretical Physics
    • Perimeter Institute/Univ of Guelph

  • Carlos Palenzuela

    • Canadian Institute for Theoretical Astrophysics

  • Christopher Thompson

    • Canadian Institute for Theoretical Astrophysics

  • Patrick Motl

    • Indiana University Kokomo