Toward the evolution of magnetized differentially rotating neutron stars with AMR

ORAL

Abstract

The interaction of rotating compact objects endowed with magnetic fields likely plays a key role in understanding and modelling the central engines of active galactic nuclei, gamma ray bursts, and jet formation. Such simulations not only require dynamic gravitational backgrounds and relativistic fluid treatments, but also adequately resolving many time and length scales in order to capture the dynamics. Using a distributed adaptive mesh refinement infrastructure, we explore simulations of differentially rotating neutron stars both with and without magnetic fields in full 3-D.

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Authors

  • Matthew Anderson

    Department of Physics and Astronomy, Louisiana State University, Baton Rouge, LA 70803, Lousiana State University

  • Eric Hirschmann

    Brigham Young University

  • Steve Liebling

    Department of Physics, Long Island University - C.W. Post Campus, Brookville, NY 11548, Long Island University, Department of Physics, Long Island University - C.W. Post Campus, Brookville, New York 11548, USA

  • David Neilsen

    Brigham Young University, Department of Physics and Astronomy, Brigham Young University, Provo, UT 84602