Distributed AMR infrastructure for PDEs

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HAD is a computational toolkit providing distributed adaptive mesh refinement for partial differential equations. It provides a flexible environment for diverse applications which can be combined or employed individually. To date we have implemented applications for the Einstein equations; General Relativistic Magneto Hydrodynamics and (complex) Klein-Gordon fields. These have been employed in full 3D simulations of:

Binary Black Holes (BBH)

EM and GW Radiation We evolve an orbiting pair of black holes and study their interaction with an electromagnetic field and plasma:
  • Magnetospheres of Black Hole Systems in Force-Free Plasma PRD 1007.1198 (2010)
  • Dual Jets from Binary Black Holes Science (2010)
  • Stirring, not shaking: binary black holes' effects on electromagnetic fields PRL 0905.1121 (2009)

Black Hole-Neutron Star Binaries (BHNS)

Isosurface of density for BHNS merger We study the remnant matter and fallback time from the disruption and merger of a neutron star with a black hole:
  • Mergers of Magnetized Neutron Stars with Spinning Black Holes: Disruption, Accretion and Fallback PRL 1006.2839 (2010)

Binary Neutron Stars (BNS)

Density of near merger of two neutron stars We examine evolutions of orbiting neutron stars looking for the effects of magnetic field and the equation of state:
  • Magnetized Neutron-Star Mergers and Gravitational-Wave Signals PRL 0801.4387 (2008)
  • Simulating binary neutron stars: dynamics and gravitational waves PRD 0708.2720 (2007)

Single Neutron Stars and Black Holes

Density and magnetic field strength of a neutron star We evolve single stars and black holes studying the effect of magnetic field and accretion disk dynamics, as well as using them to test the code.
  • Dynamics of Rotating, Magnetized Neutron Stars 1002.2217 (2010)
  • Evolutions of Magnetized and Rotating Neutron Stars PRD 1001.0575 (2010)
  • Post-merger electromagnetic emissions from disks perturbed by binary black holes PRD 0910.4969 (2010)

Black Hole Critical Behavior

Critical Scaling Results Evolutions of perturbed, unstable stellar solutions suggest Type I critical behavior. Such studies represent one of the rare critical evolutions in full 3D with no symmetries.
  • Dynamics of Rotating, Magnetized Neutron Stars 1002.2217 (2010)
  • Evolutions of Magnetized and Rotating Neutron Stars PRD 1001.0575 (2010)

Global Existence and Nonlinear Wave Equations

Near Critical Snapshot Evolutions of various flatspace, but nonlinear, systems of equations, including wave equations are of interest to mathematicians. One question in particular is whether a given model allows for the development of singularities from smooth initial data.
  • Threshold of Singularity Formation in the Semilinear Wave Equation PRD gr-qc/0502056 (2005)
  • The Nonlinear Sigma Model With Distributed Adaptive Mesh Refinement CQG gr-qc/0403076 (2004)
  • The Singularity Threshold of the Nonlinear Sigma Model Using 3D Adaptive Mesh Refinement PRD gr-qc/0202093 (2002)

Last updated August 18, 2010.
Copyright© 2002--2010
Research Supported by NSF