Now showing items 6-10 of 17

  • Direct comparisons of compressible magnetohydrodynamics and reduced magnetohydrodynamics turbulence

    Oughton, Sean; Dmitruk, Pablo; Matthaeus, William H. (American Institute of Physics, 2005-11-11)
    Direct numerical simulations of low Mach number compressible three-dimensional magnetohydrodynamic (CMHD3D) turbulence in the presence of a strong mean magnetic field are compared with simulations of reduced magnetohydrodynamics ...
  • Impact of Hall effect on energy decay in magnetohydrodynamic turbulence

    Matthaeus, William H.; Dmitruk, Pablo; Smith, D.; Ghosh, S.; Oughton, Sean (American Geophysical Union, 2003)
    We examine numerically the influence of Hall effect corrections to Ohm's law upon the decay of homogeneous compressible magnetohydrodynamic turbulence and conclude that there are no significant differences in global decay ...
  • Intermittency, nonlinear dynamics and dissipation in the solar wind and astrophysical plasmas

    Matthaeus, Willam H.; Wan, Minping; Servidio, Sergio; Greco, A.; Osman, Kareem T.; Oughton, Sean; Dmitruk, Pablo (The Royal Society, 2015)
    An overview is given of important properties of spatial and temporal intermittency, including evidence of its appearance in fluids, magnetofluids and plasmas, and its implications for understanding of heliospheric plasmas. ...
  • Local anisotropy, higher order statistics, and turbulence spectra

    Matthaeus, William H.; Servidio, Sergio; Dmitruk, Pablo; Carbone, V.; Oughton, Sean; Wan, Minping; Osman, Kareem T. (IOP PUBLISHING LTD, 2012)
    Correlation anisotropy emerges dynamically in magnetohydrodynamics (MHD), producing stronger gradients across the large-scale mean magnetic field than along it. This occurs both globally and locally, and has significant ...
  • MHD turbulence and heating of the open field-line solar corona

    Matthaeus, William H.; Mullan, D. J.; Dmitruk, Pablo; Milano, L. J.; Oughton, Sean (European Geoscience Union, 2003)
    This paper discusses the possibility that heating of the solar corona in open field-line regions emanating from coronal holes is due to a nonlinear cascade, driven by low-frequency or quasi-static magnetohydrodynamic ...