Numerical modeling of space plasma flows

By Stefano Markidis, Enrico Camporeale, D. Burgess, Rizwan‐uddin, Giovanni Lapenta. 2009

155 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/5109ee7abd01d78495811571cd247756602659e3

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Citations in the corpus

The Density Probability Distribution in Compressible Isothermal Turbulence: Solenoidal versus Compressive Forcing (2008, methodology): “The piecewise parabolic method (Colella & Woodward 1984) implementation of FLASH3 (Fryxell et al. 2000; Dubey et al. 2008) was used to solve the hydrodynamic equations on periodic uniform grids with 163841, 40962, and 10243 grid points in 1, 2 and 3 dimension(s) (1D, 2D, 3D).”
The link between shocks, turbulence, and magnetic reconnection in collisionless plasmas (2014, methodology): “Although we have conducted 3D global simulations of the magnetosphere [20, 21], here we will focus on 2D simulations for three reasons: a) One of the key issues considered is whether the shock generated turbulence can lead to formation of reconnecting current sheets.”
The Effects of a κ-Distribution in the Heliosheath on the Global Heliosphere and ENA Flux at 1 AU (2008, background): “ENAs are created in the heliosheath after a neutral atom from the local interstellar medium (LISM) chargeexchanges with a plasma proton.”
THE FRACTAL DENSITY STRUCTURE IN SUPERSONIC ISOTHERMAL TURBULENCE: SOLENOIDAL VERSUS COMPRESSIVE ENERGY INJECTION (2007, methodology): “Observations provide velocity dispersion to size relations for various molecular clouds (MCs), which document the existence of supersonic random motions on scales larger than ∼ 0.1 pc (e.g., Larson 1981; Myers 1983; Perault et al. 1986; Solomon et al. 1987; Falgarone et al. 1992; Heyer & Brunt…”