Anisotropy in Fast and Slow Solar Wind Fluctuations

By S. Dasso, L. Milano, William H. Matthaeus, Charles W. Smith. 2005

252 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/ecbf726a9f67e19308f0444bd64b79c4b8ac5944

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Citations in the corpus

ASTROPHYSICAL GYROKINETICS: KINETIC AND FLUID TURBULENT CASCADES IN MAGNETIZED WEAKLY COLLISIONAL PLASMAS (2007, methodology): “…in the spacecraft measurements of the turbulent fluctuations in the solar wind (Belcher & Davis 1971; Matthaeus et al. 1990; Bieber et al. 1996; Dasso et al. 2005; Bigazzi et al. 2006; Sorriso-Valvo et al. 2006; Horbury et al. 2005, 2008; Osman & Horbury 2007; Hamilton et al. 2008) and in the…”
Anisotropy of Alfvénic turbulence in the solar wind and numerical simulations (2010, background): “For example, the magnetic field correlation length has been shown to vary depending on the angle of observation with respect to the field direction (Crooker et al. 1982; Matthaeus, Goldstein & Roberts 1990; Dasso et al. 2005; Osman & Horbury 2007; Weygand et al. 2009).”
Particle acceleration at perpendicular shock waves: Model and observations (2005, background): “In the solar wind, lslab > l2D for fully evolved turbulence [Dasso et al., 2005].”
EMPIRICAL CONSTRAINTS ON PROTON AND ELECTRON HEATING IN THE FAST SOLAR WIND (2009, background): “A speed of 600 km s−1 is slightly more restrictive than the more standard value of 500 km s−1 that has been applied by others to define the fast wind (e.g., Dasso et al. 2005; MacBride et al. 2008).”
Power and spectral index anisotropy of the entire inertial range of turbulence in the fast solar wind (2010, background): “Many different solar wind quantities, for example; cross helicity (Milano et al. 2004), the magnetic field correlation function (Dasso et al. 2005; Osman & Horbury 2007; Weygand et al. 2009), and velocity components (Chapman & Hnat 2007), have been shown to vary anisotropically with respect to the…”
The Turbulent Cascade at 1 AU: Energy Transfer and the Third-Order Scaling for MHD (2007, methodology): “While it is not our intention to test the Dasso et al. (2005) conclusions, we note the apparent disagreement between the power spectra computed below and the conclusions of Dasso et al. Those authors assume a universal correlation function for all samples within either the fast-wind or slow-wind…”
A Model of Turbulence in Magnetized Plasmas: Implications for the Dissipation Range in the Solar Wind (2007, methodology): “At scales somewhat below the driving scale, the anisotropy of the turbulence, kk Dasso et al., 2005 ] in the slow solar wind.”