MHD-driven Kinetic Dissipation in the Solar Wind and Corona

By R. Leamon, William H. Matthaeus, Charles W. Smith, Gary Zank, D. Mullan, S. Oughton. 2000

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View Paper: https://www.semanticscholar.org/paper/b09345e524b4ff9f183ef92c0131bb39f584081e

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In Astronomy and Astrophysics

Citations in the corpus

Astrophysical Gyrokinetics: Basic Equations and Linear Theory (2005, background): “…and apply them to particle heating in solar flares, the solar wind, and hot radiatively inefficient accretion flows (see Quataert 1998; Gruzinov 1998; Quataert & Gruzinov 1999; Leamon et al. 1998, 1999, 2000;Cranmer&vanBallegooijen 2003, 2005, for related analytical and observational results).”
Bulk properties of the slow and fast solar wind and interplanetary coronal mass ejections measured by Ulysses: Three polar orbits of observations (2009, background): “Other potential sources include turbulent heating [Smith et al., 2001], heating from kinetic Alfvén waves [Leamon et al., 1999] or, perhaps, through magnetic reconnection [Leamon et al., 2000], although this last scenario appears somewhat doubtful, at least in the fast wind [Gosling, 2007].”
A Model of Turbulence in Magnetized Plasmas: Implications for the Dissipation Range in the Solar Wind (2007, background): “…[Coleman, 1968; Denskat et al., 1983; Goldstein et al., 1994; Leamon et al., 1998b; Gary , 1999], Landau damping of kinetic Alfvén waves [Leamon et al., 1998a, 1999; Leamon et al., 2000], or the dispersive nature of whistler waves [Stawicki et al., 2001; Krishan and Mahajan, 2004; Galtier , 2006].”
ASTROPHYSICAL GYROKINETICS: KINETIC AND FLUID TURBULENT CASCADES IN MAGNETIZED WEAKLY COLLISIONAL PLASMAS (2007, background): “…two scales a spectral break between the inertial and dissipation ranges occurs have produced claims thatdi is a more likely candidate (Smith et al. 2001), more comprehensive studies of the available data sets conclude basically that it is hard to tell (Leamon et al. 2000; Markovskii et al. 2008).”
Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence (2007, methodology): “We hope to link the macroscopic properties modeled by ZEPHYR with the microscopic kinetic processes studied by, e.g., Leamon et al. (1999, 2000), Cranmer & van Ballegooijen (2003), Voitenko & Goossens (2003, 2004), Gary & Nishimura (2004), Dmitruk et al. (2004), Chandran (2005), Gary et al. (2006),…”
Coronal Holes and the High-Speed Solar Wind (2002, background): “…have long been considered as the most likely, there has been much renewed interest in the ability of oblique and perpendicular-propagating waves to heat the plasma (e.g., Grappin et al. 2000; Leamon et al. 2000; Marsch and Tu 2001a; Li and Habbal 2001; Markovskii 2001; Hollweg and Markovskii 2002).”
SOLAR WIND TURBULENT SPECTRUM AT PLASMA KINETIC SCALES (2012, background): “Independent measurements at different distances from the Sun, between 0.3 AU and 0.9 AU (Bourouaine et al. 2012), and a statistical study at 1 AU (Leamon et al. 2000) indicate that the spectral break is related to the ion inertia length λi .”
Dependence of the Dissipation Range Spectrum of Interplanetary Magnetic Fluctuationson the Rate of Energy Cascade (2006, background): “Leamon et al. (2000) and Smith et al. (2001a) demonstrate that the dissipation range scales approximately with the ion inertial scale, where ion kinetics become important.”
Alfvénic Turbulence in the Extended Solar Corona: Kinetic Effects and Proton Heating (2003, methodology): “The interaction between large-scale “sweeping” terms in the corona and local turbulent cascade effects is discussed in detail by Leamon et al. (2000).”
Small-Scale Energy Cascade of the Solar Wind Turbulence (2007, background): “However, the interpretation of the smallscale energy cascade in the Hall MHD frame is supported by the observations of a clear correlation between the spectral break frequency fb and the Doppler-shifted wavevector of the ion inertia length fki (Leamon et al. 2000).”