Turbulent Heating of the Solar Wind by Newborn Interstellar Pickup Protons

By Charles W. Smith, P. Isenberg, William H. Matthaeus, J. Richardson. 2006

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In Astronomy and Astrophysics

Citations in the corpus

Electron and proton heating by solar wind turbulence (2009, methodology): “Previous theories [Zhou and Matthaeus, 1990; Marsch and Tu, 1993; Oughton and Matthaeus, 1995; Zank et al., 1996; Matthaeus et al., 1999; Smith et al., 2001, 2006; Matthaeus et al., 2004; Breech et al., 2005; Isenberg et al., 2003; Breech et al., 2008], have been able to account for radial…”
The Effects of a κ-Distribution in the Heliosheath on the Global Heliosphere and ENA Flux at 1 AU (2008, result): “…of Zank et al. (1996a) to show explicitly that PUI-enhanced turbulent dissipation of magnetic field fluctuations could account for the observed solar wind plasma heating, a result that was examined in considerably more detail by Smith et al. (2001; see also Chashei et al. 2003; Smith et al. 2006).”
Evaluation of the turbulent energy cascade rates from the upper inertial range in the solar wind at 1 AU (2007, background): “Cascade rates estimated from the energy-containing scale of turbulence at 1 AU by evaluating the triple-products of fluctuation magnetic fields and velocities and the correlation length scale of the turbulence also give values in this range [e.g., Smith et al., 2001a, 2006c; Isenberg, 2005].”
The Turbulent Cascade at 1 AU: Energy Transfer and the Third-Order Scaling for MHD (2007, background): “…of the proton temperature as measured by Voyager 2 from 1 to 45 AU and get a value of TP 3:77 ; 104R 0:49 K. Applying the Vasquez et al. (2007) analysis with an average wind speed of 400 km s 1 (Smith et al. 2006) yields a heating rate at 1AUof ¼ 1:1 ;103 J (kg s) 1 for the years 1977–1978.”
Theory and Transport of Nearly Incompressible Magnetohydrodynamic Turbulence (2017, background): “For example, Matthaeus et al. (1999a, 1999b) used α= 1, Smith et al. (2006), Breech et al. (2008), and Usmanov et al. (2012) used α= 0.8, and Usmanov et al. (2018) used α= 0.128.”
Turbulence transport throughout the heliosphere (2007, background): “In principle,fDisa function of VA/U and of the properties of the inertial range spectra, so it will depend on heliocentric position and solar cycle phase [ Smith et al., 2006 ].”
EMPIRICAL CONSTRAINTS ON PROTON AND ELECTRON HEATING IN THE FAST SOLAR WIND (2009, background): “These results may also depend on subtleties of the analysis technique, such as how the minimum-variance direction is interpreted (Smith et al. 2006b; Tessein et al. 2009) or how effects such as intermittency are treated (Bruno et al. 1999).”