List of Tables
Scaling exponents for velocity and magnetic variables calculated through ESS. Errors represent the standard deviations of the linear fitting. The data used comes from a turbulent sample of slow wind at 0.9 AU from Helios 2 spacecraft. As a comparison we show the normalized scaling exponents of structure functions calculated in a wind tunnel on Earth (Ruíz-Chavarría et al., 1995) for velocity and temperature. The temperature is a passive scalar in this experiment.
Normalized scaling exponents for radial magnetic fluctuations in a laboratory plasma, as measured at different distances ( being the minor radius of the torus in the experiment) from the external wall. Errors represent the standard deviations of the linear fitting. Scaling exponents have been obtained using the ESS.
Normalized scaling exponents for Alfvénic, velocity, and magnetic fluctuations obtained from data of high resolution 2D MHD numerical simulations. Scaling exponents have been calculated from spatial fluctuations; different times, in the statistically stationary state, have been used to improve statistics. The scaling exponents have been calculated by ESS using Equation (40) as characteristic scale rather than the third-order structure function (cf. Politano et al., 1998, for details).
Scaling exponents for velocity and magnetic variables, Elsässer variables, and fluxes. Errors on are about one order of magnitude smaller than the errors shown.
The values of the parameters , , and , in the fit of (see Equation (68) as a kernel for the scaling behavior of PDFs. FW and SW refer to fast and slow wind, respectively, as obtained from the Helios 2 spacecraft, by collecting in a single dataset all periods.
Typical values of several solar wind parameters as measured by Helios 2 at 1 AU.
Typical values of different speeds obtained at 1 AU. The Alfvén speed has been measured, while all the others have been obtained from the parameters reported in Table 6.
Typical values of different frequencies at 1 AU. These values have been obtained from the parameters reported in Table 6.
Typical values of different lengths at 1 AU plus the distance traveled by a proton before colliding with another proton. These values have been obtained from the parameters reported in Table 6.
Expected values for Alfvèn ratio , normalized cross-helicity , and normalized residual energy for a pure Alfvèn wave outward or inward oriented.