The normalized scaling exponents as a function of the moment order are reported, along with the linear expected value (full line). Data refer to the bulk velocity (black circles) and the magnitude of the magnetic field (white circles), as measured by the Helios 2 satellite in the inner heliosphere at AU during slow wind streams. Scaling exponents have been obtained through the extended self-similarity technique. Reported for comparison are the normalized scaling exponents for the longitudinal velocity field (stars) and the temperature field (passive scalar) in usual fluid flow.
(Color online) Structure functions of interplanetary magnetic field derived from (a) WIND data for the solar minimum of 1996 and (b) ACE spacecraft data for the solar maximum of 2000. Solid lines represent the best linear fit to the points between temporal scales and .
(Color online) ESS derived from (a) WIND data for the solar minimum of 1996 and (b) ACE spacecraft data for the solar maximum of 2000. Solid lines represent the best linear fit to the points between temporal scales and .
(Color online) Scaling exponents from ESS of the magnetic field magnitude fluctuations for solar minimum (empty circles), solar maximum (filled circles), and the ACE interval for (triangles).
Top: wind speed profile during 30 days of data recorded by WIND. Bottom: magnetic field intensity profile. The four vertical dashed lines and the three different symbols identify three different regions where we evaluated the intermittent character of the fluctuations.
Flatness factor versus time scale relative to the three different time intervals shown in the previous figure.
The periods of WIND measurements used in this work: average and root mean square velocity and IMF, and the size of each data set.
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