Evolution of Intermittency in the Slow and Fast Solar Wind Beyond the Ecliptic Plane
Anna Wawrzaszek, Marius Echim, Wies{\l}aw M. Macek, Roberto Bruno

TL;DR
This study analyzes how intermittency in solar wind magnetic turbulence evolves with distance and latitude beyond the ecliptic plane, revealing slow changes and hemispheric symmetry, with implications for solar origin of turbulence.
Contribution
It provides the first detailed analysis of intermittency evolution in the slow and fast solar wind beyond the ecliptic plane using multifractal modeling of Ulysses data.
Findings
Intermittency decreases slowly with distance and latitude.
Multifractality is lower than in the ecliptic.
Hemispheric symmetry in turbulent properties.
Abstract
We study intermittency as a departure from self-similarity of the solar wind magnetic turbulence and investigate the evolution with the heliocentric distance and latitude. We use data from the Ulysses spacecraft measured during two solar minima (1997-1998 and 2007-2008) and one solar maximum (1999-2001). In particular, by modeling a multifractal spectrum, we revealed the intermittent character of turbulence in the small-scale fluctuations of the magnetic field embedded in the slow and fast solar wind. Generally, at small distances from the Sun, in both the slow and fast solar wind, we observe the high degree of multifractality (intermittency) that decreases somewhat slowly with distance and slowly with latitude. The obtained results seem to suggest that generally intermittency in the solar wind has a solar origin. However, the fast and slow streams, shocks, and other nonlinear…
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