Tsallis Distribution Functions in the Solar Wind: Magnetic Field and Velocity Observations

Journal Article · Thu Dec 06 00:00:00 EST 2007 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.2828742· OSTI ID:21049432

Burlaga, Leonard F; Vinas, Adolfo F ^[1]

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1. Geospace Physics Laboratory, Code 673, Heliophysics Science Division, NASA/Goddard Space Flight Center, Greenbelt, MD (United States)

The distributions the fluctuations of magnetic field strengths B(t) observed on a scale of a year in the heliosphere between 1 AU and 90 AU are approximately lognormal. The PDFs of the corresponding increments of B(t) are Tsallis distributions on scales from 1 hr--128 days between 1 and 90 AU. A deterministic MHD model predicts these results. The model predicts that small chaotic structures merge to form large structures. There is a 'phase transition' near {approx}40 AU at which the there is a change from growth to decay. Between R{approx}40 and 85 AU the solar wind is in a quasi-equilibrium state described by a 'q-triplet'.

• OSTI ID: 21049432
• Journal Information: AIP Conference Proceedings, Vol. 965, Issue 1; Conference: International conference on complexity, metastability and nonextensivity, Catania (Italy), 1-5 Jul 2007; Other Information: DOI: 10.1063/1.2828742; (c) 2007 American Institute of Physics; Country of input: International Atomic Energy Agency (IAEA); ISSN 0094-243X
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
70 PLASMA PHYSICS AND FUSION TECHNOLOGY
CHAOS THEORY
DISTRIBUTION
DISTRIBUTION FUNCTIONS
EQUILIBRIUM
FLUCTUATIONS
HELIOSPHERE
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
PHASE TRANSFORMATIONS
SOLAR WIND
TRIPLETS
VELOCITY