Physics
Scientific paper
Jul 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005jgra..11007110b&link_type=abstract
Journal of Geophysical Research, Volume 110, Issue A7, CiteID A07110
Physics
11
Interplanetary Physics: Interplanetary Magnetic Fields, Interplanetary Physics: Mhd Waves And Turbulence (2752, 6050, 7836), Interplanetary Physics: Solar Cycle Variations (7536), Interplanetary Physics: General Or Miscellaneous
Scientific paper
The solar wind is a driven nonlinear, nonequilibrium system with large jumps and fluctuations in the temporal profiles of the magnetic field strength B. Relatively large clusters of strong fields (``merged interaction regions,'' MIRs) form beyond 1 AU, grow out to ~5-30 AU, and decay slowly between ~30 AU and at least 90 AU. We analyze the probability distribution functions (PDFs) of fluctuations of B observed by Voyager 1 between 7 and 87 AU on scales from 1 to 128 days during each of four years (1980, 1991, 2001, and 2002). The 32 PDFs of the increments of B can be described by a single function, the q-exponential distribution of the nonextensive Tsallis statistical mechanics. The tails of the PDFs are described by the entropic index q, which is scale dependent. The Tsallis distribution has a finite variance when q < 5/3 and a divergent moment when q >= 5/3. For the 1980 and 1991 data (near 8 and 45 AU, respectively), q >= 5/3 at all scales, owing to large tails of the PDFs caused by large fluctuations and jumps in B(t). For the 2001 and 2002 data (between 80 and 87 AU), q < 5/3, and q approaches 1 (the PDF tends to a Gaussian) at large scales. The standard deviation and kurtosis of the observed increments of B vary with the scale of the fluctuations. The transition from q > 5/3 at <45 AU to q < 5/3 at >80 AU suggests the possibility of a phase transition in the distant heliosphere.
Burlaga Leonard Francis
Viñas Adolfo F.
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