Physics
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh53b1493m&link_type=abstract
American Geophysical Union, Fall Meeting 2006, abstract #SH53B-1493
Physics
4490 Turbulence (3379, 4568, 7863), 7836 Mhd Waves And Instabilities (2149, 2752, 6050), 7851 Shock Waves (4455), 7863 Turbulence (4490)
Scientific paper
The heliosheath was expected to be turbulent [Zank, 1999], the result of upstream turbulence and disturbances (shock waves, pressure and density enhancements, structures, etc. [Story, 1997]) being transmitted across and interacting with the heliospheric termination shock (HTS). A turbulent heliosheath has indeed been observed downstream of the HTS [Burlaga et al., 2006], but the character of the turbulence is significantly different from that of the solar wind. The 48-sec averages of the downstream magnetic field analyzed by Burlaga et al. [2006] reveal that the turbulence is isotropic, and each component has a Gaussian distribution. The distribution of 1-hour averages of the magnetic field was also Gaussian in the heliosheath, unlike the log-normal distributions found in the supersonic solar wind. The Gaussian distribution indicates a scale invariance in the form of the magnetic field distribution. The second intriguing observation was that the turbulence was substantially compressible since the width of the 48-sec magnetic field averages is greater than that for the components. Clearly MHD turbulence in the inner heliosheath is significantly different from that upstream of the HTS in the supersonic solar wind. Since the character of the turbulence is different immediately downstream of the HTS, it suggests that "processing" by the HTS plays an important role in modifying turbulent upstream fluctuations. On the basis of a linear model, we examine the transmission, amplification, and generation of turbulence by the HTS.
Ao Xianzhi
McKenzie James F.
Shaikh Dastgeer
Zank Gary P.
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