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Observations of micro-turbulence in the solar wind near the sun with interplanetary scintillationVelocity and density turbulence of solar wind were inferred from interplanetary scintillation (IPS) observations at 2.3 GHz and 8.5 GHz using a single-antenna. The observations were made during September and October in 1992 - 1994. They covered the distance range between 5 and 76 solar radii (Rs). We applied the spectrum fitting method to obtain a velocity, an axial ratio, an inner scale and a power-law spectrum index. We examined the difference of the turbulence properties near the Sun between low-speed solar wind and high-speed solar wind. Both of solar winds showed acceleration at the distance range of 10 - 30 Rs. The radial dependence of anisotropy and spectrum index did not have significant difference between low-speed and high-speed solar winds. Near the sun, the radial dependence of the inner scale showed the separation from the linear relation as reported by previous works. We found that the inner scale of high-speed solar wind is larger than that of low-speed wind.
Document ID
Document Type
Conference Paper
Yamauchi, Y. (Nagoya Univ. Toyokawa, Japan)
Misawa, H. (Nagoya Univ. Toyokawa, Japan)
Kojima, M. (Nagoya Univ. Toyokawa, Japan)
Mori, H. (Communications Research Lab. Koganei, Japan)
Tanaka, T. (Communications Research Lab. Koganei, Japan)
Takaba, H. (Communications Research Lab. Kashima, Japan)
Kondo, T. (Communications Research Lab. Kashima, Japan)
Tokumaru, M. (Communications Research Lab. Hokkaido, Japan)
Manoharan, P. K. (Tata Inst. of Fundamental Research Ootacamund, India)
Date Acquired
August 17, 2013
Publication Date
June 30, 1995
Subject Category
Solar Physics
Distribution Limits
Work of the US Gov. Public Use Permitted.