Volume 439, Number 3, September I 2005
|Page(s)||1165 - 1169|
|Published online||12 August 2005|
Phase scintillation observation during coronal sounding experiments with NOZOMI spacecraft
Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1, Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan e-mail: email@example.com
2 Nara Women's University, Kita-uoya Nishi-machi, Nara 630-8506, Japan
3 Institute of Radio Engineering and Electronics of the Russian Academy of Sciences, Russia
4 Solar-Terrestrial Environment Laboratory, Nagoya University, Honohara 3-13, Toyokawa, Aichi 442-8507, Japan
Accepted: 11 April 2005
Radio occultation observations of the solar corona at solar offset distances of 12.8–36.9 RS were performed from December of 2000 to January of 2001, using the Nozomi spacecraft (Planet-B) of Japan. Phase scintillation spectra up to the frequency of ~10 Hz were obtained in two-way mode with S-band uplink and X-band downlink. The spectra cannot be represented by a single power law especially for small offset distances. That is, at low frequencies (large scales) the spectra show slopes indicative of Kolmogorov, a local flattening occurs from ~0.5 Hz (scale ~600 km) to ~3 Hz (~100 km), and a steepening occurs again at higher frequencies. This three-component nature of the spectrum was observed with a single method for the first time, although the spectral shape is variable and the three-component feature is not always evident.
Key words: Sun: corona / Sun: solar wind / turbulence
© ESO, 2005
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