Turbulence in the Inner Solar Wind Determined from Frequency Fluctuations of the Downlink Signals from the ULYSSES and GALILEO Spacecraft

Details Turbulence in the Inner Solar Wind Determined from Frequency Fluctuations of the Downlink Signals from the ULYSSES and GALILEO Spacecraft Turbulence in the Inner Solar Wind Determined from Frequency Fluctuations of the Downlink Signals from the ULYSSES and GALILEO Spacecraft

Jun 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005arep...49..485e&link_type=abstract

Astronomy Reports, vol. 49, Issue 6, p.485-494

Astronomy and Astrophysics

Astronomy

5

Scientific paper

The results of several sets of measurements of the frequency of radio signals during coronal-sounding experiments carried out from 1991 to 2000 using the ULYSSES and GALILEO spacecraft are presented and analyzed. The S-band signals (carrier frequency f = 2295 MHz) were received at the three 70-m widely spaced ground stations of the NASA Deep Space Network. As a rule, the frequency-fluctuation spectra at frequencies above 1 mHz are power-laws. At small heliocentric distances, R < 10R &sun; (R &sun; is the solar radius), the spectral index is close to zero; this corresponds to a spectral index for the one-dimensional turbulence spectrum p 1 = 1. The index of the frequency-fluctuation spectra in the region of the supersonic solar wind at distances R > 30 R &sun; is between 0.5 and 0.7 (p 1 = 1.5 1.7). The results demonstrate a substantial difference between the turbulence regimes in these regions: in the region of the established solar wind, the power-law spectra are determined by nonlinear cascade processes that pump energy from the outer turbulence scale to the small-scale part of the spectrum, whereas such cascade processes are absent in the solar wind acceleration region. Near the solar minimum, the change in the turbulence regime of the fast, high-latitude solar wind occurs at greater distances than for the slow, low-latitude solar wind. Spectra with a sharp cutoff at high frequencies have been detected for the first time. Such spectra are observed only at R < 10 R &sun; and at sufficiently low levels of the electron density fluctuations. The measured cutoff frequencies are between 10 and 30 mHz; the cutoff frequency tends to increase with heliocentric distance. The variance of the plasma-density fluctuations has been estimated for the slow, low-latitude solar wind. These estimates suggest that the relative fluctuation level at distances 7 R &sun; < R < 30 R &sun; does not depend on heliocentric distance. The cross correlation of the frequency fluctuations recorded at widely spaced ground stations increases with the index of the frequency-fluctuation spectrum. At distances R ≈ 10 R &sun;, the rate of temporal changes in irregularities on the scale of several thousand kilometers is less than or comparable to the solar wind velocity.

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