Mid-term periodicities in solar wind and IMF: Comparison between 1AU and outer heliosphere

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2162 Solar Cycle Variations (7536), 2164 Solar Wind Plasma, 7536 Solar Activity Cycle (2162)

Scientific paper

Richardson et al. (1994) found on a strong periodicity in solar wind (SW) speed with a period of about 1.3 years which dominated the SW speed time series after 1987. Gazis et al. (1995) has examined the SW speed data from several spacecraft, and verified that the 1.3-year periodicity was dominating the low-latitude heliosphere after 1987 from inner to outer heliosphere (almost 60 AU). More recently, Howe et al. (2000) found a 1.3-year periodicity in the variation of the solar rotation speed at the bottom of the convection layer. This suggests that the mid-term periodicities are a fundamental property related to the solar dynamo. Mursula and Zieger (1999, 2000) have demonstrated that mid-term periodicities are found during the last six solar cycles with different amplitudes and slightly varying periods in several heliospheric variables (solar wind, IMF, cosmic rays, geomagnetic activity) at 1 AU. Here we use the data on solar wind and IMF parameters outside 1 AU obtained by the Voyager and Pioneer probes to study the occurrence of mid-term periodicities in the outer heliosphere and to compare these periodicities in the inner and outer heliosphere. Gazis P. R. et al. Geophys. Res. Let., Vol. 22, NO.10, Pages 1165-1168, 1995. Howe R. et al. Science, Vol. 287, Pages 2456-2460, 2000. Mursula K. and B. Zieger, Proc. of the Cosmic Ray Conference, Utah, August 17-25, 1999, Vol. 7, Pages 123-126, 1999. Mursula K. and B. Zieger, Adv. Space Res. Vol. 25, NO.9, Pages 1939-1942, 2000. Richardson J. D. et al., Geophys. Res. Let., Vol 21. NO. 14, Pages 1559-1560, 1994.

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