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1 Introduction Interplanetary scintillation (IPS) is the amplitude and phase scintillation at radio frequencies from compact sources caused by density irregularities in the solar wind (Coles, 1978). IPS has an extensive history of capturing and studying heliospheric structures (Hewish, 1989), such as stream interaction regions (SIR, Dennison & Wiseman, 1968; Hewish & Bravo, 1986).
1 Introduction Interplanetary scintillation (IPS) was discovered in 1964 (Clarke, 1964; Hewish et al., 1964). It was observed as amplitude scintillation at radio wavelengths as radiation from compact objects (0.3 arcsec for 162 MHz) traverse through the irregularities of the solar wind (Coles, 1978). IPS, as a general technique, has been used to study the solar wind, solar wind transients, and for inner-heliospheric observations for over 55 years.
Comparison With ISEE Data In the bottom panel of Figure 2 we compare our data with g-levels measured by the IPS facility operated by the ISEE in Japan (Kojima & Kakinuma, 1990; Tokumaru, 2013).
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