Abstract
Abstract. The variation of the peak intensity of energetic ions accelerated at CIR related shocks in the interplanetary medium as observed by instruments on board of ULYSSES during its pass towards the south polar region and from the north polar region back to its aphelium is discussed. From ULYSSES measurements alone it cannot be decided whether the observed variation is a function of latitude or of radial distance, as its orbit changes distance and latitude at the same time. Therefore ULYSSES data is compared with earlier observations by the PIONEER and VOYAGER spacecraft and concluded that the major part of the observed variation of the peak intensity seems to be due to a radial distance change, on to which, however, at higher latitudes a latitude dependent feature is superimposed.Key words. Interplanetary physics (Energetic particles; interplanetary shocks; general)
Highlights
It is well known that corotating structures are formed by fast solar wind streams ramming into slow solar wind ahead
The PIONEER 10/11 observations were obtained in the ecliptic plane, and have been interpreted as showing a radial gradient
If this inference is true, the ULYSSES observations could be interpreted as showing a radial gradient
Summary
It is well known that corotating structures are formed by fast solar wind streams ramming into slow solar wind ahead. In the picture described by Fisk (1996) the observed particles would have moved along a magneticux tube which temporarily connected the observer to the shock surface These observed CIR relateduxes encountered at high latitudes are due to the topological structure of the heliospheric magnetic ®elds, and latitude dependent. This model has been used by Roelof and Simnett (1996) to explain the increasing time lag between shock accelerated energetic electrons (E > 50 keV) and ions once the shocks no longer passed the S/C.
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