Untitled

Abstract

Ulysses observed a stable strong CIR from early 1992 through 1994 during its first journey into the southern hemisphere. After the rapid latitude scan in early 1995, Ulysses observed a weaker CIR from early 1996 to mid-1997 in the northern hemisphere as it traveled back to the ecliptic at the orbit of Jupiter. These two CIRs are the observational basis of the investigation into the latitudinal structure of CIRs. The first CIR was caused by an extension of the northern coronal hole into the southern hemisphere during declining solar activity, whereas the second CIR near solar minimum activity was caused by small warps in the streamer belt. The latitudinal structure is described through the presentation of three 26-day periods during the southern CIR. The first at 24 S shows the full plasma interaction region including fast and slow wind streams, the compressed shocked flows with embedded stream interface and heliospheric current sheet (HCS), and the forward and reverse shocks with associated accelerated ions and electrons. The second at 40 S exhibits only the reverse shock, accelerated particles, and the 26-day modulation of cosmic rays. The third at 60 S shows only the accelerated particles and modulated cosmic rays. The possible mechanisms for the access of the accelerated particles and the CIR-modulated cosmic rays to high latitudes above the plasma

Solar wind stream interaction regions throughout the heliosphere

“…(1998), Kunow et al. (1999), Lanzerotti and Sanderson (2001) and Heber et al. (1999), for reviews of these observations.…”

“…Kunow et al. (1999) also focus on observations of interaction regions during the first orbit, while Gosling and Pizzo (1999) review the three-dimensional structure of stream interaction regions from a modeling perspective.

Fig. 35Left: Solar wind observations made during the first orbit of the Ulysses mission, specifically the magnetic field intensity, proton temperature, density and speed, , , and Fe/O ratios and mean Fe charge state.

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POSSIBLE EVIDENCE FOR A FISK-TYPE HELIOSPHERIC MAGNETIC FIELD. I. ANALYZINGULYSSES/KET ELECTRON OBSERVATIONS

“…Hence, the influence of the HMF structure may be masked by other interplanetary phenomena. During the second potential period from 1995.6 to 1996.3, Heber et al (1997) and Kunow et al (1999) could show that CIR particle events and CIR related cosmic ray decreases were first observed from 1996.0 onward. The left panel of Figure 5 presents the expected detrended 7 MeV electron intensities yielded by the model along the Ulysses trajectory when the spacecraft was located between 80 • N and 40 • N heliographic latitude.…”

A Numerical Study of the Effects of a Corotating Interaction Region on Cosmic-Ray Transport. II. Features of Cosmic-Ray Composition and Rigidity

“…Their strength evidently varies with rigidity over time (solar activity). They are also observed by ground-based neutron monitors (NMs; e.g., Gil & Alania 2016), at high heliolatitudes by Ulysses (Kunow et al 1995;Heber et al 1999), and even beyond 60 au by Voyager 1 (Decker et al 1999; see the reviews by Gazis et al 1999;Kunow et al 1999;McKibben et al 1999). Of particular interest is how the value of the maximum decrease of these GCR variations depends on rigidity, which is usually reported as the "amplitude of the 27 day variation," as done by Modzelewska et al (2020).…”