Solar wind stream interfaces in corotating interaction regions: SWICS/Ulysses results

Wimmer‐Schweingruber, R. F.; Steiger, R. von; Paerli, Raoul

doi:10.1029/97ja00951

Cited by 93 publications

(68 citation statements)

References 20 publications

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“…Gosling et al (1978) suggested that the fast and slow solar wind streams have different origins. This was supported by later studies such as that of Wimmer-Schweingruber, von Steiger, and Paerli (1997), which showed that solar wind composition changed with the passage of a SI. In addition, Gosling et al (1978) also reported that the plasma in the vicinity of a SI undergoes an east -west deflection in the ecliptic plane.…”

Section: Solar Wind Stream Interfacessupporting

confidence: 69%

In Situ Observations of Solar Wind Stream Interface Evolution

et al. 2009

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The heliocentric orbits of the two STEREO satellites are similar in radius and ecliptic latitude, with separation in longitude increasing by about 45°per year. This arrangement provides a unique opportunity to study the evolution of stream interfaces near 1 AU over time scales of hours to a few days, much less than the period of a Carrington rotation. Assuming nonevolving solar wind sources that corotate with the Sun, we calculated the expected time and longitude of arrival of stream interfaces at the Ahead observatory based L.M. Blush now in Prilly, Switzerland.

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Section: Solar Wind Stream Interfacessupporting

confidence: 69%

In Situ Observations of Solar Wind Stream Interface Evolution

et al. 2009

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“…Intriligator and Siscoe (1994) noted that this signature was that of a relatively abrupt increase in specific entropy. More recently, Wimmer-Schweingruber, von Steiger, andPaerli (1997, 1999) used the data from the solar-wind ion-composition spectrometer (SWICS)/Ulysses instrument, to show additional evidence that the stream interface separates plasmas originating in Figure 1. Schematic illustrating 2-D corotating stream structure in the solar equatorial plane in the inner heliosphere (after Pizzo, 1978).…”

Section: Introductionmentioning

confidence: 99%

Properties of Stream Interactions at One AU During 1995 – 2004

et al. 2006

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Abstract.A stream interaction region (SIR) forms when a fast solar stream overtakes a slow stream, leading to structure that evolves as an SIR moves away from the Sun. Based on Wind (1995 -2004) and ACE (1998ACE ( -2004 in situ observations, we have conducted a comprehensive survey of SIRs at one AU, including a separate assessment of the longer-lasting corotating interaction regions (CIRs) that recur on more than one solar rotation. In all there are 196 CIRs, accounting for about 54% of the 365 SIRs. The largest proportion of CIRs to SIRs (64%) appears in 1999, and the smallest proportion (49%) is in 2002. Over the ten years, the annual number of SIR events varies little, from 32 up to 45. On average, the occurrence rate of shocks at SIRs at one AU is about 24%. Seventy percent of the SIRs with shocks have only forward shocks, more than twice the percentage of SIRs with only reverse shocks. This preponderance of forward shocks is consistent with the deflections of forward and reverse shocks relative to the ecliptic plane. In order to help address the effect of SIRs and CIRs on geomagnetic activity, we determine the solar-cycle variation of the event duration, scale size, the change in velocity from slow stream to fast stream, and the solar-cycle variation of the maximum magnetic field, peak total perpendicular pressure, and other properties. These statistics also provide a baseline for future studies at other heliocentric distances and for validating heliospheric models.

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“…Wimmer-Schweingruber et al, 1997). At the distances from the Sun accessible to EISCAT (15±120 R) the angle between the streams is too shallow for such dramatic e ects to be observed, although by 30 R conditions do allow a considerable degree of steepening in the interaction region, as discussed in Sect.…”

Section: Introductionmentioning

confidence: 99%

Interplanetary scintillation observations of interaction regions in the solar wind

et al. 1998

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Abstract. Co-rotating interaction regions (CIRs) between fast and slow streams of plasma are a prominent feature of the solar wind. Measurements of interplanetary scintillation (IPS) using the three widely separated antennas of the EISCAT facility have been used to detect the compression regions at the leading edges of interaction regions and to determine the location and velocity of the structure. Observations show that interaction regions have developed as close to the Sun as 25±30 solar radii, a result supported by theoretical modelling which shows that the conditions needed for CIRs to develop exist inside 30 solar radii.

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Solar wind stream interfaces in corotating interaction regions: SWICS/Ulysses results

Cited by 93 publications

References 20 publications

In Situ Observations of Solar Wind Stream Interface Evolution

In Situ Observations of Solar Wind Stream Interface Evolution

Properties of Stream Interactions at One AU During 1995 – 2004

Interplanetary scintillation observations of interaction regions in the solar wind

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