Observations of interaction regions and corotating shocks between one and five AU: Pioneers 10 and 11

Smith, E. J.; Wolfe, J. H.

doi:10.1029/gl003i003p00137

Cited by 456 publications

(270 citation statements)

References 16 publications

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“…1 that there are many potential shocks. At 5 AU, most shocks are associated with corotating interaction regions (CIRs) (e.g., Smith & Wolfe 1976;Echer et al 2010, and references therein), but the interplanetary remnants of coronal mass ejections (ICMEs) are also present, such as the big peak of solar wind speed reaching 1000 km s −1 in this data set (de Koning et al 2005). Figure 2 shows the distribution of the occurrence of non-Io DAM emissions in the CML Io phase plane.…”

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confidence: 99%

Solar wind effects on Jupiter non-Io DAM emissions during Ulysses distant encounter (2003–2004)

Echer

Zarka

González

et al. 2010

A&A

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Aims. We analyze solar wind data from the Ulysses spacecraft during the distant Jupiter encounter from 2003 November to 2004 March as well as Nançay decametric (DAM) radio observations non-controlled by Io. Methods. The Ulysses solar wind data are balistically propagated towards Jupiter and are correlated with Nançay non-Io DAM emissions. Results. It is found that the average solar wind dynamic pressure around the time of DAM emissions is 1.7 times higher than its average value during the Ulysses encounter. The occurrence of fast forward (FS) and reverse (RS) interplanetary shocks and heliospheric current sheet crossings (HCS) is correlated with the occurrence of non-Io DAM emissions. We note an enhanced probability of occurrence of non-Io DAM emissions after the expected arrival of FS, RS and HCS at Jupiter. However, about half emissions (54%) did not seem to be associated with these interplanetary structures. We also note that the average duration and power of non-Io DAM emissions are enhanced during periods associated with those interplanetary structures. Conclusions. From the results obtained in this work it seems that non-Io DAM emissions occur during intervals of enhanced solar wind dynamic pressure. Yet, there is no direct correlation between the non-Io DAM emissions duration or power versus the solar wind pressure values and the interplanetary shock Mach number.

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Section: Html)mentioning

confidence: 99%

Solar wind effects on Jupiter non-Io DAM emissions during Ulysses distant encounter (2003–2004)

Echer

Zarka

González

et al. 2010

A&A

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“…However, due to the frozen-in nature of the solar wind flow, the interplanetary magnetic field (IMF) magnitude measured by Cassini MAG can be used as a proxy for the solar wind dynamic pressure. In general, a compression region in the solar wind will be observed as an increase in IMF magnitude, bounded by forward and reverse shocks (Smith and Wolfe, 1976;Gosling and Pizzo, 1999). As heliospheric current sheet (HCS) crossings usually occur within CIR compression regions in the solar wind, a reversal in the sense of the B T interplanetary field component (RTN coordinates) can further be used to identify a CIR compression event (Gosling and Pizzo, 1999).…”

Section: Cassini Measurements Of Skr Emissions and Interplanetary Magmentioning

confidence: 99%

Relationship between solar wind corotating interaction regions and the phasing and intensity of Saturn kilometric radiation bursts

et al. 2008

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Abstract. Voyager spacecraft measurements of Saturn kilometric radiation (SKR) identified two features of these radio emissions: that they pulse at a period close to the planetary rotation period, and that the emitted intensity is correlated with the solar wind dynamic pressure (Desch and Kaiser, 1981; Desch, 1982;Desch and Rucker, 1983). In this study the inter-relation between the intensity and the pulsing of the SKR is analysed using Cassini spacecraft measurements of the interplanetary medium and SKR over the interval encompassing Cassini's approach to Saturn, and the first extended orbit. Cassini Plasma Spectrometer ion data were only available for a subset of the dates of interest, so the interplanetary conditions were studied primarily using the nearcontinuously available magnetic field data, augmented by the ion moment data when available. Intense SKR bursts were identified when solar wind compressions arrived at Saturn. The intensity of subsequent emissions detected by Cassini during the compression intervals was variable, sometimes remaining intense for several planetary rotations, sometimes dimming and rarely disappearing. The timings of the initial intense SKR peaks were sometimes independent of the longterm pulsing behaviour identified in the SKR data. Overall, however, the pulsing of the SKR peaks during the disturbed intervals was not significantly altered relative to that during non-compression intervals.

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“…The boundary within the compression region, separating the slow and fast wind, is known as a stream interface (SI) (Gosling et al, 1978). In the simplest possible scenario, where speed variations depend only on their source location at the Sun, that is, the flow pattern does not vary significantly on the time scale of a solar rotation (such as at solar minimum), the large-scale compressive structures created by the interactions of these streams are fixed in a frame corotating with the Sun, and they are known as corotating interaction regions (CIRs, Smith and Wolfe, 1976). If the speed difference is sufficiently large, and typically beyond about 2 AU, a pair of shocks may form, bounding the CIR (e.g., Pizzo, 1985).…”

Section: Corotating Interaction Regionsmentioning

confidence: 99%

Global MHD Modeling of the Solar Corona and Inner Heliosphere for the Whole Heliosphere Interval

et al. 2011

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In an effort to understand the three-dimensional structure of the solar corona and inner heliosphere during the Whole Heliosphere Interval (WHI), we have developed a global magnetohydrodynamics (MHD) solution for Carrington rotation (CR) 2068. Our model, which includes energy-transport processes, such as coronal heating, conduction of heat parallel to the magnetic field, radiative losses, and the effects of Alfvén waves, is capable of producing significantly better estimates of the plasma temperature and density in the corona than have been possible in the past. With such a model, we can compute emission in extreme ultraviolet (EUV) and X-ray wavelengths, as well as scattering in polarized white light. Additionally, from our heliospheric solutions, we can deduce magnetic-field and plasma parameters along specific spacecraft trajectories. In this paper, we present a general analysis of the large-scale structure of the solar corona and inner heliosphere during WHI, focusing, in particular, on i) helmet-streamer structure; ii) the location of the heliospheric current sheet; and iii) the geometry of corotating interaction regions. We also compare model results with i) EUV observations from the EIT instrument onboard SOHO; and ii) in-situ measurements made by the STEREO-A and B spacecraft. Finally, we contrast the global structure of the corona and inner heliosphere during WHI with its structure during the Whole Sun Month (WSM) interval. Overall, our model reproduces the essential features of the observations; however, many discrepancies are present. We discuss several likely causes for them and suggest how model predictions may be improved in the future.

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Observations of interaction regions and corotating shocks between one and five AU: Pioneers 10 and 11

Cited by 456 publications

References 16 publications

Solar wind effects on Jupiter non-Io DAM emissions during Ulysses distant encounter (2003–2004)

Solar wind effects on Jupiter non-Io DAM emissions during Ulysses distant encounter (2003–2004)

Relationship between solar wind corotating interaction regions and the phasing and intensity of Saturn kilometric radiation bursts

Global MHD Modeling of the Solar Corona and Inner Heliosphere for the Whole Heliosphere Interval

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