An unusually fast interplanetary coronal mass ejection observed by Ulysses at 5 AU on 15 November 2003

Koning, C. A. de; Steinberg, J. T.; Gosling, J. T.; Reisenfeld, D. B.; Skoug, R. M.; Cyr, O. C. St.; Malayeri, M. L.; Balogh, A.; Rees, A.; McComas, D. J.

doi:10.1029/2004ja010645

Cited by 8 publications

(20 citation statements)

References 47 publications

(78 reference statements)

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“…In order to aid a visual comparison, a horizontal line has been drawn at unity representing the reference SEP value for the elements. The dashed vertical lines mark the times of forward (F) and reverse (R) shocks whereas the black horizontal bars denote the ICMEs observed during this period as identified by de Koning et al [2005] and Lario et al [2005]. F shocks in red indicate ICME‐driven shocks.…”

Section: Observations and Data Analysismentioning

confidence: 99%

“…The SIR/CIR intervals observed during this period are indicated by green dashed vertical lines. The red dashed bar indicates the ambiguity in the time of termination of the large 15 November 2003 [day of year (DOY) 319] ICME as noted by de Koning et al [2005]. Solid black triangles mark the times of X‐class flares (as reported by McKibben et al [2005]).…”

Section: Observations and Data Analysismentioning

confidence: 99%

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Energetic particle observations by Ulysses during the declining phase of solar cycle 23

et al. 2007

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[1] We present recent energetic particle measurements from 1-20 MeV/n recorded by the Ulysses/COSPIN/LET instrument from mid-October to the end of November 2003 and from May 2004 to the end of February 2005. Long-lasting periods with enhanced solar activity occurred during the declining phase of the current solar cycle contributing to the high-intensity particle events and heavy ion signatures observed by Ulysses near the ecliptic plane, at $5 AU from the Sun. The energetic particles injected from the Sun during the January 2005 intense solar activity were not observed at Ulysses until a stream interface that acted as a barrier for the particles reached the spacecraft. Our observations during this period thus show that the propagation of energetic particles is largely governed by the existence of large-scale solar wind structures that impede the transport of the particles. We use the elemental composition of the particle fluxes recorded by COSPIN/LET to gain insight into the possible origin of the particle events. We study and provide a possible interpretation of the composition signatures observed at $5 AU during periods of CME/CIR combinations. Although predominantly SEP-like, the observed composition showed evidence for enhancements in He, which we suggest is of interstellar origin, consistent with CIR shocks accelerating ions from multiple sources.

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Section: Observations and Data Analysismentioning

confidence: 99%

Section: Observations and Data Analysismentioning

confidence: 99%

Energetic particle observations by Ulysses during the declining phase of solar cycle 23

et al. 2007

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“…Spikes in speed were generally associated with fast ICMEs. These include ICMEs labeled 1 (∼2030 UT 11/15/03 to ∼1200 UT 11/21/03) [ de Koning et al , 2005], 2 (∼0445 UT 9/16/2004 to ∼0000 UT 09/21/2004) and 3 (∼1850 UT 1/29/2005 to ∼1800 UT 2/8/2005). In addition to transient events and an erratic stream structure, the average speed exhibited a long, slow variation over this interval, rising in the first half of 2003, falling through October 2004, and then rising again after that, particularly from June through September of 2005.…”

Section: Observationsmentioning

confidence: 99%

Ulysses observations of very different heliospheric structure during the declining phase of solar activity cycle 23

McComas¹,

Elliott²,

Gosling³

et al. 2006

Geophysical Research Letters

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[1] This study examines the most recent observations from the solar wind experiment (SWOOPS) on the Ulysses spacecraft. In contrast to observations over the same locations in the declining phase of the previous solar activity cycle, these data show a more complicated heliospheric structure. Around the start of 2003, a band of slow solar wind resided at $20°-25°N latitude at all heliolongitudes. Subsequently, Ulysses failed to observe a wellorganized corotating stream structure as it headed southward from the ecliptic plane, even though, in the previous solar cycle, Ulysses observed a regularly structured stream pattern. These observations show that the three-dimensional structure of the heliosphere can differ significantly from one solar cycle to the next. Finally, we show that the solar wind dynamic pressure has been relatively stable throughout 2005, indicating that the termination shock distance will also likely be relatively stable throughout 2006.

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“…The inward polarity high‐speed streams expected to be observed by ACE during the time interval of the October–November 2003 events were not easily identifiable. Similarly, the inward polarity CIR expected at Ulysses during the rotation on days 309–335 was not clearly distinguishable in the wake of the fast ICME observed by Ulysses on days 320–324 [ de Koning et al , 2005]. The outward polarity CIR expected at Cassini during the rotation on days 306–332 cannot be identified due to the passage of an enhanced transient magnetic field structure.…”

Section: Preevent and Postevent Structure Of The Heliospherementioning

confidence: 99%

“…From 19 October 2003 (day of year 292) to 5 November 2003 (day of year 309), 44 M‐class and 11 X‐class flares were observed [ Woods et al , 2004] coinciding with the transit of the NOAA active regions AR 0484, 0486, and 0488 over the disk of the Sun. The intense level of solar activity continued after these active regions crossed the west limb of the Sun [ de Koning et al , 2005]. The interplanetary consequences of these series of events extended over an even longer time interval.…”

Section: Introductionmentioning

confidence: 99%

Heliospheric energetic particle observations during the October–November 2003 events

et al. 2005

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[1] The intense level of solar activity recorded from 19 October to 12 November 2003 led to unusually high energetic particle intensities observed throughout the heliosphere. The fleet of spacecraft distributed in the inner and outer heliosphere offers us the opportunity to study both the effects of these events in different regions of the heliosphere and the evolution of the energetic particle intensities measured at different heliocentric radial distances. Observations at 1 AU by the ACE and GOES-11 spacecraft show multiple particle intensity enhancements associated with individual injections of solar energetic particles (SEPs) and with the arrival of shocks driven by coronal mass ejections (CMEs), resulting in a long time interval ($40 days) of elevated low-energy (<1 MeV) ion and near-relativistic (<315 keV) electron intensities. Observations from the Ulysses spacecraft at 5.2 AU, 6°north of the ecliptic, and 120-90°west of the Earth also showed elevated low-energy ion and near-relativistic electron intensities for more than $40 days that were modulated by the effects of recurrent corotating interaction regions (CIRs) and the passage of a fast interplanetary coronal mass ejection (ICME). The Cassini spacecraft at 8.7 AU, 3°south of the ecliptic, and 75-35°west of the Earth saw an intense low-energy ion and near-relativistic electron event in association with the passage of an enhanced magnetic field structure formed by the compression of transient solar wind flows and CIRs. The prompt component of the SEP event at Cassini was largely reduced due to the modulating effect of intervening transient flows propagating between the Sun and the spacecraft. The Voyager-2 spacecraft at 73 AU and 25°south of the ecliptic did not observe these events until April 2004. The arrival of a merged interaction region (MIR) at Voyager-2 produced a $70-day period with elevated <17 MeV proton and <60 keV electron intensities. Particle fluences computed over the duration of the events at each spacecraft show a radial dependence that decays more slowly than that expected from a simple model assuming adiabatic cooling of an isotropic particle population uniformly distributed in a shell symmetrically expanding at the solar wind speed. Although the SEP events were observed throughout the heliosphere, both (1) the solar particle injections occurring at different times and longitudes, and (2) the marked differences in the interplanetary stream structures propagating toward different longitudes resulted in distinct time-intensity histories at each spacecraft, and therefore periods with equal particle intensities were not observed by this fleet of spacecraft.

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An unusually fast interplanetary coronal mass ejection observed by Ulysses at 5 AU on 15 November 2003

Abstract: [1] On 15 November 2003, at $2030 UT, Ulysses/SWOOPS observed the onset of a large, unusually fast interplanetary coronal mass ejection (ICME) in the solar wind at 5.2 AU. Ulysses measured the peak solar wind flow speed associated with this event, v max = 993 km s À1

Cited by 8 publications

References 47 publications

Energetic particle observations by Ulysses during the declining phase of solar cycle 23

Energetic particle observations by Ulysses during the declining phase of solar cycle 23

Ulysses observations of very different heliospheric structure during the declining phase of solar activity cycle 23

Heliospheric energetic particle observations during the October–November 2003 events

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