Properties of Stream Interactions at One AU During 1995 – 2004

Jian, L. K.; Russell, C. T.; Luhmann, J. G.; Skoug, R. M.

doi:10.1007/s11207-006-0132-3

Cited by 271 publications

(354 citation statements)

References 49 publications

Supporting

Mentioning

328

Contrasting

Unclassified

Order By: Relevance

“…Two statistical studies, by Cane & Richardson (2003) and Jian et al (2006a), have produced ICME lists for solar cycle 23, but no ICME was reported during these SEP events. As another alternative of a local disturbance, we also checked the stream interaction region list by Jian et al (2006b), and, again, no such structure was detected during the day of the events (see also the middle panel of Fig. 1).…”

Section: Discussionmentioning

confidence: 99%

Observation of a solar energetic particle event behind previous coronal mass ejection

Al-Sawad

Saloniemi

Laitinen

et al. 2009

A&A

View full text Add to dashboard Cite

On 2001 October 19-21 the Energetic and Relativistic Nuclei and Electron (ERNE) instrument on the Solar and HeliosphericObservatory (SOHO) observed two gradual solar energetic particle (SEP) events separated by 15 h, in association with two X1.6/2B solar flares and halo coronal mass ejections (CMEs). The observational data suggest that the second acceleration of ∼10−100 MeV protons occurred behind the first CME and the previous CME was not an obstacle for new particles to directly reach 1 AU. The proton flux anisotropy data support the idea that the particle production significantly declined in about 10 h after the shock wave started, while the prolonged temporal profile of the solar energetic particle event was due to a slow transport of previously accelerated particles in the interplanetary space. These observations call into question the view that in all gradual events high-energy particles are continuously produced at a CME bow shock as it travels from near the Sun to beyond 1 AU.

show abstract

Section: Discussionmentioning

confidence: 99%

Observation of a solar energetic particle event behind previous coronal mass ejection

Al-Sawad

Saloniemi

Laitinen

et al. 2009

A&A

View full text Add to dashboard Cite

show abstract

“…The spectra are taken during four time intervals, which are marked in blue, gray, cyan, and red. In the solar wind speed and density data one can clearly identify the SIR at approximately DoY 127 -129 by the strong increase in density, which is subsequently followed by a sudden drop and then an increase in solar wind speed (see Jian et al 2006). The blue and red periods correspond to comparatively undisturbed solar wind before and after the SIR, respectively.…”

Section: Acceleration Sitesmentioning

confidence: 93%

Challenges in the determination of the interstellar flow longitude from the pickup ion cutoff

Taut

Berger

Möbius

et al. 2018

A&A

View full text Add to dashboard Cite

Context. The interstellar flow longitude corresponds to the Sun's direction of movement relative to the local interstellar medium. Thus, it constitutes a fundamental parameter for our understanding of the heliosphere and, in particular, its interaction with its surroundings, which is currently investigated by the Interstellar Boundary EXplorer (IBEX). One possibility to derive this parameter is based on pickup ions (PUIs) that are former neutral ions that have been ionized in the inner heliosphere. The neutrals enter the heliosphere as an interstellar wind from the direction of the Sun's movement against the partially ionized interstellar medium. PUIs carry information about the spatial variation of their neutral parent population (density and flow vector field) in their velocity distribution function. From the symmetry of the longitudinal flow velocity distribution, the interstellar flow longitude can be derived. Aims. The aim of this paper is to identify and eliminate systematic errors that are connected to this approach of measuring the interstellar flow longitude; we want to minimize any systematic influences on the result of this analysis and give a reasonable estimate for the uncertainty. Methods. We use He + data measured by the PLAsma and SupraThermal Ion Composition (PLASTIC) sensor on the Solar TErrestrial RElations Observatory Ahead (STEREO A) spacecraft. We analyze a recent approach, identify sources of systematic errors, and propose solutions to eliminate them. Furthermore, a method is introduced to estimate the error associated with this approach. Additionally, we investigate how the selection of interplanetary magnetic field angles, which is closely connected to the pickup ion velocity distribution function, affects the result for the interstellar flow longitude. Results. We find that the revised analysis used to address part of the expected systematic effects obtains significantly different results than presented in the previous study. In particular, the derived uncertainties are considerably larger. Furthermore, an unexpected systematic trend of the resulting interstellar flow longitude with the selection of interplanetary magnetic field orientation is uncovered.

show abstract

“…For times through the end of 2004, all the CIRs in the survey (except No. 22) were included in the comprehensive list from Jian et al (2006), who selected events on the basis of plasma and field data. Figure 1 shows a sample event with ACE SWEPAM solar wind speed, ULEIS O intensities, and a particle arrival spectrogram that illustrates the dispersionless nature of the event.…”

Section: Event Selectionmentioning

confidence: 99%

Abundances and Energy Spectra of Corotating Interaction Region Heavy Ions Observed during Solar Cycle 23

Mason

Leske

Desai

et al. 2008

ApJ

103

View full text Add to dashboard Cite

Using instruments on the ACE spacecraft, we surveyed the heavy-ion spectra and composition over the range HeFe for 41 corotating interaction regions (CIRs) during 1998-2007. Below $1 MeV nucleon À1 the spectra are power laws in kinetic energy nucleon À1 with an average spectral index of 2:51 AE 0:10, rolling over above $1 MeV nucleon À1 to power-law spectra with an average index of 4:47 AE 0:17. The spectral shapes for different species are similar, leading to relative abundances that are constant over our energy range, even though the intensities cover up to 8 orders of magnitude. Relative to oxygen, the measured abundances at 385 keV nucleon À1 for 4 He, C, N, Ne, Mg, Si, S, Ca, and Fe are 273 AE 72, 0:760 AE 0:023, 0:143 AE 0:005, 0:206 AE 0:009, 0:148 AE 0:006, 0:095 AE 0:005, 0:028 AE 0:002, 0:007 AE 0:001, and 0:088 AE 0:007, respectively. Except for an overabundance of 4 He and Ne, the abundances are quite close to that of the fast solar wind. We have found 3 He/ 4 He ratios to be enhanced over solar wind values in $40% of the CIRs. The Fe/O ratio in individual CIRs is observed to vary over a factor of $10 and is strongly correlated with the solar wind Fe/O ratio measured 2-4 days preceding each CIR. Taken together with previous studies showing the presence of pickup He + in CIRs, the observational data provide evidence that CIR energetic particles are accelerated out of a suprathermal ion pool that includes heated solar wind ions, pickup ions, and remnant suprathermals from impulsive solar energetic particle events.

show abstract

Properties of Stream Interactions at One AU During 1995 – 2004

Cited by 271 publications

References 49 publications

Observation of a solar energetic particle event behind previous coronal mass ejection

Observation of a solar energetic particle event behind previous coronal mass ejection

Challenges in the determination of the interstellar flow longitude from the pickup ion cutoff

Abundances and Energy Spectra of Corotating Interaction Region Heavy Ions Observed during Solar Cycle 23

Contact Info

Product

Resources

About