Iron charge distribution as an identifier of interplanetary coronal mass ejections

Lepri, S. T.; Zurbuchen, T. H.; Fisk, L. A.; Richardson, I. G.; Cane, H. V.; Gloeckler, G.

doi:10.1029/2001ja000014

Cited by 201 publications

(202 citation statements)

References 35 publications

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“…These intervals cover interaction regions formed by the merging of interplanetary CMEs (ICMEs), commonly known as merged interaction regions (MIRs; Burlaga & Ness 1994). High ionization state Fe is observed in at least one-third of all ICMEs ( Lepri et al 2001;Lepri & Zurbuchen 2004), and these are obvious examples of a positive detection. Figure 14 (bottom) gives the ratio of flux in Fe xvii to the total Fe flux in Fe vii-Fe xvii.…”

Section: Ulysses Observationsmentioning

confidence: 99%

Current Sheet Evolution in the Aftermath of a CME Event

Бемпорад

Poletto

Suess

et al. 2006

ApJ

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We report on SOHO UVCS observations of the coronal restructuring following a coronal mass ejection (CME) on 2002 November 26, at the time of a SOHO-Ulysses quadrature campaign. Starting about 1.5 hr after a CME in the northwest quadrant, UVCS began taking spectra at 1.7 R , covering emission from both cool and hot plasma. Observations continued, with occasional gaps, for more than 2 days. Emission in the 974.8 8 line of [Fe xviii], indicating temperatures above 6 ; 10 6 K, was observed throughout the campaign in a spatially limited location. Comparison with EIT images shows the [Fe xviii] emission to overlie a growing post-flare loop system formed in the aftermath of the CME. The emission most likely originates in a current sheet overlying the arcade. Analysis of the [Fe xviii] emission allows us to infer the evolution of physical parameters in the current sheet over the entire span of our observations: in particular, we give the temperature versus time in the current sheet and estimate its density. At the time of the quadrature, Ulysses was directly above the location of the CME and intercepted the ejecta. High ionization state Fe was detected by the Ulysses SWICS throughout the magnetic cloud associated with the CME, although its rapid temporal variation suggests bursty, rather than smooth, reconnection in the coronal current sheet. The SOHOUlysses data set provided us with the unique opportunity of analyzing a current sheet structure from its lowest coronal levels out to its in situ properties. Both the remote and in situ observations are compared with predictions of theoretical CME models.

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Section: Ulysses Observationsmentioning

confidence: 99%

Current Sheet Evolution in the Aftermath of a CME Event

Бемпорад

Poletto

Suess

et al. 2006

ApJ

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“…Compressions from behind by a trailing high speed solar wind stream are also evident in some events, as are compositional signs that a filament of originally colder, denser coronal material forms a part of the observed ICME structures (e.g., Schwenn et al 1980;Gosling et al 1980;Skoug et al 1999). On the other hand, many ICMEs are characterized by ions of high charges states, indicating probable flare origins to some ICME material (e.g., Bame et al 1979;Lepri et al 2001).…”

Section: Interplanetary Consequencesmentioning

confidence: 99%

“…Several efforts described in the literature (e.g. Lario et al 1998;Li et al 2003) make use of MHD model simulations of interplanetary shocks as the basis for SEP spatial distribution and time profile descriptions that can be compared to multipoint or single spacecraft observations. The existence of the IMPACT modeling efforts and others are expected to lead to realistic and detailed SEP event descriptions that are consistent with both the SEP observations on STEREO and the related CME and ICME measurements and models.…”

Section: Sep Acceleration and Propagationmentioning

confidence: 99%

STEREO IMPACT Investigation Goals, Measurements, and Data Products Overview

et al. 2007

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The IMPACT (In situ Measurements of Particles And CME Transients) investigation on the STEREO mission was designed and developed to provide multipoint solar wind and suprathermal electron, interplanetary magnetic field, and solar energetic particle information required to unravel the nature of coronal mass ejections and their heliospheric consequences. IMPACT consists of seven individual sensors which are packaged into a boom suite, and a SEP suite. This review summarizes the science objectives of IMPACT, the instruments that comprise the IMPACT investigation, the accommodation of IMPACT on the STEREO twin spacecraft, and the overall data products that will flow from the IMPACT measurements. Accompanying papers in this volume of Space Science Reviews highlight the individual sensor technical details and capabilities, STEREO project plans for the use of IMPACT data, and modeling activities for IMPACT (and other STEREO) data interpretation.

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“…6 Enhancements in minor ions such as Fe and higher charge states of heavy ions such as Fe and O Lepri et al, 2001). …”

Section: Identification Of Icmesmentioning

confidence: 99%

Propagation and Evolution of ICMES in the Solar Wind

Richardson

Liu

Belcher

2005

NATO Science Series II: Mathematics, Physics and Chemistry

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Interplanetary coronal mass ejections (ICMEs) evolve as they propagate outward from the Sun. They interact with and eventually equilibrate with the ambient solar wind. One difficulty in studying this evolution is that ICMEs have no unique set of identifying characteristics, so boundaries of the ICMEs are difficult to identify. Two characteristics present in some ICMEs but generally not present in the ambient solar wind, high helium/proton density ratios and low temperature/speed ratios, are used to identify ICMEs. We search the Helios 1 and 2, WIND, ACE, and Ulysses data for ICMEs with these characteristics and use them to study the radial evolution of ICMEs. We find that the magnetic field magnitude and density decrease faster in ICMEs than in the ambient solar wind, but the temperature decreases more slowly than in the ambient solar wind. Since we also find that ICMEs expand in radial width with distance, the protons within ICMEs must be heated. Scale sizes for He structures are smaller than for proton structures within ICMEs.

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Iron charge distribution as an identifier of interplanetary coronal mass ejections

Cited by 201 publications

References 35 publications

Current Sheet Evolution in the Aftermath of a CME Event

Current Sheet Evolution in the Aftermath of a CME Event

STEREO IMPACT Investigation Goals, Measurements, and Data Products Overview

Propagation and Evolution of ICMES in the Solar Wind

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