Unusual composition of the solar wind in the 2–3 May 1998 CME observed with SWICS on ACE

Gloeckler, G.; Fisk, L. A.; Hefti, S.; Schwadron, N. A.; Zurbuchen, T. H.; Ipavich, F. M.; Geiss, J.; Bochsler, P.; Wimmer‐Schweingruber, R. F.

doi:10.1029/1998gl900166

Cited by 111 publications

(60 citation statements)

References 9 publications

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“…[Schwenn et al, 1980;Rakowski et al, 2007], being present. For these candidate ions, Gloeckler et al [1999] compared the charge state distribution in a CME event with that in slow solar wind as measured by ACE. The results indicated that in the CME the density of He + obviously increased.…”

Section: Observational Resultsmentioning

confidence: 99%

Identification of prominence ejecta by the proton distribution function and magnetic fine structure in interplanetary coronal mass ejections in the inner heliosphere

Yao

Marsch

et al. 2010

J. Geophys. Res.

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[1] This work presents in situ solar wind observations of three magnetic clouds (MCs) that contain cold high-density material when Helios 2 was located at 0.3 AU on 9 May 1979, 0.5 AU on 30 March 1976, and 0.7 AU on 24 December 1978. In the cold high-density regions embedded in the interplanetary coronal mass ejections we find (1) that the number density of protons is higher than in other regions inside the magnetic cloud, (2) the possible existence of He + , (3) that the thermal velocity distribution functions are more isotropic and appear to be colder than in the other regions of the MC, and the proton temperature is lower than that of the ambient plasma, and (4) that the associated magnetic field configuration can for all three MC events be identified as a flux rope. This cold high-density region is located at the polarity inversion line in the center of the bipolar structure of the MC magnetic field (consistent with previous solar observation work that found that a prominence lies over the neutral line of the related bipolar solar magnetic field). Specifically, for the first magnetic cloud event on 8 May 1979, a coronal mass ejection (CME) was related to an eruptive prominence previously reported as a result of the observation of Solwind (P78-1). Therefore, we identify the cold and dense region in the MC as the prominence material. It is the first time that prominence ejecta were identified by both the plasma and magnetic field features inside 1 AU, and it is also the first time that the thermal ion velocity distribution functions were used to investigate the microstate of the prominence material. Moreover, from our three cases, we also found that this material tended to fall behind the magnetic cloud and become smaller as it propagated farther away from the Sun, which confirms speculations in previous work. Overall, our in situ observations are consistent with three-part CME models.Citation: Yao, S., E. Marsch, C.-Y. Tu, and R. Schwenn (2010), Identification of prominence ejecta by the proton distribution function and magnetic fine structure in interplanetary coronal mass ejections in the inner heliosphere,

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Section: Observational Resultsmentioning

confidence: 99%

Identification of prominence ejecta by the proton distribution function and magnetic fine structure in interplanetary coronal mass ejections in the inner heliosphere

Yao

Marsch

et al. 2010

J. Geophys. Res.

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“…IMPACT field and electron measurements, coupled with PLASTIC measurements of the plasma ion composition, can be used to distinguish the magnetic fields in the filamentary material from those of other parts of the ICME structure, and examine their relationship, an important step toward resolving the source region question (e.g. Gloeckler et al 1999).…”

Section: The Solar Magnetic Cyclementioning

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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“…Observations of soft X-ray loops as well as of chromospheric flare ribbons indicate that reconnection occurs initially along highly sheared loops and only later do the magnetic field lines make a transition to more potential arcade loops (Canfield et al 2000;Martin & McAllister 1995;Su et al 2006) in a manner explained by models where reconnections take place initially in a sheared magnetic core (e.g., Moore et al 1997). A further analysis of flare ribbons implies that the bulk of magnetic cloud poloidal flux originates in reconnecting field lines (Qiu et al 2007), and studies of magnetic cloud charge states indicate possibly flare-associated heating along prominence-mass-carrying field lines (Skoug et al 1999;Gloeckler et al 1999;Reinard 2005). These observations indicate that the flux rope that escapes in the CME is made up of field lines that have undergone significant reconnection, as would be the case if the flux ropes were formed in situ during eruption, but which would not be the case for a pre-existing rope expanding in its entirety upwards without significant change of topology/connectivity.…”

Section: Introductionmentioning

confidence: 99%

Partially-erupting prominences: a comparison between observations and model-predicted observables

Tripathi

Gibson

Qiu

et al. 2009

A&A

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Aims. We investigate several partially-erupting prominences to study their relationship with other CME-associated phenomena and compare these observations with observables predicted by a model of partially-expelled-flux-ropes (Gibson & Fan 2006a, ApJ, 637, L65; 2006b, J. Geophys. Res., 111, 12103). Methods. We studied 6 selected events with partially-erupting prominences using multi-wavelength observations recorded by the Extreme-ultraviolet Imaging Telescope (EIT), Transition Region and Coronal Explorer (TRACE), Mauna Loa Solar Observatory (MLSO), Big Bear Solar Observatory (BBSO), and Soft X-ray Telescope (SXT). The observational features associated with partiallyerupting prominences were then compared with the predicted observables from the model. Results. The partially-expelled-flux-rope (PEFR) model can explain the partial eruption of these prominences, and in addition predicts a variety of other CME-related observables that provide evidence of internal reconnection during eruption. We find that all of the partially-erupting prominences studied in this paper exhibit indirect evidence of internal reconnection. Moreover, all cases showed evidence of at least one observable unique to the PEFR model, e.g., dimmings external to the source region and/or a soft X-ray cusp overlying a reformed sigmoid. Conclusions. The PEFR model provides a plausible mechanism to explain the observed evolution of partially-erupting-prominenceassociated CMEs in our study.

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Unusual composition of the solar wind in the 2–3 May 1998 CME observed with SWICS on ACE

Cited by 111 publications

References 9 publications

Identification of prominence ejecta by the proton distribution function and magnetic fine structure in interplanetary coronal mass ejections in the inner heliosphere

Identification of prominence ejecta by the proton distribution function and magnetic fine structure in interplanetary coronal mass ejections in the inner heliosphere

STEREO IMPACT Investigation Goals, Measurements, and Data Products Overview

Partially-erupting prominences: a comparison between observations and model-predicted observables

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