A prolonged He<sup>+</sup> enhancement within a coronal mass ejection in the solar wind

Skoug, R. M.; Bame, S. J.; Feldman, W. C.; Gosling, J. T.; McComas, D. J.; Steinberg, J. T.; Tokar, R. L.; Riley, Pete; Burlaga, L. F.; Ness, N. F.; Smith, C. W.

doi:10.1029/1998gl900207

Cited by 91 publications

(94 citation statements)

References 14 publications

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“…Several studies have examined the solar and heliospheric aspects of this event (Gloeckler et al, 1999;Skoug et al, 1999;Farrugia et al, 2002), and details of the solar wind and interplanetary magnetic field can be found therein. It is actually this stream that hits early on 4 May 1998, after the cloud had passed by geospace on 2-3 May 1998.…”

Section: The 1-7 May 1998 Stormmentioning

confidence: 99%

Magnetospheric convection electric field dynamics andstormtime particle energization: case study of the magneticstorm of 4 May 1998

Khazanov

Liemohn²,

Newman³

et al. 2004

Ann. Geophys.

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Abstract. It is shown that narrow channels of high electric field are an effective mechanism for injecting plasma into the inner magnetosphere. Analytical expressions for the electric field cannot produce these channels of intense plasma flow, and thus, result in less entry and adiabatic energization of the plasma sheet into near-Earth space. For the ions, omission of these channels leads to an underprediction of the strength of the stormtime ring current and therefore, an underestimation of the geoeffectiveness of the storm event. For the electrons, omission of these channels leads to the inability to create a seed population of 10-100 keV electrons deep in the inner magnetosphere. These electrons can eventually be accelerated into MeV radiation belt particles. To examine this, the 1-7 May 1998 magnetic storm is studied with a plasma transport model by using three different convection electric field models: Volland-Stern, Weimer, and AMIE. It is found that the AMIE model can produce particle fluxes that are several orders of magnitude higher in the L = 2 − 4 range of the inner magnetosphere, even for a similar total cross-tail potential difference.

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Section: The 1-7 May 1998 Stormmentioning

confidence: 99%

Magnetospheric convection electric field dynamics andstormtime particle energization: case study of the magneticstorm of 4 May 1998

Khazanov

Liemohn²,

Newman³

et al. 2004

Ann. Geophys.

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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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“…Given its relatively cool temperatures, filament material in the corona is dominated by heavy ion charge states such as C 2−3+ , O 2−4+ and Fe 4−6+ , which have been directly observed with SOHO/UVCS (e.g., Lee and Raymond 2012). Filament material can be ejected into interplanetary space where it can be distinguished by these ionization states (Schwenn et al 1980;Burlaga et al 1998;Skoug et al 1999;Yao et al 2010). Gopalswamy et al (1998) provides a clear example of the identification of low charge state filament material in the 07-11 February 1997 CME/ICME event.…”

Section: Plasma Evolutionmentioning

confidence: 99%

The Physical Processes of CME/ICME Evolution

et al. 2017

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As observed in Thomson-scattered white light, coronal mass ejections (CMEs) are manifest as large-scale expulsions of plasma magnetically driven from the corona in the most energetic eruptions from the Sun. It remains a tantalizing mystery as to how these erupting magnetic fields evolve to form the complex structures we observe in the solar wind at Earth. Here, we strive to provide a fresh perspective on the post-eruption and interplanetary evolution of CMEs, focusing on the physical processes that define the many complex interactions of the ejected plasma with its surroundings as it departs the corona and propagates through the heliosphere. We summarize the ways CMEs and their interplanetary CMEs (ICMEs) are rotated, reconfigured, deformed, deflected, decelerated and disguised during their journey through the solar wind. This study then leads to consideration of how structures originating in coronal eruptions can be connected to their far removed interplanetary counterparts. Given that ICMEs are the drivers of most geomagnetic storms (and the sole driver of extreme storms), this work provides a guide to the processes that must be considered in making space weather forecasts from remote observations of the corona.

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A prolonged He⁺ enhancement within a coronal mass ejection in the solar wind

Cited by 91 publications

References 14 publications

Magnetospheric convection electric field dynamics andstormtime particle energization: case study of the magneticstorm of 4 May 1998

Magnetospheric convection electric field dynamics andstormtime particle energization: case study of the magneticstorm of 4 May 1998

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

The Physical Processes of CME/ICME Evolution

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A prolonged He+ enhancement within a coronal mass ejection in the solar wind

Cited by 91 publications

References 14 publications

Magnetospheric convection electric field dynamics andstormtime particle energization: case study of the magneticstorm of 4 May 1998

Magnetospheric convection electric field dynamics andstormtime particle energization: case study of the magneticstorm of 4 May 1998

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

The Physical Processes of CME/ICME Evolution

Contact Info

Product

Resources

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A prolonged He⁺ enhancement within a coronal mass ejection in the solar wind