Analysis of the substructure within a complex magnetic cloud on 3–4 September 2008

Andréeová, K.; Kilpua, Emilia; Hietala, Heli; Koskinen, H.; Isavnin, Alexey; Vainio, R.

doi:10.5194/angeo-31-555-2013

Cited by 2 publications

(2 citation statements)

References 24 publications

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“…4) could be signatures of the processes that separate the flux rope from the surrounding ICME. Such substructures have been reported regularly at MC/flux ropes boundaries (e.g., Farrugia et al, 2001;Wei et al, 2002;Andreeova et al, 2013) and their electron and proton flux variations are similar to those in the reconnection exhausts (Wang et al, 2012).…”

Section: Summary and Discussionmentioning

confidence: 73%

On the relationship between interplanetary coronal mass ejections and magnetic clouds

et al. 2013

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Abstract. The relationship of magnetic clouds (MCs) to interplanetary coronal mass ejections (ICMEs) is still an open issue in space research. The view that all ICMEs would originate as magnetic flux ropes has received increasing attention, although near the orbit of the Earth only about one-third of ICMEs show clear MC signatures and often the MC occupies only a portion of the more extended region showing ICME signatures. In this work we analyze 79 events between 1996 and 2009 reported in existing ICME/MC catalogs (Wind magnetic cloud list and the Richardson and Cane ICME list) using near-Earth observations by ACE (Advanced Composition Explorer) and Wind. We perform a systematic comparison of cases where ICME and MC signatures coincided and where ICME signatures extended significantly beyond the MC boundaries. We find clear differences in the characteristics of these two event types. In particular, the events where ICME signatures continued more than 6 h past the MC rear boundary had 2.7 times larger speed difference between the ICME's leading edge and the preceding solar wind, 1.4 times higher magnetic fields, 2.1 times larger widths and they experienced three times more often strong expansion than the events for which the rear boundaries coincided. The events with significant mismatch in MC and ICME boundary times were also embedded in a faster solar wind and the majority of them were observed close to the solar maximum. Our analysis shows that the sheath, the MC and the regions of ICME-related plasma in front and behind the MC have different magnetic field, plasma and charge state characteristics, thus suggesting that these regions separate already close to the Sun. Our study shows that the geometrical effect (the encounter through the CME leg and/or far from the flux rope center) does not contribute much to the observed mismatch in the MC and ICME boundary times.

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Section: Summary and Discussionmentioning

confidence: 73%

On the relationship between interplanetary coronal mass ejections and magnetic clouds

et al. 2013

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“…Using multiple spacecraft, gradients are resolved, and the IMF can be determined at a specific location around Earth's magnetosphere. Such localized predictions are important considering the scale sizes of solar wind structure (Andréeová et al, 2013;Borovsky, 2018;Kessel et al, 1999). For example, a significant rotation of the IMF occurring over 10 s of R E (Earth radii) can segment the bow shock into more than one region of quasiperpendicular or quasiparallel shock geometry.…”

Section: Introductionmentioning

confidence: 99%

Use of the L1 Constellation as a Multispacecraft Solar Wind Monitor

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Nykyri

2020

JGR Space Physics

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A novel multispacecraft solar wind monitor is developed, which expands on the forecasting ability of OMNI by giving spatially resolved predictions. The prediction algorithm ingests all the data from the current fleet of three L1 monitors, allowing gradients in the solar wind to be resolved on scale sizes similar to the magnetosphere. Understanding structure of the solar wind is vital to determine the global magnetospheric configuration, which is important in both real time as a space‐weather product and data users wanting to know upstream conditions when interpreting observations. The model is validated by comparing the predictions with other spacecraft observing the solar wind in situ. We perform a statistical study with thousands of hours of magnetospheric multiscale observations in the solar wind, comparing the prediction accuracy of the multispacecraft monitor to all of the OMNIWeb single‐spacecraft monitors. The multispacecraft monitor shows improvement over all three of the single‐spacecraft predictions for 44% of the cases and also outperforms both ACE and Wind, which are the primary magnetic field contributors to the OMNI IMF prediction, 55% of the time. We propose that the realistic structure of the solar wind that is resolved with multiple solar wind monitors could be vitally important to implement as upstream conditions in global magnetospheric simulations.

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Analysis of the substructure within a complex magnetic cloud on 3–4 September 2008

Cited by 2 publications

References 24 publications

On the relationship between interplanetary coronal mass ejections and magnetic clouds

On the relationship between interplanetary coronal mass ejections and magnetic clouds

Use of the L1 Constellation as a Multispacecraft Solar Wind Monitor

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