Geomagnetic storms driven by ICME‐ and CIR‐dominated solar wind

Denton, M. H.; Borovsky, Joseph E.; Skoug, R. M.; Thomsen, M. F.; Lavraud, B.; Henderson, M. G.; McPherron, R. L.; Zhang, J. C.; Liemohn, Michael W.

doi:10.1029/2005ja011436

Cited by 212 publications

(270 citation statements)

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“…Extensive statistical studies of the plasma within the near-Earth magnetosphere have previously revealed the behaviour of such parameters (e.g. Baumjohann et al, 1988;Newell and Meng, 1992;Borovsky et al, 1998;Wing and Newell, 1998;Měrka et al, 2002;Tysganenko and Mukai, 2003;Wing et al, 2005;Neagu et al, 2005;Denton et al, 2005Denton et al, , 2006Borovsky and Denton, 2006a, b;Lavraud et al, 2005Lavraud et al, , 2006Thomsen et al, 2007;Nagata et al, 2007;Åsnes et al, 2008) under a variety of conditions. The primary aim of the work outlined in the current paper is to reveal the averaged bulk parameters in the magnetosphere as a first step to a determination of how such parameters evolve during geomagnetic disturbances.…”

Section: Introductionmentioning

confidence: 99%

“…Such analyses are particularly aimed at modellers of the Earth's ring current and radiation belts who utilise values of ion temperature, density, and composition from the nightside region as boundary conditions for simulations (e.g. Liemohn et al, 2006;Fok et al, 1999;Jordanova et al, 1997). In particular, this current study is the first step in adding the database of Cluster measurements Published by Copernicus Publications on behalf of the European Geosciences Union.…”

Section: Introductionmentioning

confidence: 99%

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Solar wind dependence of ion parameters in the Earth's magnetospheric region calculated from CLUSTER observations

Denton

Taylor

2008

Ann. Geophys.

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Abstract. Moments calculated from the ion distributions (∼0-40 keV) measured by the Cluster Ion Spectrometry (CIS) instrument are combined with data from the Cluster Flux Gate Magnetometer (FGM) instrument and used to characterise the bulk properties of the plasma in the nearEarth magnetosphere over five years (2001)(2002)(2003)(2004)(2005). Results are presented in the form of 2-D xy, xz and yz GSM cuts through the magnetosphere using data obtained from the Cluster Science Data System (CSDS) and the Cluster Active Archive (CAA). Analysis reveals the distribution of ∼0-40 keV ions in the inner magnetosphere is highly ordered and highly responsive to changes in solar wind velocity. Specifically, elevations in temperature are found to occur across the entire nightside plasma sheet region during times of fast solar wind. We demonstrate that the nightside plasma sheet ion temperature at a downtail distance of ∼12 to 19 Earth radii increases by a factor of ∼2 during periods of fast solar wind (500-1000 km s −1 ) compared to periods of slow solar wind (100-400 km s −1 ). The spatial extent of these increases are shown in the xy, xz and yz GSM planes. The results from the study have implications for modelling studies and simulations of solar-wind/magnetosphere coupling, which ultimately rely on in situ observations of the plasma sheet properties for input/boundary conditions.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Solar wind dependence of ion parameters in the Earth's magnetospheric region calculated from CLUSTER observations

Denton

Taylor

2008

Ann. Geophys.

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“…Because IMF lies in the ecliptic plane under steady interplanetary conditions and substantial B z < 0 is observed only in disturbed types of solar wind (SW), it was found in many investigations that interplanetary coronal mass ejections (ICME) and corotating interaction regions (CIR) are the most important drivers of magnetic disturbances on the Earth. Therefore, it is natural to categorize these solar wind drivers during a study of magnetic storm generation (see reviews and recent papers, for instance, Tsurutani et al, 1988;Tsurutani and Gonzalez, 1997;Gonzalez et al, 1999;Yermolaev and Yermolaev, 2002;Huttunen and Koskinen, 2004;Echer and Gonzalez , 2004;Denton et al, 2006;Huttunen et al, 2006;Yermolaev et al, 2007a,b,c;Pulkkinen et al, 2007a,b;Zhang et al, 2007;Turner et al, 2009;Yermolaev et al, 2010b, and references therein). As shown by numerous researchers, the different interplanetary drivers result in specific reactions of magnetosphere, for example, CIR-and ICME-induced magnetic storms (Huttunen et al, 2002;Pulkkinen et al, 2007a) or the specific development of substorms (Despirak et al, 2009).…”

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confidence: 99%

Specific interplanetary conditions for CIR-, Sheath-, and ICME-induced geomagnetic storms obtained by double superposed epoch analysis

et al. 2010

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Abstract.A comparison of specific interplanetary conditions for 798 magnetic storms with Dst < −50 nT during 1976-2000 was made on the basis of the OMNI archive data. We categorized various large-scale types of solar wind as interplanetary drivers of storms: corotating interaction region (CIR), Sheath, interplanetary CME (ICME) including both magnetic cloud (MC) and Ejecta, separately MC and Ejecta, and "Indeterminate" type. The data processing was carried out by the method of double superposed epoch analysis which uses two reference times (onset of storm and minimum of Dst index) and makes a re-scaling of the main phase of the storm in a such way that all storms have equal durations of the main phase in the new time reference frame. This method reproduced some well-known results and allowed us to obtain some new results. Specifically, obtained results demonstrate that (1) in accordance with "output/input" criteria the highest efficiency in generation of magnetic storms is observed for Sheath and the lowest one for MC, and (2) there are significant differences in the properties of MC and Ejecta and in their efficiencies.

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“…Moreover, co-rotating interaction regions (CIRs) are regions of intense magnetic field formed when high-speed solar wind streams overtake slow solar wind streams as they propagate away from the Sun. Geomagnetic storms produced by co-rotating interaction regions are generally weaker than those produced by coronal mass ejections (Tsurutani et al, 2006;Alves et al, 2006;Denton et al, 2006;Borovsky and Denton, 2006;Richardson et al, 2006), although there are some notable exceptions (Richardson et al, 2006). However, a detailed discussion of the different types of solar activity that result in recurrent and non-recurrent geomagnetic storms is well beyond the intended scope of the present paper.…”

Section: Day -6mentioning

confidence: 90%

The presence of large sunspots near the central solar meridian at the times of major geomagnetic storms

2009

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Abstract.A further study is made of the validity of a technique developed by the authors to identify historical occurrences of intense geomagnetic storms, which is based on finding approximately coincident observations of sunspots and aurorae recorded in East Asian histories. Previously, the validity of this technique was corroborated using scientific observations of aurorae in Japan during the interval 1957-2004 and contemporaneous white-light images of the Sun obtained by the Royal Greenwich Observatory, the Big Bear Solar Observatory, the Debrecen Heliophysical Observatory, and the Solar and Heliospheric Observatory spacecraft. The present investigation utilises a list of major geomagnetic storms in the interval 1868-2008, which is based on the magnitude of the AA* magnetic index, and reconstructed solar images based on the sunspot observations acquired by the Royal Greenwich Observatory during the shorter interval 1874-1976. It is found that a sunspot large enough to be seen with the unaided eye by an "experienced" observer was located reasonably close to the central solar meridian for almost 90% of these major geomagnetic storms. Even an "average" observer would easily achieve a corresponding success rate of 70% and this success rate increases to about 80% if a minority of ambiguous situations are interpreted favourably. The use of information on major geomagnetic storms, rather than modern auroral observations from Japan, provides a less direct corroboration of the technique for identifying historical occurrences of intense geomagnetic storms, if only because major geomagnetic storms do not necessarily produce auroral displays over East Asia. Nevertheless, the present study provides further corroboration of the validity of the original technique for identifying intense geomagnetic Correspondence to: D. M. Willis (d.m.willis@rl.ac.uk) storms. This additional corroboration of the original technique is important because early unaided-eye observations of sunspots and aurorae provide the only possible means of identifying individual geomagnetic storms during the greater part of the past two millennia.

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Geomagnetic storms driven by ICME‐ and CIR‐dominated solar wind

Cited by 212 publications

References 49 publications

Solar wind dependence of ion parameters in the Earth's magnetospheric region calculated from CLUSTER observations

Solar wind dependence of ion parameters in the Earth's magnetospheric region calculated from CLUSTER observations

Specific interplanetary conditions for CIR-, Sheath-, and ICME-induced geomagnetic storms obtained by double superposed epoch analysis

The presence of large sunspots near the central solar meridian at the times of major geomagnetic storms

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