Major geomagnetic storms (<i>Dst</i> ≤ −100 nT) generated by corotating interaction regions

Richardson, I. G.; Webb, D. F.; Zhang, J.; Berdichevsky, D. B.; Biesecker, D. A.; Kasper, J. C.; Kataoka, Ryuho; Steinberg, J. T.; Thompson, B. J.; Wu, Chin‐Chun; Zhukov, A. N.

doi:10.1029/2005ja011476

Cited by 176 publications

(152 citation statements)

References 50 publications

Supporting

Mentioning

140

Contrasting

Order By: Relevance

“…Consequently, CMEs and CIRs/HSSs drive geomagnetic activity differently. Most intense (Dst < −100 nT) geomagnetic storms are produced by CMEs, while CIR-driven storms are typically limited to smaller intensities [Zhang et al, 2007;Richardson et al, 2006], and about 50% of moderate geomagnetic storms (−100 nT < Dst < −50 nT) are driven by CIRs/HSSs [Echer et al, 2013]. Due to their longer duration and the embedded…”

Section: Introductionmentioning

confidence: 99%

Annual fractions of high‐speed streams from principal component analysis of local geomagnetic activity

et al. 2014

View full text Add to dashboard Cite

We study the latitudinal distribution of geomagnetic activity in 1966–2009 with local geomagnetic activity indices at 26 magnetic observatories. Using the principal component analysis method we find that more than 97% of the variance in annually averaged geomagnetic activity can be described by the two first principal components. The first component describes the evolution of the global geomagnetic activity, and has excellent correlation with, e.g., the Kp/Ap index. The second component describes the leading pattern by which the latitudinal distribution of geomagnetic activity deviates from the global average. We show that the second component is highly correlated with the relative (annual) fraction of high‐speed streams (HSS) in solar wind. The latitudinal distribution of the second mode has a high maximum at auroral latitudes, a local minimum at subauroral latitudes and a low maximum at midlatitudes. We show that this distribution is related to the difference in the average location and intensity between substorms related to coronal mass ejections (CMEs) and HSSs. This paper demonstrates a new way to extract useful, quantitative information about the solar wind from local indices of geomagnetic activity over a latitudinally extensive network.

show abstract

Section: Introductionmentioning

confidence: 99%

Annual fractions of high‐speed streams from principal component analysis of local geomagnetic activity

et al. 2014

View full text Add to dashboard Cite

show abstract

“…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: 88%

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

2009

View full text Add to dashboard Cite

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.

show abstract

“…These storm levels indicate that intense events have lower probability of occurrence than weaker storms, as already noticed in previous studies (Tsurutani et al 2006;Alves et al 2006, see also Paper I and II). Richardson et al (2006) also show the lower occurrence of weaker events for a 159 CIR sample (see their Fig. 9).…”

Section: Overall Characteristics Of the Employed Samplesmentioning

confidence: 99%

“…9). We note that, CIRs alone occasionally may produce intense storms (Richardson et al 2006;Zhang et al 2003).…”

Section: Overall Characteristics Of the Employed Samplesmentioning

confidence: 99%

“…The geoeffectiveness of ICMEs and HSS/CIRs has been studied by many researchers (e.g., Schwenn et al 2005;Huttunen et al 2005;Georgieva et al 2006;Lavraud et al 2006;Alves et al 2006;Richardson et al 2006;Yermolaev & Yermolaev 2006;Vršnak et al 2007;Zhang et al 2007b;Echer et al 2008;Verbanac et al 2011a;Richardson & Cane 2010Verbanac et al 2011b, and references therein). In most of these studies, the level of the geomagnetic activity is commonly quantified with the storm-time disturbance index Dst, which is a relatively good measure of the ring current strength Wang et al 2003;Kane 2005;Alves et al 2006;Bakare & Chukwuma 2010).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Comparison of geoeffectiveness of coronal mass ejections and corotating interaction regions

Verbanac

Živković

Vršnak

et al. 2013

A&A

View full text Add to dashboard Cite

Context. A detailed comparison of the geomagnetic responses to interplanetary coronal mass ejection (ICMEs) and corotating interaction regions (CIRs) during solar cycle 23 was performed using geomagnetic indices Dst, Ap, and AE. Aims. We aim to find out if there are relative differences in the response of various magnetospheric current systems to the impact of ICMEs and CIRs. In addition, we are exploring the possibility of forecasting geomagnetic activity using the coronagraphic observations of the ICME take-off. Methods. The peak values of the plasma characteristics of ICMEs and CIRs (velocity V, magnetic field B, and BV related to the electric field), and geomagnetic indices were investigated by applying the linear and power-law cross correlation analysis. The influence of the time-resolution on the results was performed for two time resolutions obtained by one-hour (three-hour for Ap) and six-hour data averaging. Results. For ICMEs the power-law fits are found to be important only for the relationships between BV and geomagnetic indices. For Ap and Dst, there is no difference between the one-hour (three-hour for Ap) and six-hour option. For AE, the one-hour data distribution shows more clearly the non-linear dependence on BV. Our data set shows that below BV ∼ 5 mV m −1 ICMEs have practically no geomagnetic effect at low and mid latitudes, but at high latitudes at least some geomagnetic activity will be triggered. For all HSS/CIRs dependencies, a power law is found to better describe the data than the linear fit. The data distributions show that BV has to reach ∼4 mV m −1 in order to drive at least some geomagnetic activity at all latitudes. We observed that there are fast CMEs that have almost no geomagnetic effect at low and mid latitudes. On the other hand, at high latitudes, fast CMEs always trigger some geomagnetic activity. This might be have implications for space weather forecasting. Conclusions. Magnetospheric response to both solar drivers (ICMEs and CIRs) is different at various latitudes, thus results in different development of various current systems within the Earth's magnetosphere and ionosphere. Furthermore, we show that ICMEs and CIRs cause different geomagnetic activity. In the case of ICMEs equatorial current system responses in a linear manner, while the response of the polar-current system is likely to be non-linear. For HSS/CIRs, apparently all current systems respond in a non-linear way, especially the polar current system.

show abstract

Major geomagnetic storms (Dst ≤ −100 nT) generated by corotating interaction regions

Cited by 176 publications

References 50 publications

Annual fractions of high‐speed streams from principal component analysis of local geomagnetic activity

Annual fractions of high‐speed streams from principal component analysis of local geomagnetic activity

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

Comparison of geoeffectiveness of coronal mass ejections and corotating interaction regions

Contact Info

Product

Resources

About