Correction to “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:10.1029/2007ja012332

Cited by 21 publications

(21 citation statements)

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“…There is a great interest in understanding the propagation characteristics of CMEs and predicting the CME-related space weather. In this connection several studies have been made to investigate (a) the relationship between the speed of the CME at the near-Sun region and effects created by its shock ejecta and/or magnetic cloud at the Earth's magnetosphere (e.g., Richardson et al, 2007), and (b) the arrival times of the CME and its associated shock at 1 AU (e.g., Gopalswamy et al, 2001;2005;Manoharan et al, 2004). In such recent studies, white-light images mainly obtained from LASCO/SOHO space mission and 1-AU in-situ measurements have been employed.…”

Section: Introductionmentioning

confidence: 99%

Coronal mass ejections—Propagation time and associated internal energy

Manoharan¹,

Rahman²

2011

Journal of Atmospheric and Solar-Terrestrial Physics

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In this paper, we analyze 91 coronal mass ejection (CME) events studied by Manoharan et al. (2004) and Gopalswamy and Xie (2008). These earthdirected CMEs are large (width > 160• ) and cover a wide range of speeds (∼120-2400 kms −1 ) in the LASCO field of view. This set of events also includes interacting CMEs and some of them take longer time to reach 1 AU than the travel time inferred from their speeds at 1 AU. We study the link between the travel time of the CME to 1 AU (combined with its final speed at the Earth) and the effective acceleration in the Sun-Earth distance. Results indicate that (1) for almost all the events (85 out of 91 events), the speed of the CME at 1 AU is always less than or equal to its initial speed measured at the near-Sun region, (2) the distributions of initial speeds, CME-driven shock and CME speeds at 1 AU clearly show the effects of aerodynamical drag between the CME and the solar wind and in consequence, the speed of the CME tends to equalize to that of the background solar wind, (3) for a large fraction of CMEs (for ∼50% of the events), the inferred effective acceleration along the Sun-Earth line dominates the above drag force. The net acceleration suggests an average dissipation of energy ∼10 31−32ergs, which is likely provided by the Lorentz force associated with the internal magnetic energy carried by the CME.

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Section: Introductionmentioning

confidence: 99%

Coronal mass ejections—Propagation time and associated internal energy

Manoharan¹,

Rahman²

2011

Journal of Atmospheric and Solar-Terrestrial Physics

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“…Otherwise, the storms are predominantly driven by CME-related flows, including 96% of C3-C5 storms. A complexity not included in these results is that occasionally (e.g., two of the 88 intense storms examined by [8]), both CME-related flows and streams may be involved in the production of a storm [3,18,19]. As noted above, we assign the flow associated with the more intense activity as the storm driver.…”

Section: Solar Wind Drivers Of Geomagnetic Storms In 1964-2011mentioning

confidence: 90%

“…Here, we use this classification to determine the drivers of geomagnetic storms of various sizes since 1964, updating the results of [6]. For discussion of the interplanetary causes of geomagnetic storms, see e.g., [7,8,9]. For a more extended version of the current study, see [10].…”

Section: Introductionmentioning

confidence: 97%

Solar wind drivers of geomagnetic storms over more than four solar cycles

Richardson¹,

Cane²

2013

AIP Conference Proceedings

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“…The Kasper database provides parameters for shocks during 1995 to 2004 but is not complete. In particular, only shocks in 2003 and 2004 associated with intense geomagnetic storms [Zhang et al, 2007] are included. To complement this database, we used the ACE shock list (http://www.ssg.sr.unh.edu/mag/ace/ACElists/obslist.html) compiled by C. W. Smith (University of New Hampshire).…”

Section: Introductionmentioning

confidence: 99%

Interplanetary circumstances of quasi‐perpendicular interplanetary shocks in 1996–2005

Richardson

Cane

2010

J. Geophys. Res.

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[1] The angle ( Bn ) between the normal to an interplanetary shock front and the upstream magnetic field direction, though often thought of as a property "of the shock," is also determined by the configuration of the magnetic field immediately upstream of the shock. We investigate the interplanetary circumstances of 105 near-Earth quasi-perpendicular shocks during 1996-2005 identified by Bn ≥ 80°and/or by evidence of shock drift particle acceleration. Around 87% of these shocks were driven by interplanetary coronal mass ejections (ICMEs); the remainder were probably the forward shocks of corotating interaction regions. For around half of the shocks, the upstream field was approximately perpendicular to the radial direction, either east-west or west-east or highly inclined to the ecliptic. Such field directions will give quasi-perpendicular configurations for radially propagating shocks. Around 30% of the shocks were propagating through, or closely followed, ICMEs at the time of observation. Another quarter were propagating through the heliospheric plasma sheet (HPS), and a further quarter occurred in slow solar wind that did not have characteristics of the HPS. Around 11% were observed in high-speed streams, and 7% in the sheaths following other shocks. The fraction of shocks found in high-speed streams is around a third of that expected based on the fraction of the time when such streams were observed at Earth. Quasi-perpendicular shocks are found traveling through ICMEs around 2-3 times more frequently than expected. In addition, shocks propagating through ICMEs are more likely to have larger values of Bn than shocks outside ICMEs.

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Correction to “Major geomagnetic storms (Dst ≤ −100 nT) generated by corotating interaction regions”

Cited by 21 publications

References 0 publications

Coronal mass ejections—Propagation time and associated internal energy

Coronal mass ejections—Propagation time and associated internal energy

Solar wind drivers of geomagnetic storms over more than four solar cycles

Interplanetary circumstances of quasi‐perpendicular interplanetary shocks in 1996–2005

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