An analysis of interplanetary sources of geomagnetic storm during November 7–8, 1998

Le, G. M.; Tang, Yuhua; Ling, Zheng; Liu, Lianguang

doi:10.1007/s11434-009-0228-x

Cited by 3 publications

(3 citation statements)

References 16 publications

(16 reference statements)

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“…Wanliss & Showalter (2006) recommended that the SYM-H index can be used as a high-resolution Dst index. The SYM-H index has been widely used in geomagnetic storm studies (e.g., Nosé et al 2003;Le et al 2010;Hutchinson et al 2011). SYM-H index is applied in this study to describe detailed variation of geomagnetic storm intensity.…”

Section: Introductionmentioning

confidence: 99%

Sun-Earth connection event of super geomagnetic storm on 2001 March 31: the importance of solar wind density

Cheng

Zhao

2020

Res. Astron. Astrophys.

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An X1.7 flare at 10:15 UT and a halo CME with a projected speed of 942 km s−1 erupted from NOAA solar active region 9393 located at N20W19, which were observed on 2001 March 29. When the CME reached the Earth, it triggered a super geomagnetic storm (hereafter super storm). We find that the CME always moved towards the Earth according to the intensity-time profiles of protons with different energies. The solar wind parameters responsible for the main phase of the super storm occurred on 2001 March 31 are analyzed while taking into account the delayed geomagnetic effect of solar wind at the L1 point and using the SYM-H index. According to the variation properties of SYM-H index during the main phase of the super storm, the main phase of the super storm is divided into two parts. A comparative study of solar wind parameters responsible for two parts shows the evidence that the solar wind density plays a significant role in transferring solar wind energy into the magnetosphere, besides the southward magnetic field and solar wind speed.

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Section: Introductionmentioning

confidence: 99%

Sun-Earth connection event of super geomagnetic storm on 2001 March 31: the importance of solar wind density

Cheng

Zhao

2020

Res. Astron. Astrophys.

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“…For geomagnetic storms, many studies have focused on the relationship between the intensity of geomagnetic storms and interplanetary sources and/or on causes of the one‐step/two‐step morphology of the main phases of geomagnetic storms (Akasofu and Chapman, ; Russell et al, ; Srivastava and Venkatakrishnan, ; Le GM et al, ; Zhao H et al, ). It is now well established that intense geomagnetic storms ( Dst min ≤ 100 nT) are caused mainly by coronal mass ejections (Brueckner et al, ; Gonzalez et al, ; Cane et al, ; Gopalswamy et al, ; Zhang J et al, ), while moderate and weak storms can be caused by high‐speed streams in corotating interaction regions (Gosling et al, ; Tsurutani and Gonzalez, ).…”

Section: Introductionmentioning

confidence: 99%

Statistical study on interplanetary drivers behind intense geomagnetic storms and substorms

Tian

Chang

Sun

et al. 2019

Earth and Planetary Physics

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Geomagnetic storms and substorms play a central role in both the daily life of mankind and in academic space physics. The profiles of storms, especially their initial phase morphology and the intensity of their substorms under different interplanetary conditions, have usually been ignored in previous studies. In this study, 97 intense geomagnetic storms (Dstmin ≤ –100 nT) between 1998 and 2018 were studied statistically using the double superposed epoch analysis (DSEA) and normalized superposed epoch analysis (NSEA) methods. These storms are categorized into two types according to different interplanetary magnetic field (IMF) Bz orientations: geomagnetic storms whose IMF is northward, both upstream and downstream relative to the interplanetary shock, and geomagnetic storms whose upstream and downstream IMF is consistently southward. We further divide these two types into two subsets, by different geomagnetic storm profiles: Type I/Type II — one/two‐step geomagnetic storms with northward IMF both upstream and downstream of the interplanetary shock; Type III/TypeIV — one/two‐step geomagnetic storms with southward IMF both upstream and downstream of the interplanetary shock. The results show that: (1) geomagnetic storms with northward IMF both upstream and downstream of the interplanetary shock have a clear initial phase; geomagnetic storms with southward IMF in both upstream and downstream of the interplanetary shock do not; (2) the IMF is an important controlling factor in affecting the intensity characteristics of substorms. When Bz is positive before and after the interplanetary shock arrival, the Auroral Electrojet (AE) index changes gently during the initial phase of geomagnetic storms, the median value of AE index is maintained at 500–1000 nT; (3) whenBz is negative before and after the interplanetary shock arrival, the AE index rises rapidly and reaches its maxmum value about one hour after storm sudden commencements (SSC), although the time is scaled between reference points and the maximum value of AE is usually greater than 1,000 nT, representing intense substorms; (4) for most cases, the Dst0 usually reaches its minimum at least one hour after Bz. These results are useful in improving contemporary space weather models, especially for those that address geomagnetic storms and substorms.

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“…Dst index. As a matter of fact, the SYM-H index has been widely used in geomagnetic storm studies (e.g., Nosé et al 2003;Le et al 2010;Hutchinson et al 2011). SYM-H index is applied in this study to describe detailed variation of geomagnetic storm intensity.…”

Section: Introductionmentioning

confidence: 99%

Sun-Earth connection Event of Super Geomagnetic Storm on March 31, 2001: the Importance of Solar Wind Density

Cheng,

Le,

Zhao

2019

Preprint

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An X1.7 flare at 10:15 UT and a halo CME with a projected speed of 942 km/s erupted from NOAA solar active region 9393 located at N20W19, were observed on 2001 March 29. When the CME reached the Earth, it triggered a super geomagnetic storm (hereafter super storm). We find that the CME always moved towards the Earth according to the intensity-time profiles of protons with different energies. The solar wind parameters responsible for the main phase of the super storm occurred on March 31, 2001 is analyzed taking into account the delayed geomagnetic effect of solar wind at the L1 point and using the SYM-H index. According to the variation properties of SYM-H index during the main phase of the super storm, the main phase of the super storm is divided into two parts. A comparative study of solar wind parameters responsible for the two parts shows the evidence that the solar wind density plays a significant role in transferring solar wind energy into the magnetosphere, besides the southward magnetic field and solar wind speed.

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An analysis of interplanetary sources of geomagnetic storm during November 7–8, 1998

Cited by 3 publications

References 16 publications

Sun-Earth connection event of super geomagnetic storm on 2001 March 31: the importance of solar wind density

Sun-Earth connection event of super geomagnetic storm on 2001 March 31: the importance of solar wind density

Statistical study on interplanetary drivers behind intense geomagnetic storms and substorms

Sun-Earth connection Event of Super Geomagnetic Storm on March 31, 2001: the Importance of Solar Wind Density

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