Solar and interplanetary sources of major geomagnetic storms during 1996–2002

Srivastava, Nandita; Venkatakrishnan, P.

doi:10.1029/2003ja010175

Cited by 140 publications

(96 citation statements)

References 62 publications

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“…We now know that CMEs are the major causes of geomagnetic activity at the Earth (Feynman and Gabriel, 2000;Plunkett et al, 2001;Wang et al, 2002;Zhang et al, 2003;Vilmer et al, 2003;Srivastava and Venkatakrishnan, 2004). Intense geomagnetic activity can also occur due to fast streams originating from coronal holes (Klein and Burlaga, 1982;Sheeley et al, 1976).…”

Section: Introductionmentioning

confidence: 99%

“…However, the solar properties that influence the interplanetary properties have not been widely investigated in detail. Srivastava and Venkatakrishnan (2004) recently attempted to identify solar variables that control interplanetary variables responsible for producing major geomagnetic storms. Their results show that fast full-halo CMEs associated with strong flares and originating close to the central meridian and low and middle latitudes are potentially favourable candidates for producing strong ram pressure at the Earth's magnetosphere.…”

Section: Introductionmentioning

confidence: 99%

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Predicting the occurrence of super-storms

Srivastava

2005

Ann. Geophys.

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Abstract.A comparative study of five super-storms (D st <−300 nT) of the current solar cycle after the launch of SoHO, to identify solar and interplanetary variables that influence the magnitude of resulting geomagnetic storms, is described. Amongst solar variables, the initial speed of a CME is considered the most reliable predictor of the strength of the associated geomagnetic storm because fast mass ejections are responsible for building up the ram pressure at the Earth's magnetosphere. However, although most of the super-storms studied were associated with high speed CMEs, the D st index of the resulting geomagnetic storms varied between −300 to −472 nT. The most intense storm of 20 November 2003, (D st ∼−472 nT) had its source in a comparatively smaller active region and was associated with a relatively weaker, M-class flare while all other super-storms had their origins in large active regions and were associated with strong X-class flares. However, this superstorm did not show any associated extraordinary solar and interplanetary characteristics. The study also reveals the challenge in the reliable prediction of the magnitude of a geomagnetic storm from solar and interplanetary variables.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Predicting the occurrence of super-storms

Srivastava

2005

Ann. Geophys.

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“…Solar energetic particles (SEPs) can reach the Earth when the magnetic connectivity of the flaring active region is matching, with a tolerance of 25Њ-30Њ in heliographic longitude (Ippolito et al 2005), although sometimes apparently not-connected events rooted in the eastern solar disk happen (Miroshnichenko et al 2005b). During a 7-year period of the current solar cycle, 64 geoeffective CMEs were found to produce major geomagnetic storms at Earth (Srivastava & Venkatakrishnan 2004). The SEP event of 14 July 2000 (the "Bastille-day flare") was investigated by using simultaneous ground-based and satellite measurements of the particle flux, together with a tissue equivalent proportional counter on board a Virgin Atlantic Airways flight from London Heathrow to Hong Kong, but fortunately no increased radiation levels were detected (Iles et al 2004).…”

Section: Space Weathermentioning

confidence: 99%

Astrophysics in 2005

Trimble

Aschwanden

Hansen

2006

PUBL ASTRON SOC PAC

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ABSTRACT. We bring you, as usual, the Sun and Moon and stars, plus some galaxies and a new section on astrobiology. Some highlights are short (the newly identified class of gamma-ray bursts, and the Deep Impact on Comet 9P/Tempel 1), some long (the age of the universe, which will be found to have the Earth at its center), and a few metonymic, for instance the term "down-sizing" to describe the evolution of star formation rates with redshift.

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“…1a of the paper by Willis et al (2006) also shows dotted lines (meridians) at ±50 • of heliographic longitude with respect to the central meridian. Based on the statistical evidence for an association between the heliographic location of an active solar region and the subsequent onset of a geomagnetic storm (Hudson et al, 1998;Webb et al, 2000;Cane et al, 2000;Berdichevsky et al, 2002;Cane and Richardson, 2003;Srivastava and Venkatakrishnan, 2004;Kim et al, 2005;Gopalswamy et al, 2005Gopalswamy et al, , 2007Schwenn et al, 2005;Kang et al, 2006;Zhang et al, 2007a, b;Tsurutani et al, 2008), sunspot groups that are closer to the central meridian than the dotted lines, and also large enough to be seen with the unaided eye, are likely to be associated with major geomagnetic storms. Conversely, sunspot groups that are further from the central meridian than the dotted lines are unlikely be associated with major geomagnetic storms, irrespective of their size.…”

Section: Criteria For Sunspot Visibility With the Unaided Eyementioning

confidence: 99%

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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Solar and interplanetary sources of major geomagnetic storms during 1996–2002

Cited by 140 publications

References 62 publications

Predicting the occurrence of super-storms

Predicting the occurrence of super-storms

Astrophysics in 2005

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

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