Torsional Alfvén Wave Embedded ICME Magnetic Cloud and Corresponding Geomagnetic Storm

Raghav, Anil; Kule, Ankita; Bhaskar, Ankush; Mishra, Wageesh; Vichare, Geeta; Surve, Shobha

doi:10.3847/1538-4357/aabba3

Cited by 25 publications

(14 citation statements)

References 60 publications

(61 reference statements)

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“…In addition to this, Raghav et al. (2019) suggested that Alfvénic fluctuations are associated with the extended/long duration recovery of a storm (Raghav et al., 2018; Shaikh et al., 2019).…”

Section: Introductionmentioning

confidence: 99%

“…Moreover, Jordanova et al (2003) proposed that the ring current decay during the initial fast recovery is highly affected by the time-varying night-side inflow of plasma from the magneto-tail, and particle precipitation by wave-particle interactions (Dessler & Parker, 1959). In addition to this, Raghav et al (2019) suggested that Alfvénic fluctuations are associated with the extended/long duration recovery of a storm (Raghav et al, 2018;Shaikh et al, 2019).…”

Section: Introductionmentioning

confidence: 99%

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Properties of the Recovery Phase of Extreme Storms

et al. 2021

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A geomagnetic storm is a phenomenon of weakening of Earth's magnetic field from a few hours to several days, which directly or indirectly affects navigation, transportation, communication, power grids, satellite electronics, etc. In general, the duration of the recovery phase is larger. Thus, its cumulative effect is greater than the main phase. Therefore, it is important to understand the physical processes involved during the recovery phase. In this paper, we have studied the recovery phase of 31 extreme geomagnetic storms that occurred from 1990 to 2020. Each storm demonstrates two distinct features of the recovery phase that is, initial fast and later slow recovery phase. During the fast recovery phase, the rate of recovery either linearly or non‐linearly depends on SYM−H, which has been characterized by an exponential or hyperbolic decay function in various reported studies. In our study, we have noted that the hyperbolic function explains the complete recovery phase of only 11 extreme events. Furthermore, both decay functions fail to explain the late recovery phase of storms. Interestingly, we have found that the rate of recovery during the slow phase shows steady variation (independent to SYM−H), that is, d(SYMbadbreak−H)dt0.3333em=0.3333emconstant. Our analysis suggests that the magnitude of the recovery rate during the late phase is proportional to the magnitude of the storm.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Properties of the Recovery Phase of Extreme Storms

et al. 2021

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“…High-intensity long-duration continuous AE activities (HILDCAAs) are the effects of Alfvén wave trains in the IMF (Tsurutani & Gonzalez 1987). Alfvénic fluctuations are associated with repetitive substorms (Lee et al 2006) and inferred to extend the recovery phase of geomagnetic storms (Tsurutani et al 2011;Raghav et al 2018;Telloni et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Geoeffectiveness of Interplanetary Alfvén Waves. I. Magnetopause Magnetic Reconnection and Directly Driven Substorms

Dai¹,

Han

Wang³

et al. 2023

ApJ

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In particular during the descending phase of the solar cycle, Alfvén waves in the high-speed solar wind streams are a major form of interplanetary disturbances. The fluctuating southward interplanetary magnetic field (IMF) of Alfvén waves has been suggested to induce geomagnetic activities through intermittent magnetic reconnection at the magnetopause. In this study, we provide in situ observational evidence for dayside magnetopause reconnection induced by such interplanetary Alfvén waves. Using multipoint conjunction observations, we show that the IMF B z from interplanetary Alfvén waves is transmitted through and amplified by the Earth’s bow shock. Associated with the intensified southward B z to the magnetopause, in situ signatures of magnetic reconnection are detected. Repetitively, interplanetary Alfvén waves transmit the intensified B z to the magnetosheath, leading to intervals of large magnetic shear angles across the magnetopause and magnetopause reconnection. Such intervals are promptly followed by hundreds of nanoTesla (nT) increases in the auroral electrojet indices (AE and AU) within 10–20 minutes. These observations are confirmed in multiple events in corotating interaction region-driven geomagnetic storms. To put the observations into context, we propose a phenomenological model of a strongly driven substorm. The substorm electrojet is linked to the enhanced magnetopause reconnection in the short timescale of re-establishing the ionosphere electric field and the two-cell convection. These results provide insights on the temporal patterns of solar wind magnetosphere–ionosphere coupling, especially during the descending phase of the solar cycle.

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“…ICMEs occasionally interact with the terrestrial magnetic field with sufficient mass, velocity, and southward interplanetary magnetic field (IMF) to cause geomagnetic storms and equatorward extensions of the auroral oval (Gonzalez et al, 1994;Yokoyama et al, 1998;Daglis et al, 1999;Pulkkinen, 2007). Analyses of such solar and geomagnetic storms are more than just of academic interest due to their potential to create space weather conditions that frequently enhance electric currents in space, which in turn can affect essential societal infrastructure such as power grid systems, satellite operations, and long-range communication systems (Pulkkinen, 2007;Baker et al, 2008;Schrijver, 2015;Pulkkinen et al, 2017;Riley et al, 2018;Raghav et al, 2018Raghav et al, , 2019Oliveira et al, 2020aOliveira et al, , 2021aHapgood et al, 2021).…”

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confidence: 99%

The extreme solar and geomagnetic storms on 1940 March 20–25

Hayakawa

Oliveira

Shea³

et al. 2021

Monthly Notices of the Royal Astronomical Society

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In late March 1940, at least five significant solar flares were reported. They likely launched interplanetary coronal mass ejections (ICMEs), and were associated with one of the largest storm sudden commencements (SSCs) since the year 1868, resulting in space weather hazards that today would have significant societal impacts. The initial solar activity is associated with a short geomagnetic storm and a notable SSC. Afterward, the third flare was reported in the eastern solar quadrant (N12 E37-38) at 11:30–12:30 UT on 23 March, with significant magnetic crochets (up to ≈ |80| nT at Eskdalemuir) during 11:07–11:40 UT. On their basis, we estimate the required energy flux of the source flare as X35±1 in soft X-ray class. The resultant ICMEs caused enormous SSCs (up to > 425 nT recorded at Tucson) and allowed us to estimate an extremely inward magnetopause position (estimated magnetopause standoff position ≈ 3.4 RE). The time series of the resultant geomagnetic storm is reconstructed using a Dst estimate, which peaked at 20 UT on 24 March at ≈ −389 nT. Around the storm main phase, the equatorial boundary of the auroral oval extended ≤ 46.3° at invariant latitudes. This sequence also caused a solar proton event and Forbush decrease (≈ 3%). These sequences indicate pileups of multiple ICMEs, which even achieved a record value of inward magnetopause position. Our analyses of this historical pioneer event bring more insights into possible serious space weather hazards and provide a quantitative basis for future analyses and predictions.

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Torsional Alfvén Wave Embedded ICME Magnetic Cloud and Corresponding Geomagnetic Storm

Cited by 25 publications

References 60 publications

Properties of the Recovery Phase of Extreme Storms

Properties of the Recovery Phase of Extreme Storms

Geoeffectiveness of Interplanetary Alfvén Waves. I. Magnetopause Magnetic Reconnection and Directly Driven Substorms

The extreme solar and geomagnetic storms on 1940 March 20–25

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