Influence of the interplanetary driver type on the durations of the main and recovery phases of magnetic storms

Yermolaev, Yu. I.; Лодкина, И. Г.; Nikolaeva, N. S.; Yermolaev, M. Yu.

doi:10.1002/2014ja019826

Cited by 30 publications

(10 citation statements)

References 59 publications

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“…This is consistent with Yermolaev et al. (2014) who showed that although there are large spreads in the recovery phase distributions, sheath‐driven storms have longer recovery phase durations than MC storms. The time between the arrival of the ICME and t 0 was 15–16 hr for low p dyn /MC storms and 4 hr for high p dyn /sheath storms.…”

Section: Resultssupporting

confidence: 91%

Effect of ICME‐Driven Storms on Field‐Aligned and Ionospheric Currents From AMPERE and SuperMAG

et al. 2022

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This study investigates the field‐aligned currents (FACs) and ionospheric equivalent currents for interplanetary coronal mass ejection (ICME)‐driven storms by considering 45 events with a minimum Dst ≤ −50 nT. The FACs and ionospheric equivalent currents are studied by applying a superposed epoch analysis to data from AMPERE and SuperMAG with the zero epoch (t0) centered at the onset of the storm main phase. The currents and number of substorm onsets begin to increase 3 hr before t0 and maximizes about 1 hr after t0. The currents and number of substorm onsets remain high throughout the entire storm main phase, until at t0 + 14 hr they start to slowly relax back to quiet time conditions. The storms were separated into two groups based on the solar wind dynamic pressure pdyn around t0. High pdyn storms are mostly driven by the sheath region ahead of the ejecta. These storms have short main phase durations and larger currents early in the main phase which maximize at t0 + 50 min. The low pdyn group contains storms that start during the magnetic clouds (MC) and have gradually increasing currents that maximize at t0 + 11 hr, close to the end of the storm main phase. For the first 4 hr of the storm main phase, the currents in sheath‐driven storms are larger than for MC‐driven storms. The Russell‐McPherron effect is less important for ICME‐driven storms where only 44% have a contribution, compared to 82% of high speed stream/stream interaction driven storms.

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Section: Resultssupporting

confidence: 91%

Effect of ICME‐Driven Storms on Field‐Aligned and Ionospheric Currents From AMPERE and SuperMAG

et al. 2022

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“…The number of storms, especially CIR‐driven storms, are small compared to previous studies (e.g., Yermolaev et al., 2022) because only the clear storms satisfying four selection criteria are identified. The ICME driven storms could be generated by both magnetic clouds and area of compression in front of them, the sheath (Yermolaev et al., 2014). The corresponding storms in the SymH, Kp and AE indices are identified.…”

Section: Discussionmentioning

confidence: 99%

Double Superposed Epoch Analysis of Geomagnetic Storms and Corresponding Solar Wind and IMF in Solar Cycles 23 and 24

et al. 2023

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The large (fluctuating) electric currents flowing at different regions in the magnetosphere and ionosphere during space weather events produce large fluctuations in the geomagnetic field lasting from several hours to several days in all latitudes (e.g., Akasofu, 1981;Gonzalez et al., 1994;Svalgaard, 1977). The field fluctuations at low latitudes are produced mainly by the enhanced low latitude magnetospheric ring current; they undergo 3-phase variations and are referred as geomagnetic storms. At high latitudes, the field fluctuations are produced mainly by the enhanced high latitude ionospheric auroral electrojet current; they undergo irregular variations and are referred as storm-time substorms or activities. At mid latitudes, the field fluctuations are the combined effect of the poleward extension of the low latitude fluctuations and equatorward extension of the high latitude fluctuations; they undergo 2-phase variations and are referred also as geomagnetic storms (e.g.

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“…The schematic in Figure 6 showed a long "recovery phase" that trails the CIR magnetic storm main phase (see Tsurutani andGonzalez, 1987 andYermolaev et al 2014 for a contrast in interpretation). However we now know that the storm wasn't "recovering" as in the case of an MC magnetic storm but that something else was occurring.…”

Section: High Speed Solar Wind Streams Alfvén Waves and Hildcaasmentioning

confidence: 99%

Space Weather Forecasting: What We Know Now and What Are the Current and Future Challenges?

Tsurutani

Lakhina²,

Hajra

2019

Preprint

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Abstract. Geomagnetic storms are caused by solar wind southward magnetic fields that impinge upon the Earth’s magnetosphere (Dungey, 1961). How can we forecast the occurrence of these interplanetary events? We view this as the most important challenge in Space Weather. We discuss the case for magnetic clouds (MCs), interplanetary sheaths upstream of ICMEs, corotating interaction regions (CIRs) and high speed streams (HSSs). The sheath- and CIR-related magnetic storms will be difficult to predict and will require better knowledge of the slow solar wind and modeling to solve. There are challenges for forecasting the fluences and spectra of solar energetic particles. This will require better knowledge of interplanetary shock properties from the Sun to 1 AU (and beyond), the upstream slow solar wind and energetic seed particles. Dayside aurora, triggering of nightside substorms, and formation of new radiation belts can all be caused by shock and interplanetary ram pressure impingements onto the Earth’s magnetosphere. The acceleration and loss of relativistic magnetospheric killer electrons and penetrating electric fields in terms of causing positive and negative ionospheric storms are currently reasonable well understood, but refinements can still be made. The forecasting of extreme events (extreme shocks, extreme solar energetic particle events, and extreme geomagnetic storms (Carrington events or greater)) are also discussed. Energetic particle precipitation and ozone destruction is briefly discussed. For many of the studies, the Parker Solar Probe, Solar Orbiter, Magnetospheric Multiscale Mission (MMS), Arase, and SWARM data will be useful.

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Influence of the interplanetary driver type on the durations of the main and recovery phases of magnetic storms

Cited by 30 publications

References 59 publications

Effect of ICME‐Driven Storms on Field‐Aligned and Ionospheric Currents From AMPERE and SuperMAG

Effect of ICME‐Driven Storms on Field‐Aligned and Ionospheric Currents From AMPERE and SuperMAG

Double Superposed Epoch Analysis of Geomagnetic Storms and Corresponding Solar Wind and IMF in Solar Cycles 23 and 24

Space Weather Forecasting: What We Know Now and What Are the Current and Future Challenges?

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