A telescopic and microscopic examination of acceleration in the June 2015 geomagnetic storm: Magnetospheric Multiscale and Van Allen Probes study of substorm particle injection

Baker, D. N.; Jaynes, A. N.; Turner, D. L.; Nakamura, R.; Schmid, Daniel; Mauk, B. H.; Cohen, I. J.; Fennell, J. F.; Blake, J. B.; Strangeway, R. J.; Russell, C. T.; Torbert, R. B.; Dorelli, J.; Gershman, D. J.; Giles, B. L.; Burch, J. L.

doi:10.1002/2016gl069643

Cited by 31 publications

(19 citation statements)

References 32 publications

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“…We should remark here that the June 2015 storm period offered an opportunity to utilize new measurements made by the recently launched four‐spacecraft Magnetospheric Multiscale (MMS) mission. In [ Baker et al , ], the VAP measurements as described here have been studied in the context of the high spatial and temporal resolution data from the MMS spacecraft. These results strongly reaffirm the findings of Jaynes et al .…”

Section: Discussionmentioning

confidence: 99%

Highly relativistic radiation belt electron acceleration, transport, and loss: Large solar storm events of March and June 2015

et al. 2016

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Two of the largest geomagnetic storms of the last decade were witnessed in 2015. On 17 March 2015, a coronal mass ejection‐driven event occurred with a Dst (storm time ring current index) value reaching −223 nT. On 22 June 2015 another strong storm (Dst reaching −204 nT) was recorded. These two storms each produced almost total loss of radiation belt high‐energy (E ≳ 1 MeV) electron fluxes. Following the dropouts of radiation belt fluxes there were complex and rather remarkable recoveries of the electrons extending up to nearly 10 MeV in kinetic energy. The energized outer zone electrons showed a rich variety of pitch angle features including strong “butterfly” distributions with deep minima in flux at α = 90°. However, despite strong driving of outer zone earthward radial diffusion in these storms, the previously reported “impenetrable barrier” at L ≈ 2.8 was pushed inward, but not significantly breached, and no E ≳ 2.0 MeV electrons were seen to pass through the radiation belt slot region to reach the inner Van Allen zone. Overall, these intense storms show a wealth of novel features of acceleration, transport, and loss that are demonstrated in the present detailed analysis.

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Section: Discussionmentioning

confidence: 99%

Highly relativistic radiation belt electron acceleration, transport, and loss: Large solar storm events of March and June 2015

et al. 2016

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“…Substorms are more transient and less predictable than storms, and they may cause substantial damage to satellites (Connors et al, 2011) and ground-based systems (Boteler, 2001). They also inject the seed populations of energetic radiation belt particles that are further accelerated during storms (Baker et al, 2016;Reeves et al, 2003;Turner et al, 2015). Since the beginning of space era, substorms were considered as building blocks of storms (Chapman, 1962;Kamide, 1992;Kamide et al, 1998;Sharma et al, 2013).…”

Section: 1029/2018ja025843mentioning

confidence: 99%

Global Empirical Picture of Magnetospheric Substorms Inferred From Multimission Magnetometer Data

et al. 2019

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Magnetospheric substorms represent key explosive processes in the interaction of the Earth's magnetosphere with the solar wind, and their understanding and modeling are critical for space weather forecasting. During substorms, the magnetic field on the nightside is first stretched in the antisunward direction and then it rapidly contracts earthward bringing hot plasmas from the distant space regions into the inner magnetosphere, where they contribute to geomagnetic storms and Joule dissipation in the polar ionosphere, causing impressive splashes of aurora. Here we show for the first time that mining millions of spaceborne magnetometer data records from multiple missions allows one to reconstruct the global 3‐D picture of these stretching and dipolarization processes. Stretching results in the formation of a thin (less than the Earth's radius) and strong current sheet, which is diverted into the ionosphere during dipolarization. In the meantime, the dipolarization signal propagates further into the inner magnetosphere resulting in the accumulation of a longer lived current there, giving rise to a protogeomagnetic storm. The global 3‐D structure of the corresponding substorm currents including the substorm current wedge is reconstructed from data.

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“…Electron radiation belt variability is particularly evident during geomagnetic storms (e.g., Baker, Jaynes, Turner, et al, 2016;Baker, Jaynes, Kanekal, et al, 2016), which is the focus of this statistical study. ©2019.…”

Section: Introductionmentioning

confidence: 99%

The Response of Earth's Electron Radiation Belts to Geomagnetic Storms: Statistics From the Van Allen Probes Era Including Effects From Different Storm Drivers

et al. 2019

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A statistical study was conducted of Earth's radiation belt electron response to geomagnetic storms using NASA's Van Allen Probes mission. Data for electrons with energies ranging from 30 keV to 6.3 MeV were included and examined as a function of L‐shell, energy, and epoch time during 110 storms with SYM‐H ≤−50 nT during September 2012 to September 2017 (inclusive). The radiation belt response revealed clear energy and L‐shell dependencies, with tens of keV electrons enhanced at all L‐shells (2.5 ≤ L ≤ 6) in all storms during the storm commencement and main phase and then quickly decaying away during the early recovery phase, low hundreds of keV electrons enhanced at lower L‐shells (~3 ≤ L ≤ ~4) in upward of 90% of all storms and then decaying gradually during the recovery phase, and relativistic electrons throughout the outer belt showing main phase dropouts with subsequent and generally unpredictable levels of replenishment during the recovery phase. Compared to prestorm levels, electrons with energies >1 MeV also revealed a marked increase in likelihood of a depletion at all L‐shells through the outer belt (3.5 ≤ L ≤ 6). Additional statistics were compiled revealing the storm time morphology of the radiation belts, confirming the aforementioned qualitative behavior. Considering storm drivers in the solar wind: storms driven by coronal mass ejection (CME) shocks/sheaths and CME ejecta only are most likely to result in a depletion of >1‐MeV electrons throughout the outer belt, while storms driven by full CMEs and stream interaction regions are most likely to produce an enhancement of MeV electrons at lower (L < ~5) and higher (L > ~4.5) L‐shells, respectively. CME sheaths intriguingly result in a distinct enhancement of ~1‐MeV electrons around L~5.5, and on average, CME sheaths and stream interaction regions result in double outer belt structures.

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A telescopic and microscopic examination of acceleration in the June 2015 geomagnetic storm: Magnetospheric Multiscale and Van Allen Probes study of substorm particle injection

Cited by 31 publications

References 32 publications

Highly relativistic radiation belt electron acceleration, transport, and loss: Large solar storm events of March and June 2015

Highly relativistic radiation belt electron acceleration, transport, and loss: Large solar storm events of March and June 2015

Global Empirical Picture of Magnetospheric Substorms Inferred From Multimission Magnetometer Data

The Response of Earth's Electron Radiation Belts to Geomagnetic Storms: Statistics From the Van Allen Probes Era Including Effects From Different Storm Drivers

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