The Storm Time Development of Source Electrons and Chorus Wave Activity During CME‐ and CIR‐Driven Storms

Bingham, S.; Mouikis, C.; Kistler, L. M.; Paulson, K. W.; Farrugia, Charles J.; Huang, C. L.; Reeves, G. D.; Kletzing, C. A.

doi:10.1029/2019ja026689

Cited by 16 publications

(16 citation statements)

References 94 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…As the geomagnetic response varies between the HSS, CME, and QSW categories of the SW activity (e.g., Bingham et al, 2019; Ogawa et al, 2019; Shen et al, 2017), for statistical studies of EMIC wave events, it is important to have a systematic way of identifying the associated state of the SW. To identify the HSS, CME, and QSW conditions in the upstream SW we analyze the magnitude (| B |) and north‐south component ( B z ) of the IMF, the SW speed ( V sw ), and the SW proton density ( N sw ) preceding and during each EMIC wave event analyzed in this study. Here we use the 5‐min time resolution OMNI data, and all the SW data are propagated in time from the upstream point of observation to the nose of the Earth's bow shock.…”

Section: Resultsmentioning

confidence: 99%

EMIC Waves in the Earth's Inner Magnetosphere as a Function of Solar Wind Structures During Solar Maximum

2020

View full text Add to dashboard Cite

Here we analyze the statistics of electromagnetic ion cyclotron (EMIC) waves observed in the Earth's inner magnetosphere during coronal mass ejection (CME), high-speed stream (HSS), and quiet solar wind (QSW) conditions in the upstream solar wind (SW). For our analysis we use the EMIC wave observations by the two Van Allen Probes during their first magnetic local time (MLT) revolution. The major results of our analysis are as follows: (1) Criteria to identify the HSS, CME, and QSW conditions in the SW are formulated. (2) 54%, 36%, and 10% of EMIC wave events are observed during CME, HSS, and QSW, respectively. (3) 12% of events are closely associated with the fast growth of magnetospheric compression, among which 76%, 24%, and 0% are observed during CME, HSS, and QSW, respectively. (4) A majority of the QSW, HSS-driven, and CME-driven events is observed in the 9-12, 12-24, and 8-24 hr MLT sectors, respectively. (5) CME-driven events are distributed along all L shells, whereas the majority of the HSS-driven and QSW events are confined to L > 3.5. (6) The fractions of events during CME and HSS have a maximum in the near-equatorial region, whereas the fractions of the QSW events have a minimum there. (7) Independent of the SW driver, no strong events are observed below the local O + gyrofrequency, whereas 65-70% and 30-35% of events are observed between the O + and He + gyrofrequencies and above the He + gyrofrequency, respectively.

show abstract

Section: Resultsmentioning

confidence: 99%

EMIC Waves in the Earth's Inner Magnetosphere as a Function of Solar Wind Structures During Solar Maximum

2020

View full text Add to dashboard Cite

show abstract

“…This crucial assumption has to be tested and examined. Bingham et al () in this collection show the importance of the timing and the level of the seed electron enhancements in radiation belt dynamics through a superposed epoch analysis of the chorus wave activity, the seed electron development, and the outer radiation belt electron response between L* = 2.5 and L* = 5.5, for 25 coronal mass ejection and 35 corotating interaction region storms using Van Allen Probes observations (see also Bingham et al, ). Khoo et al () in this collection show that the initial enhancement of tens of kiloelectron volt electrons was observed before the initial enhancement of hundreds of kiloelectron volt electrons for five intense storm periods observed with the the Magnetic Electron Ion Spectrometer (MagEIS) instrument on board the Van Allen Probes (Blake et al, ).…”

Section: Particle Acceleration and Transport In The Inner And Outer Zmentioning

confidence: 99%

Particle Dynamics in the Earth's Radiation Belts: Review of Current Research and Open Questions

et al. 2020

View full text Add to dashboard Cite

The past decade transformed our observational understanding of energetic particle processes in near‐Earth space. An unprecedented suite of observational systems was in operation including the Van Allen Probes, Arase, Magnetospheric Multiscale, Time History of Events and Macroscale Interactions during Substorms, Cluster, GPS, GOES, and Los Alamos National Laboratory‐GEO magnetospheric missions. They were supported by conjugate low‐altitude measurements on spacecraft, balloons, and ground‐based arrays. Together, these significantly improved our ability to determine and quantify the mechanisms that control the buildup and subsequent variability of energetic particle intensities in the inner magnetosphere. The high‐quality data from National Aeronautics and Space Administration's Van Allen Probes are the most comprehensive in situ measurements ever taken in the near‐Earth space radiation environment. These observations, coupled with recent advances in radiation belt theory and modeling, including dramatic increases in computational power, have ushered in a new era, perhaps a “golden era,” in radiation belt research. We have edited a Journal of Geophysical Research: Space Science Special Collection dedicated to Particle Dynamics in the Earth's Radiation Belts in which we gather the most recent scientific findings and understanding of this important region of geospace. This collection includes the results presented at the American Geophysical Union Chapman International Conference in Cascais, Portugal (March 2018) and many other recent and relevant contributions. The present article introduces and review the context, current research, and main questions that motivate modern radiation belt research divided into the following topics: (1) particle acceleration and transport, (2) particle loss, (3) the role of nonlinear processes, (4) new radiation belt modeling capabilities and the quantification of model uncertainties, and (5) laboratory plasma experiments.

show abstract

“…Usanova et al, 2014) and sub-megaelectronvolt electrons (e.g. Blum et al, 2019;Hendry et al, 2019), although the efficiency of submegaelectronvolt electron precipitation is still debated. Both chorus and EMIC waves occur outside the high-density plasmasphere, whose outer boundary, the plasmapause, varies significantly in location with geomagnetic activity and also with the magnetic local time (MLT) (O'Brien and Moldwin, 2003).…”

Section: Introductionmentioning

confidence: 99%

Cosmic noise absorption signature of particle precipitation during interplanetary coronal mass ejection sheaths and ejecta

et al. 2020

View full text Add to dashboard Cite

Abstract. We study here energetic-electron (E>30 keV) precipitation using cosmic noise absorption (CNA) during the sheath and ejecta structures of 61 interplanetary coronal mass ejections (ICMEs) observed in the near-Earth solar wind between 1997 and 2012. The data come from the Finnish riometer (relative ionospheric opacity meter) chain from stations extending from auroral (IVA, 65.2∘ N geomagnetic latitude; MLAT) to subauroral (JYV, 59.0∘ N MLAT) latitudes. We find that sheaths and ejecta lead frequently to enhanced CNA (>0.5 dB) both at auroral and subauroral latitudes, although the CNA magnitudes stay relatively low (medians around 1 dB). Due to their longer duration, ejecta typically lead to more sustained enhanced CNA periods (on average 6–7 h), but the sheaths and ejecta were found to be equally effective in inducing enhanced CNA when relative-occurrence frequency and CNA magnitude were considered. Only at the lowest-MLAT station, JYV, ejecta were more effective in causing enhanced CNA. Some clear trends of magnetic local time (MLT) and differences between the ejecta and sheaths were found. The occurrence frequency and magnitude of CNA activity was lowest close to midnight, while it peaked for the sheaths in the morning and afternoon/evening sectors and for the ejecta in the morning and noon sectors. These differences may reflect differences in typical MLT distributions of wave modes that precipitate substorm-injected and trapped radiation belt electrons during the sheaths and ejecta. Our study also emphasizes the importance of substorms and magnetospheric ultra-low-frequency (ULF) waves for enhanced CNA.

show abstract

The Storm Time Development of Source Electrons and Chorus Wave Activity During CME‐ and CIR‐Driven Storms

Cited by 16 publications

References 94 publications

EMIC Waves in the Earth's Inner Magnetosphere as a Function of Solar Wind Structures During Solar Maximum

EMIC Waves in the Earth's Inner Magnetosphere as a Function of Solar Wind Structures During Solar Maximum

Particle Dynamics in the Earth's Radiation Belts: Review of Current Research and Open Questions

Cosmic noise absorption signature of particle precipitation during interplanetary coronal mass ejection sheaths and ejecta

Contact Info

Product

Resources

About