Radiation belt 2D and 3D simulations for CIR-driven storms during Carrington Rotation 2068

Hudson, M. K.; Brito, Thiago; Elkington, S. R.; Kress, Brian; Zhao, Li; Wiltberger, M. J.

doi:10.1016/j.jastp.2012.03.017

Cited by 16 publications

(24 citation statements)

References 39 publications

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“…A dropout in flux centered on 90° pitch angle is the first indication of the IP shock arrival prior to the first drift echo. Note by contrast that the flux peaked at 90° in measurements from Probe A at L = 3 at the time of IP shock arrival, as reported by Kanekal et al () and Baker et al (), where drift shell splitting (Hudson et al, ; Sibeck et al ) and magnetopause shadowing are expected to have negligible effect, also evident in the low L value portion of Figure , left.…”

Section: Observations and Simulation Resultssupporting

confidence: 65%

Simulated Prompt Acceleration of Multi‐MeV Electrons by the 17 March 2015 Interplanetary Shock

et al. 2017

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Prompt enhancement of relativistic electron flux at L = 3–5 has been reported from Van Allen Probes Relativistic Electron Proton Telescope (REPT) measurements associated with the 17 March 2015 interplanetary shock compression of the dayside magnetosphere. Acceleration by ∼1 MeV is inferred on less than a drift timescale as seen in prior shock compression events, which launch a magnetosonic azimuthal electric field impulse tailward. This impulse propagates from the dayside around the flanks accelerating electrons in drift resonance at the dusk flank. Such longitudinally localized acceleration events produce a drift echo signature which was seen at >1 MeV energy on both Van Allen Probe spacecraft, with sustained observations by Probe B outbound at L = 5 at 2100 MLT at the time of impulse arrival, measured by the Electric Fields and Waves instrument. MHD test particle simulations are presented which reproduce drift echo features observed in the REPT measurements at Probe B, including the energy and pitch angle dependence of drift echoes observed. While the flux enhancement was short lived for this event due to subsequent inward motion of the magnetopause, stronger events with larger electric field impulses, as observed in March 1991 and the Halloween 2003 storm, produce enhancements which can be quantified by the inward radial transport and energization determined by the induction electric field resulting from dayside compression.

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Section: Observations and Simulation Resultssupporting

confidence: 65%

Simulated Prompt Acceleration of Multi‐MeV Electrons by the 17 March 2015 Interplanetary Shock

et al. 2017

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“…CIR‐driven storms also experience inward motion of the magnetopause due to increased solar wind dynamic pressure, which can be calculated from proton density and V x in Figure . With less flux increase by rapid radial transport and local heating than CME‐driven storms [ Hudson et al , ], CIR‐driven storms do not enhance flux as efficiently at and above 360 keV at lower L ∗ , see Figure . In summary, the results of this work using Van Allen Probe measurements confirm the relative importance of CIR‐driven storms at higher L ∗ and lower energy versus CME‐driven storms at lower L ∗ and higher energy.…”

Section: Discussionmentioning

confidence: 99%

Statistical study of the storm time radiation belt evolution during Van Allen Probes era: CME‐ versus CIR‐driven storms

et al. 2017

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Coronal mass ejection (CME)‐driven or corotating interaction region (CIR)‐driven storms can change the electron distributions in the radiation belt dramatically, which can in turn affect the spacecraft in this region or induce geomagnetic effects. The Van Allen Probes twin spacecraft, launched on 30 August 2012, orbit near the equatorial plane and across a wide range of L∗ with apogee at 5.8 RE and perigee at 620 km. Electron data from Van Allen Probes MagEIS and REPT instruments have been binned every 6 h at L∗=3 (defined as 2.5 < L∗<3.5), 4 (3.5 < L∗<4.5), 5 (4.5 < L∗<5.5). The superposed epoch analysis shows that (1) CME storms induce more electron flux enhancement at L∗=3 for energy channels below 1 MeV than CIR storms; (2) CME storms induce more electron flux enhancement at L∗=4 and 5 in the energy channels above 1 MeV than CIR storms; (3) CIR storms induce more electron flux enhancement at L∗=4 and 5 in the energy channels below 1 MeV than CME storms; (4) intense CME induce more than 50 times flux enhancement for the energy channel around 400 keV at L∗=3; (5) intense CIR induce more than 50 times flux enhancement for the energy channel around 200 keV at L∗=4. These results are consistent with a general picture of enhanced convection over a longer period for CIR storms which increased flux closer to geosynchronous orbit consistent with earlier studies, while CME storms likely produce deeper penetration of enhanced flux and local heating which is greater at higher energies at lower L∗.

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“…6. These fields can also be used in studies of longer-timescale behavior such as plasma sheet transport and adiabatic acceleration Kress et al, 2014) as well as radial diffusive acceleration over storm timescales (Elkington et al, 2002(Elkington et al, , 2004Fei et al, 2006;Huang et al, 2010;Hudson et al, 2012). Figure B1 shows a shock impulse arrival measured by two ground-based magnetometers from the Canadian magnetometer array CARISMA on 8 October 2013.…”

Section: Discussion and Summarymentioning

confidence: 99%

Magnetohydrodynamic modeling of three Van Allen Probes storms in 2012 and 2013

et al. 2015

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Abstract. Coronal mass ejection (CME)-shock compression of the dayside magnetopause has been observed to cause both prompt enhancement of radiation belt electron flux due to inward radial transport of electrons conserving their first adiabatic invariant and prompt losses which at times entirely eliminate the outer zone. Recent numerical studies suggest that enhanced ultra-low frequency (ULF) wave activity is necessary to explain electron losses deeper inside the magnetosphere than magnetopause incursion following CME-shock arrival. A combination of radial transport and magnetopause shadowing can account for losses observed at radial distances into L = 4.5, well within the computed magnetopause location. We compare ULF wave power from the Electric Field and Waves (EFW) electric field instrument on the Van Allen Probes for the 8 October 2013 storm with ULF wave power simulated using the Lyon-FedderMobarry (LFM) global magnetohydrodynamic (MHD) magnetospheric simulation code coupled to the Rice Convection Model (RCM). Two other storms with strong magnetopause compression, 8-9 October 2012 and 17-18 March 2013, are also examined. We show that the global MHD model captures the azimuthal magnetosonic impulse propagation speed and amplitude observed by the Van Allen Probes which is responsible for prompt acceleration at MeV energies reported for the 8 October 2013 storm. The simulation also captures the ULF wave power in the azimuthal component of the electric field, responsible for acceleration and radial transport of electrons, at frequencies comparable to the electron drift period. This electric field impulse has been shown to explain observations in related studies (Foster et al., 2015) of electron acceleration and drift phase bunching by the Energetic Particle, Composition, and Thermal Plasma Suite (ECT) instrument on the Van Allen Probes.

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Radiation belt 2D and 3D simulations for CIR-driven storms during Carrington Rotation 2068

Cited by 16 publications

References 39 publications

Simulated Prompt Acceleration of Multi‐MeV Electrons by the 17 March 2015 Interplanetary Shock

Simulated Prompt Acceleration of Multi‐MeV Electrons by the 17 March 2015 Interplanetary Shock

Statistical study of the storm time radiation belt evolution during Van Allen Probes era: CME‐ versus CIR‐driven storms

Magnetohydrodynamic modeling of three Van Allen Probes storms in 2012 and 2013

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