Electron scattering loss in Earth's inner magnetosphere: 1. Dominant physical processes

Abel, Bob; Thorne, R. M.

doi:10.1029/97ja02919

Cited by 464 publications

(677 citation statements)

References 38 publications

(6 reference statements)

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“…In this region and at these energies whistler mode waves from ground-based VLF transmitters, used for communication with submarines are likely to be the dominant loss mechanism [e.g., Abel and Thorne, 1998a].…”

Section: Discussionmentioning

confidence: 99%

Slot region electron loss timescales due to plasmaspheric hiss and lightning‐generated whistlers

et al. 2007

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[1] Energetic electrons (E > 100 keV) in the Earth's radiation belts undergo Dopplershifted cyclotron resonant interactions with a variety of whistler mode waves leading to pitch angle scattering and subsequent loss to the atmosphere. In this study we assess the relative importance of plasmaspheric hiss and lightning-generated whistlers in the slot region and beyond. Electron loss timescales are determined using the Pitch Angle and energy Diffusion of Ions and Electrons (PADIE) code with global models of the spectral distributions of the wave power based on CRRES observations. Our results show that plasmaspheric hiss propagating at small and intermediate wave normal angles is a significant scattering agent in the slot region and beyond. In contrast, plasmaspheric hiss propagating at large wave normal angles and lightning-generated whistlers do not contribute significantly to radiation belt loss. The loss timescale of 2 MeV electrons due to plasmaspheric hiss propagating at small and intermediate wave normal angles in the center of the slot region (L = 2.5) lies in the range 1-10 days, consistent with recent Solar Anomalous and Magnetospheric Particle Explorer (SAMPEX) observations. Wave turbulence in space, which is responsible for the generation plasmaspheric hiss, thus leads to the formation of the slot region. During active periods, losses due to plasmaspheric hiss may occur on a timescale of 1 day or less for a wide range of energies, 200 keV < E < 1 MeV, in the region 3.5 < L < 4.0. Plasmaspheric hiss may thus also be a significant loss process in the inner region of the outer radiation belt during magnetically disturbed periods.Citation: Meredith, N. P., R. B. Horne, S. A. Glauert, and R. R. Anderson (2007), Slot region electron loss timescales due to plasmaspheric hiss and lightning-generated whistlers,

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Section: Discussionmentioning

confidence: 99%

Slot region electron loss timescales due to plasmaspheric hiss and lightning‐generated whistlers

et al. 2007

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“…On the other hand, the loss mechanism of the particles has been discussed in relation to the atmospheric loss (e.g. Walt, 1964;Williams et al, 1968;Abel and Thorne, 1998a and 1998b) and to the whistler mode waves (e.g. Lyons and Williams, 1975;Tsurutani et al, 1975;Throne, 1998a and1998b).…”

Section: Introductionmentioning

confidence: 99%

Pitch angle distribution of relativistic electrons in the inner radiation belt and its relation to equatorial plasma wave turbulence phenomena

Morioka¹,

Misawa²,

Miyoshi³

et al. 2001

Geophysical Research Letters

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Abstract. The pitch angie distribution of relativistic electrons in the inner radiation belt and its relation to local plasma waves were investigated using the data from the Akebono satellite. It was found that energetic electrons (> i MeV) in the inner radiation belt showed an unexpected dumbbell distribution near the magnetic equator. This feature was commonly observed both in magnetically disturbed and undisturbed conditions. It was also found that this anomalous pitch angle distribution of energetic electrons was always accompanied with the enhancement of local UHR waves around the magnetic equator. These newly found features indicate the existence of an unknown waveparticle interaction process between the relativistic electrons and quasi-electrostatic plasma waves in the equatorial region of the plasmasphere.

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“…Part of the answer lies in the flux decays. The decay times indicate that combined transport and loss process along the field lines matches expectations for wave-particle interaction models of the type discussed by Lyons and Thome [1973] and Abel and Thome [1998]. The processes are primarily ones of pitch angle transport, coulomb drag (energy transport), and atmospheric losses in competition with radial transport.…”

Section: Discussionmentioning

confidence: 56%

The Energetic Electron Response to Magnetic Storms: HEO Satellite Observations

Fennell

Blake

Friedel

et al. 2013

The Inner Magnetosphere: Physics and Modeling

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Public reporting burden for this collection of information is estimated to average 1 ttour per response, including the time for reviewing instructions, searching existing data sources, gathering and maintaining the data needed, and completing and reviewing this collection of information. Send comments regarding this burden estimate or any other aspect of this collection of infomnation, including suggestions for reducing this burden PERFORMING ORGANIZATION NAME(S) AND ADDRESS(ES)The Aerospace Corporation Laboratory Operations El Segundo, CA 90245-4691 PERFORMING ORGANIZATION REPORT NUMBER TR-2004(8570)-5 SPONSORING / MONITORING AGENCY NAME(S) AND ADDRESS(ES)Space and Missile Systems Center Air Force Space Command 2450 E. El Segundo Blvd. Los Angeles Air Force Base, CA 90245 SPONSOR/MONITOR'S ACRONYM(S) SMC SPONSOR/MONITOR'S REPORT NUMBER(S)SMC-TR-04-22 DISTRIBUTION/AVAILABILITY STATEMENTApproved for public release; distribution unlimited. SUPPLEMENTARY NOTES 20041008 318 ABSTRACTThe energetic electron observations from the HEO 97-068 satellite are used to study the electron response to magnetic storms in the inner magnetosphere during 1998-2002. The observations cover L values in the range 2.5 < L < 6. The same L values are covered at both high (>2.3 Re) and low (<1.2 Re) geocentric altitudes. The electron flux histories at low and high altitudes are directly compared and are found to track with a high degree of fidelity independent of flux levels and energy for a wide range of L values. The low-altitude >1.5 MeV electron fluxes were ~10-16% of the high-altitude fluxes for L = 3-5.5, except during the rapid post-storm flux rises. The decay of the post-storm electron fluxes were examined to obtain the e-folding decay times at L = 3, near the peak of the outer zone. The high-altitude >1.5 MeV electron fluxes were found to have three distinct 1/e decay times of about 5,10.5, and 17.5 days. The 5 and 10.5 day efolding times ocurred in the first several days after the post-storm fluxes peaked during 2000-2001 and 1998 periods, respectively. The longer e-folding times occurred late in the decay history. These results support the view that the acceleration and loss mechanisms are operating essentially simultaneously over much of the outer zone. SUBJECT TERMS

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Electron scattering loss in Earth's inner magnetosphere: 1. Dominant physical processes

Cited by 464 publications

References 38 publications

Slot region electron loss timescales due to plasmaspheric hiss and lightning‐generated whistlers

Slot region electron loss timescales due to plasmaspheric hiss and lightning‐generated whistlers

Pitch angle distribution of relativistic electrons in the inner radiation belt and its relation to equatorial plasma wave turbulence phenomena

The Energetic Electron Response to Magnetic Storms: HEO Satellite Observations

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