Understanding relativistic electron losses with BARREL

Millan, R. M.

doi:10.1016/j.jastp.2011.01.006

Cited by 34 publications

(31 citation statements)

References 52 publications

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“…The two types are differentiated by their temporal profiles and distribution in magnetic local time as described in detail in Millan (2011), and briefly reviewed here.…”

Section: Types Of Relativistic Electron Precipitationmentioning

confidence: 99%

“…Such maps reveal important features such as the effects of the South Atlantic Magnetic Anomaly, but the spacecraft revisit a particular location infrequenty, thus limiting the time resolution. Observations from the MINIS balloons revealed complicated temporal and spatial structure of energetic precipitation (Millan 2011) which can only be observed from a nearly stationary platform that does not move quickly through the precipitation region. Untangling the spatial structure of precipitation should reveal information about important boundaries that control or influence precipitation.…”

Section: Large-scale Spatial Structure Of Relativistic Precipitationmentioning

confidence: 99%

“…Wave-particle interactions are believed to be the main cause of scattering into the atmospheric loss cone (see e.g., Millan andThorne 2007 andThorne 2010 for a review). However, there is still very little quantitative comparison between theoretical predictions and observational data.…”

Section: Introductionmentioning

confidence: 99%

“…Test campaigns, conducted from McMurdo, Antarctica in 2009 and 2010 with support from the NSF and NASA/CSBF, allowed for validation of the payload design in the actual flight environment, and improvement of the operations plans. Science data were also obtained and preliminary results are summarized in Millan (2011).…”

Section: Introductionmentioning

confidence: 99%

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The Balloon Array for RBSP Relativistic Electron Losses (BARREL)

et al. 2013

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“…The two types are differentiated by their temporal profiles and distribution in magnetic local time as described in detail in Millan (2011), and briefly reviewed here.…”

Section: Types Of Relativistic Electron Precipitationmentioning

confidence: 99%

Section: Large-scale Spatial Structure Of Relativistic Precipitationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

The Balloon Array for RBSP Relativistic Electron Losses (BARREL)

et al. 2013

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“…For more than twenty years, observations of 'microbursts,' short bursts of relativistic electrons, have been seen by balloon detectors or low altitude satellites imaging the loss cone [Blake et al, 1996;Millan andThorne, 2007, Millan et al, 2011 for review]. Although electromagnetic ion cyclotron waves [Thorne and Kennel, 1971;Alpert and Bortnik, 2009] are often proposed to provide the scattering, no good explanation has yet been presented that can account for all the observed phenomenology.…”

Section: Waves Are Associated With Microburstsmentioning

confidence: 99%

Large-Amplitude Whistler Waves and Electron Acceleration in the Earth's Radiation Belts: A Review of Stereo and Wind Observations

Cattell¹,

Breneman²,

Goetz³

et al. 2013

Dynamics of the Earth's Radiation Belts and Inner Magnetosphere

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One of the critical problems for understanding the dynamics of Earth's radiation belts is determining the physical processes that energize and scatter relativistic electrons. We review measurements from the Wind/Waves and STEREO S/Waves waveform capture instruments of large amplitude whistler-mode waves. These observations have provided strong evidence that large amplitude (100s mV/m) whistlermode waves are common during magnetically active periods. The large amplitude whistlers have characteristics that are different from typical chorus. They are usually nondispersive and obliquely propagating, with a large longitudinal electric field and significant parallel electric field. We will also review comparisons of STEREO and Wind wave observations with SAMPEX observations of electron microbursts. Simulations show that the waves can result in energization by many MeV and/or scattering by large angles during a single wave packet encounter due to coherent, nonlinear processes including trapping. The experimental observations combined with simulations suggest that quasilinear theoretical models of electron energization and scattering via smallhttps://ntrs.nasa.gov/search.jsp?R=20120016644 2018-05-13T02:45:38+00:00Z amplitude waves, with timescales of hours to days, may be inadequate for understanding radiation belt dynamics.

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Van Allen Probes observations of direct wave‐particle interactions

Fennell

Roeder

Kurth

et al. 2014

Geophysical Research Letters

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Quasiperiodic increases, or "bursts," of 17-26 keV electron fluxes in conjunction with chorus wave bursts were observed following a plasma injection on 13 January 2013. The pitch angle distributions changed during the burst events, evolving from sin N (α) to distributions that formed maxima at α = 75-80°, while fluxes at 90°and <60°remained nearly unchanged. The observations occurred outside of the plasmasphere in the postmidnight region and were observed by both Van Allen Probes. Density, cyclotron frequency, and pitch angle of the peak flux were used to estimate resonant electron energy. The result of~15-35 keV is consistent with the energies of the electrons showing the flux enhancements and corresponds to electrons in and above the steep flux gradient that signals the presence of an Alfvén boundary in the plasma. The cause of the quasiperiodic nature (on the order of a few minutes) of the bursts is not understood at this time.

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Understanding relativistic electron losses with BARREL

Cited by 34 publications

References 52 publications

The Balloon Array for RBSP Relativistic Electron Losses (BARREL)

The Balloon Array for RBSP Relativistic Electron Losses (BARREL)

Large-Amplitude Whistler Waves and Electron Acceleration in the Earth's Radiation Belts: A Review of Stereo and Wind Observations

Van Allen Probes observations of direct wave‐particle interactions

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