Solar proton increases and dynamics of the electron outer radiation belt during solar events in December 2006

Tverskaya, L. V.; Balashov, Sergey; Vedenkin, N.; Ivanov, V. V.; Иванова, Т. А.; Karpenko, D. S.; Kochura, S. G.; Максимов, И. В.; Pavlov, N. N.; Rubinstein, I. A.; Teltsov, M. V.; Trofimchuk, D. A.; Tulupov, V. I.; Хартов, В. В.

doi:10.1134/s0016793208060042

Cited by 5 publications

(3 citation statements)

References 3 publications

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“…Mechanisms that are thought to act on the outer proton radiation belt include radial diffusion caused by magnetic and electric perturbations [e.g., Nakada et al , ; Cornwall , ; Beutier et al , ; Boscher et al , ; Vacaresse et al , ; Panasyuk , ] including substorm perturbations [ Spjeldvik , ; Smolin , ], pitch angle scattering by magnetic field curvature effects in the stretched nightside magnetic field [ Tsyganenko , ; Sergeev et al , ], pitch angle scattering and energy diffusion by plasmaspheric whistler mode hiss [ Kozyra et al , ; Villalon and Burke , ] and by ion cyclotron waves [ Søraas et al , ; Shoji and Omura , ], and charge exchange and Coulomb scattering [ Liemohn , ; Beutier et al , ; Walt et al , ]. Potential sources for the outer proton radiation belt include solar protons [ Lazutin et al , ; Panasyuk , ; Tverskaya et al , ] and substorm particle injections [ Vacaresse et al , ]. Finite gyroradius effects can be important for the proton radiation belt, whereas in the nominal dipole field strength of 106 nT at geosynchronous orbit (6.6 R E ) a 1 MeV ( γ = 1.001) proton has a gyroradius r g of 1370 km, whereas a 1 MeV ( γ = 2.96) electron has a gyroradius of 45 km (using the formula r g = [(2Em) 1/2 c/eB][1 + (E/2mc 2 )] 1/2 with kinetic energy E.…”

Section: Introductionmentioning

confidence: 99%

“…Although the outer proton radiation belt has been observed by spacecraft instrumentation for five decades [e.g., Davis and Williamson , , ; Yershkovitch et al , ; Stevens et al , ; Spjeldvik , ; Fritz and Spjeldvik , ; Sheldon , ; Green et al , ; Lazutin et al , , ; Tverskaya et al , ; Forster et al , ], much less is known about its properties and dynamics than is known about the outer electron radiation belt. Modeling efforts for the outer proton radiation belt in those five decades [e.g., Nakada and Mead , ; Spjeldvik , ; Beutier et al , ; Bourdarie et al , ; Boscher et al , ; Vacaresse et al , ; Panasyuk , ; Smolin , , ] have been much less sophisticated than the modeling efforts for the outer electron radiation belt.…”

Section: Introductionmentioning

confidence: 99%

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The proton and electron radiation belts at geosynchronous orbit: Statistics and behavior during high‐speed stream‐driven storms

Borovsky

Cayton²,

Denton

et al. 2016

JGR Space Physics

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The outer proton radiation belt (OPRB) and outer electron radiation belt (OERB) at geosynchronous orbit are investigated using a reanalysis of the LANL CPA (Charged Particle Analyzer) 8‐satellite 2‐solar cycle energetic particle data set from 1976 to 1995. Statistics of the OPRB and the OERB are calculated, including local time and solar cycle trends. The number density of the OPRB is about 10 times higher than the OERB, but the 1 MeV proton flux is about 1000 times less than the 1 MeV electron flux because the proton energy spectrum is softer than the electron spectrum. Using a collection of 94 high‐speed stream‐driven storms in 1976–1995, the storm time evolutions of the OPRB and OERB are studied via superposed epoch analysis. The evolution of the OERB shows the familiar sequence (1) prestorm decay of density and flux, (2) early‐storm dropout of density and flux, (3) sudden recovery of density, and (4) steady storm time heating to high fluxes. The evolution of the OPRB shows a sudden enhancement of density and flux early in the storm. The absence of a proton dropout when there is an electron dropout is noted. The sudden recovery of the density of the OERB and the sudden density enhancement of the OPRB are both associated with the occurrence of a substorm during the early stage of the storm when the superdense plasma sheet produces a “strong stretching phase” of the storm. These storm time substorms are seen to inject electrons to 1 MeV and protons to beyond 1 MeV into geosynchronous orbit, directly producing a suddenly enhanced radiation belt population.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The proton and electron radiation belts at geosynchronous orbit: Statistics and behavior during high‐speed stream‐driven storms

Borovsky

Cayton²,

Denton

et al. 2016

JGR Space Physics

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“…Within a few hours the European Giove, a research spacecraft in medium Earth orbit began reporting spacecraft charging effects that continued into January 2007 (Fig. 12, Cannon, 2013) as Earth's radiation belts were energized and remained so for weeks (Tverskaya et al, 2008).…”

Section: December 2006 Storm Event Timelinementioning

confidence: 99%

Timelines as a tool for learning about space weather storms

Knipp

Bernstein

Wahl

et al. 2021

J. Space Weather Space Clim.

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Space weather storms typically have solar, interplanetary, geophysical and societal-effect components that overlap in time, making it hard for students and novices to determine cause-and-effect relationships and relative timing. To address this issue, we use timelines to provide context for space weather storms of different intensities. First, we present a timeline and tabular description for the great auroral storms of the last 500 years as an example for space climate. The graphical summary for these 14 events suggests that they occur about every 40-60 years, although the distribution of such events is far from even. One outstanding event in 1770 may qualify as a one-in-500-year auroral event, based on duration. Additionally, we present two examples that describe space weather storms using solar, geospace and effects categories. The first of these is for the prolonged storm sequence of late January1938 that produced low-latitude auroras and space weather impacts on mature technology (telegraphs) and on high frequency radio communication for aviation, which was a developing technology. To illustrate storm effects in the space-age, we produce a detailed timeline for the strong December 2006 geomagnetic storm that impacted numerous space-based technologies for monitoring space weather and for communication and navigation. During this event there were numerous navigations system disturbances and hardware disruptions. We adopt terminology developed in many previous space weather studies and blend it with historical accounts to create graphical timelines to help organize and disentangle the events presented herein.

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Planetary Distribution of the Space Radiation Dose Rate Based on Results of the DEPRON Experiment Onboard the Lomonosov Satellite

et al. 2022

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Solar proton increases and dynamics of the electron outer radiation belt during solar events in December 2006

Cited by 5 publications

References 3 publications

The proton and electron radiation belts at geosynchronous orbit: Statistics and behavior during high‐speed stream‐driven storms

The proton and electron radiation belts at geosynchronous orbit: Statistics and behavior during high‐speed stream‐driven storms

Timelines as a tool for learning about space weather storms

Planetary Distribution of the Space Radiation Dose Rate Based on Results of the DEPRON Experiment Onboard the Lomonosov Satellite

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