Simulation of the prompt energization and transport of radiation belt particles during the March 24, 1991 SSC

Li, Xinlin; Roth, I.; Temerin, M.; Wygant, J. R.; Hudson, M. K.; Blake, J. B.

doi:10.1029/93gl02701

Cited by 410 publications

(422 citation statements)

References 8 publications

(6 reference statements)

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“…on all (B,L) drift shells. They are energized by time dependent induction electric fields or betatron acceleration, as conclusively demonstrated by the numerical simulations of Li et al (1993). Massive flux enhancements, however, are observed less frequently at the deepest drift shells than at the outermost ones.…”

Section: The Contributions Of the Pioneer And Lunik Missionsmentioning

confidence: 55%

Space Storms and Space Weather Hazards

Daglis¹

2001

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Subject Terms Report Classification unclassified Classification of this page unclassified Classification of Abstract unclassified Limitation of Abstract UU Number of Pages 486REPORT DOCUMENTATION PAGE Public reporting burden for this collection of information is estimated to average 1 hour per response, including the time for reviewing instructions, searching existing data sources, gathering and maintaining the data needed, and completing and reviewing the collection of information. Send comments regarding this burden estimate or any other aspect of this collection of information, including suggestions for reducing this burden to Washington Headquarters Services, Directorate for Information Operations and Reports, 1215 Jefferson Davis Highway, Suite 1204, Arlington, VA 22202-4302, and to the Office of Management and Budget, -to review recent spacecraft measurements that have provided new insight into the dynamics and effects of space storms; -to review space weather hazards associated with space storms and pertinent to the operation of technological systems in space and on ground;-to discuss and assess methods of space weather forecasting, as well as national and international initiatives towards an efficient development of space climatology.Space weather, the invisible but nevertheless effective result of solar activity and solar-terrestrial coupling, has affected the operations of communication systems since the appearance of telegraph in the 19th century, though as an unknown trouble factor. Nowadays, the effects of space weather affect in various ways all communication modes, from cable to wireless to space-based systems. Moreover, space weather hazards include malfunction or even permanent damage of power distribution grids and of telecommunication, navigation and surveillance satellites, disturbances of over-the-horizon (OTH) radar, HF, VHF and UHF communications, surveying and navigation systems that use Global Positioning System (GPS) satellites, surveillance (optical and radar), and satellite tracking. Space weather influences on the Earth's weather and climate is still a developing topic. Little is known concerning the biological effects of space weather, especially regarding astronauts.This Institute could not be timelier. Space Weather, which has been defined as "conditions on the sun and in the solar wind, magnetosphere, ionosphere, and thermosphere that can influence the performance and reliability of space-and ground-based technological systems and can endanger human life", encompasses a broad range of phenomena impacting both space science and technology. The effects of Space Weather, while present throughout the solar cycle, gain particular prominence around the peak of the 11-year sunspot activity; the maximum of cycle 23 occurred in summer 2000.The fact that this ASI on Space Weather was held in Europe is particularly appropriate. European countries host a considerable repository of knowledge and world-class facilities in this field. Nevertheless, while Space Weather activities in c...

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Section: The Contributions Of the Pioneer And Lunik Missionsmentioning

confidence: 55%

Space Storms and Space Weather Hazards

Daglis¹

2001

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“…Specifically, it would be interesting to study the dependence of pitch angle dispersion with ring current intensity and other factors that are parameterized separately in more recent generations of the Tsyganenko models [Tsyganenko, 1995]. For detailed event studies it may be necessary to perform modeling calculations in time-dependent model fields either of MHD model runs or of heuristic models as has recently been done for electrons [Li et al, 1993[Li et al, , 1998]. are correct when the orbits are wrong, the effects of this scattering on the average drift needed to be included in the present calculations.…”

Section: Discussionmentioning

confidence: 99%

Pitch angle dispersion of ion injections

Anderson¹,

Takahashi²

2000

J. Geophys. Res.

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Abstract. Substorm-injected particles are time dispersed with pitch angle such that low pitch angle particles arrive earliest on the dayside at geosynchronous orbit, opposite the sense predicted by drift in a dipole field. In contrast to energy dispersion which is well understood, pitch angle dispersion of particle injections has not been quantitatively explained. We present a statistical analysis of energetic ion injections observed by the Active Magnetospheric Particle Tracer Explorers/Charge Composition Explorer (AMPTE/CCE) satellite, and we compare the results with model calculations of single-particle drift in realistic model magnetospheric electric and magnetic fields. The data analysis is based on observations made from August 1984 to February 1986, which cover all local times, radial distances between 5.5 and 8.8 Roe, and dipole latitudes between-16 ø and 16 ø and includes over 400 events mostly beyond 8 Roe. Using events observed between L = 8 and L = 9, where the effects of the satellite radial motion are minimal, we study the local time dependence of the injection delay time between different energies and pitch angles. We find that high pitch angle injection is delayed from low pitch angle injection and that the delay increases westward from the evening sector reaching --2 min (67 ø versus 23 ø pitch angles) at 1200 magnetic local time (MLT) at 120-220 keV. The observations are compared to proton drift calculations in static magnetic (T89c) and electric (Volland-Stern) field models. The calculations reproduce the observed drift times, pitch angle dispersion, and local time dependences, showing for the first time that sufficiently realistic magnetospheric magnetic field models can account for reverse pitch angle dispersion. Detailed examination of the curvature and gradient drift terms shows that the pitch angle dispersion is due principally to compression of the dayside magnetosphere, which preferentially suppresses the gradient and curvature drifts of near equatorially mirroring particles.

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“…This indicates that erosion of the plasmapause to low L is one process that occurs simultaneously with electrons being transported to or accelerated at equally low L. It is not clear from the observations in Figure 1 whether the erosion of the plasmapause is a necessary condition for all low-L electron flux enhancements. Shock acceleration of the type that occurred during the famous March 1991 event [Li et al, 1993;Blake et al, 1992] may occur without plasmapause erosion. However, the relationship between plasmapause erosion and low-L electron enhancements needs to be examined in detail.…”

Section: Observationsmentioning

confidence: 99%

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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Simulation of the prompt energization and transport of radiation belt particles during the March 24, 1991 SSC

Cited by 410 publications

References 8 publications

Space Storms and Space Weather Hazards

Space Storms and Space Weather Hazards

Pitch angle dispersion of ion injections

The Energetic Electron Response to Magnetic Storms: HEO Satellite Observations

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