Injection of electrons and protons with energies of tens of MeV into L &lt; 3 on 24 March 1991

Blake, J. B.; Kolasinski, W. A.; Fillius, R. W.; Mullen, E.G.

doi:10.1029/92gl00624

Cited by 398 publications

(346 citation statements)

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“…Usually, the two centers of the twin vortices are located approximately symmetrically with respect to the noon meridian corresponding to the normal incidence of the interplanetary shock along the SunEarth line. If the shock is incident obliquely on the afternoonside of the magnetosphere as reported by Blake et al [1992], the centers will rotate eastward around the north pole, and the current vortex on the morningside shifts toward noon. This situation is illustrated in Figure 10.…”

Section: Dp Fieldmentioning

confidence: 99%

Anomalous sudden commencement on March 24, 1991

Araki¹,

Fujitani²,

Emoto³

et al. 1997

J. Geophys. Res.

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Abstract. An anomalous geomagnetic sudden commencement (SC) occurred on March 24, 1991. It is characterized by an exceptionally large and sharp impulse observed in its initial part along the noon meridian in middle and low latitudes. The analysis of the SC was made by using high time resolution digital data from the 210 ø Meridian Magnetometer Chain in the west Pacific, Sub-Auroral Magnetometer Network (SAMNET) in the United Kingdom and southern Scandinavia, the EISCAT Magnetometer Cross in northern Scandinavia and Svalbard, and Canopus in Canada together with other ground and satellite (GOES 6, GOES 7, CRRES, and GMS) data. The results of the analysis suggest that the pulse observed at lower-latitude ground stations was caused by the propagation of a strong magnetospheric compression of short duration (less than 1 min) which has never been observed before this event. The HF Doppler observation in Kyoto near local noon seems to be consistent with existence of the bipolar electric field associated with the propagating compressional magnetic pulse. The SAMNET stations and CRRES in the early morning also detected positive pulses which delays 30-50 s from the pulses in noon sector. Although the delay in the peak time of the pulse observed on the ground is consistent with ionospheric hydromagnetic wave propagation from the dayside to the nightside with finite speed, the initial onset time of the pulse on the ground was almost simultaneous everywhere suggesting the existence of an "almost instantaneous" propagation mode below the ionosphere. [1993] successfully simulated this event by particle acceleration due to a sharp compressional electromagnetic pulse launched from the magnetopause at 1500 LT in the very initial stage of the SC. The CRRES actually observed an 130 nT monopolar magnetic pulse and an associated bipolar electric pulse with a peak-topeak amplitude of 80 mV/m. The duration of the pulse is about 2 min. Such a large and sharp pulse has never been observed before in this region of the magnetosphere. The SC itself might be produced by a coronal mass ejection (CME) driven interplanetary shock which was presumably related with a 3B optical flare at 2246 UT on March 22, 1991.Since the analyses of this event have mostly been limited to particle data so far, it is necessary to study properties of the electromagnetic pulse observed by CRRES in more detail by analyzing other magnetic data. Although the CRRES observations and the simulation by Li et al. [1993] greatly contributed to understand this peculiar event, we have to recognize that the CRRES observations were made at one point in the magnetosphere. It is difficult therefore to discuss in detail about excitation and propagation of the observed pulse. Analyses of SCs made so far [see Araki, 1994] show that a simple compression of the magnetosphere causes a complex global distribution of amplitude and waveform of SC. The main positive H component increase of SCs is often preceded by a positive or negative impulse of short duration. This preceding impulse ...

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Section: Dp Fieldmentioning

confidence: 99%

Anomalous sudden commencement on March 24, 1991

Araki¹,

Fujitani²,

Emoto³

et al. 1997

J. Geophys. Res.

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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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“…Nevertheless, between the CRRES orbit numbers 500 and 750, during one of the hugest injection/acceleration events (on March 24, 1991), the flux of electrons at all energies up to 15 MeV was enhanced by orders of magnitude on all drift shells down to L < 3. On such rare instances the slot region has filled up and for a few days afterward there is no way to distinguish between an inner and outer radiation belt in the equatorial flux distribution (Blake et al, 1992).…”

Section: The Contributions Of the Pioneer And Lunik Missionsmentioning

confidence: 99%

“…3, showing more modern observations of the temporal changes of electrons flux above different energy thresholds. These fluxes were measured between August 1990 and October 1991 by detectors on board of CRRES (Blake et al, 1992). This picture shows that electrons are impulsively injected or accelerated at all radial distances: i.e.…”

Section: The Contributions Of the Pioneer And Lunik Missionsmentioning

confidence: 99%

“…This proposal evolved into Argus -the first active experiment in space. Today we know that the Van Allen radiation belts have a fairly stable basic structure (Figure 4), and a highly dynamic nature that is influenced by intense space storms (e.g., Blake et al, 1992;Baker et al, 1997). The radiation belts population includes high-energy (>1 MeV) ions and electrons.…”

Section: Space Storm Effects In the Terrestrial Magnetosphere: Radiatmentioning

confidence: 99%

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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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Injection of electrons and protons with energies of tens of MeV into L < 3 on 24 March 1991

Abstract: On 24 March 1991 instrumentation aboard CRRES observed the almost instantaneous injection of electrons and protons with energies above 15 MeV into the L‐region 2 < L < 3. The energy spectrum of the injected electrons, a power law (E−6) peaked at 15 MeV and continued to at least 50 MeV

Cited by 398 publications

References 7 publications

Anomalous sudden commencement on March 24, 1991

Anomalous sudden commencement on March 24, 1991

The Energetic Electron Response to Magnetic Storms: HEO Satellite Observations

Space Storms and Space Weather Hazards

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