Ring current particle distributions during the magnetic storms of December 16-18, 1971

Smith, Paul H.; Hoffman, R. A.

doi:10.1029/ja078i022p04731

Cited by 157 publications

(79 citation statements)

References 6 publications

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“…Protons in the energy range (5-30 keV in this case) of maximum storm time enhancement (Smith and Hoffman, 1974) show the most rapid decay, and eventually develop a minimum in the spectrum characteristic of the quiet-time spectrum (Smith, 1973). The hiah energv nrotons (>100 keV1, which were depleted during the main phase due mostly to adiabatic compression (Williams, 1970), increase in flux during the gradual storm recovery.…”

Section: Oqservationsmentioning

confidence: 88%

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Ring current proton decay by charge exchange

Smith

Hoffman

Fritz³

1976

J. Geophys. Res.

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Explorer 45 (S 3 -A) measurements during the recover y phase (,f a moderate magnet;; storm have confirmed that the char g e exchange decay mechanism can account f or the decay of the storm-time proton ring current. The moderate mannetic storm of 24 February 1972 was selected for study since a svi mccric ring current hr , developed and effects due to asymmetric rin g current losses ^o!-a eliminated.In this study it was found that after the initial rapid deca y of the p roton flux, which is a consequence of the dissipation of the asymmetric ring current, the equatorially mirroring protons in the energy range 5-30 keV decayed throu q hout the L-value ran g e of 3.5 to 5.0 at the r '-arge exchange decay rate calculated by Liemohn (1961).After several days of decay, the proton fluxes reached a lower limit where an ap p arent equilibrium was maintained, between weak particle source mechanisms and the loss mechanisms, until fresh protons were injected into the rinq curr-nt renion durin q substorms. blhile other proton loss mechanisms may also be operating, the results indicate that charge exchange can entirely account for the storm-time proton ring current decay, and that this mechanism must be considered in all studies involving the loss of proton rinq current particles.

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Section: Oqservationsmentioning

confidence: 88%

“…proton data have previously shown that OE most dynamic energy region of the earth's ring current is from about 10 keV to 100 keV (Smith and Hoffman, 1972;1974;Williams, et al, 1973;Fritz, et al, 1974). …”

Section: Oqservationsmentioning

confidence: 97%

Ring current proton decay by charge exchange

Smith

Hoffman

Fritz³

1976

J. Geophys. Res.

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“…Satellite-measured spectra of ion energy density (proton assumed) during the prestorm quiet (Orbit 97 of the Explorer 45 satellite, or S 3 ) and during a large geomagnetic storm (Orbit 102). After Smith and Hoffman (1973). during a quiet period and during an intense geomagnetic storm (Smith and Hoffman, 1973).…”

Section: 2mentioning

confidence: 99%

“…After Smith and Hoffman (1973). during a quiet period and during an intense geomagnetic storm (Smith and Hoffman, 1973).…”

Section: 2mentioning

confidence: 99%

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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“…Figure 1 contains data from Orbit 99 during the storm which did not develop a symmetric ring current (Cahill, 1972;Smith and Hoffman, 1972). The outbound portion of the orbit in the evening hours displayed some of the usual charactertistics of an inflated magnetic field, a constant negative AB out towards the region of maximum particle energy density, a minimum in the field near the maximum of the protons, and a recovery at larger distances.…”

Section: Field Deformations and Proton Energy Density Distributionsmentioning

confidence: 99%

Particle and field observations from Explorer 45 during the December 1971 magnetic storm period

Hoffman¹

1973

J. Geophys. Res.

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The magnetic signatures of the extraterrestrial ring current have been measured by means of satellite‐borne magnetometers on several occasions [Smith et al., 1960; Cahill, 1966; Coleman and Cummings, 1967; Sugiura et al., 1971]. In only one case have the charged particles of the magnetic storm‐time extraterrestrial ring current system been directly observed [Frank, 1967]. In this note we present simultaneous observations from the S3‐A (Explorer 45) satellite of the magnetic signature of the ring current and complete measurements of the proton ring current to distances of 5.24 RE during the double magnetic storm of December 16–19, 1971. Magnetic records from low‐latitude and auroral magnetic observatories for this period have already been presented [Cahill, 1973].

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Ring current particle distributions during the magnetic storms of December 16-18, 1971

Cited by 157 publications

References 6 publications

Ring current proton decay by charge exchange

Ring current proton decay by charge exchange

Space Storms and Space Weather Hazards

Particle and field observations from Explorer 45 during the December 1971 magnetic storm period

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