Protons in the outer zone of the radiation belt

Bame, S. J.; Conner, J. P.; Hill, Herbert H.; Holly, Francis E.

doi:10.1029/jz068i001p00055

Cited by 20 publications

(4 citation statements)

References 16 publications

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“…The integral spectra given by Bame et al, (1963) and are very steep and agree relatively well with the spectra derived in this work, allowing for the different locations and the accuracy of the measurements.…”

Section: Discussionsupporting

confidence: 76%

“…These levels seem to be lower by about a factor of ten than the present data, although the different locations of the measurements as well as variations in the outer zone may account for the difference. Bame et al, (1963) give an intensity of -5 x 10 5/cm 2sec ster for protons above -1 Mev at L a 2. 5…”

Section: Discussionmentioning

confidence: 89%

“…Some data on protons in the energy range examined in this paper have been given by , Bame et al, (1963) and Pieper et al, (1962). These experimenters mention intensities of 04 05 c2…”

Section: Discussionmentioning

confidence: 98%

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The Energetic Charged Particle Environment of the Earth (Hitch-Hiker I Data Analysis)

Paolini¹,

Theodoridis²,

Bate³

1965

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The zesults of the reduction and analysis of data obtained from instrumentation flown on the Air Force Satellite Hitch-hiker I (1963-25B) are presented. The instrumentation included two electrostatic analyzers (one for electrons, 15 to 100 kev, the other for protons, 15 to 100 key); a scintillation spectrometer (for electrons, 0. 7 to 4. 0 Mev); a phoswich scintillation spectrometer (for protons 1. to 5. Mev and 7. 5 to 120 Mev); and a Geiger counter (electrons greater than 4. Mev, protons greater than 40. Mev). Detailed data on integral energy spectra, pitch angle distributions, and perpendicular unidirectional intensities, as functions of B, L (or X, L) and time are given in five papers appended to this report. No substantial intensities of protons, 15 to 100 key, were observed. Electrons, 15 to 10C key, were observed with intensities as great as 2 x 10 5/cm 2-sec-ster-kev at 40 key, but the anomalous angular distributions obtained cab. doubt on the credibility of these data. Peak Protons in the Radiation Belts. " Paper presented at Forty-sixth Annual Meeting of the American Geophysical Union at Washington,

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Section: Discussionsupporting

confidence: 76%

Section: Discussionmentioning

confidence: 89%

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The Energetic Charged Particle Environment of the Earth (Hitch-Hiker I Data Analysis)

Paolini¹,

Theodoridis²,

Bate³

1965

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“…Since the discovery of the low-energy (•1 Mev) protons by Bame et al [1962] and Davis and Williamson [1963], many measurements have been reported for the spatial distribution, energy spectrums, pitch-angle distributions, etc., particularly in the steady state. (For a recent review see Williams [1970].)…”

mentioning

confidence: 99%

Changes in the distribution of low-energy trapped protons associated with the April 17, 1965, magnetic storm

Burns¹,

Krimigis²

1972

J. Geophys. Res.

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The absolute intensity of geomagnetically trapped protons in the energy ranges 0.52 ≤ Ep ≤ 4.0 Mev and 0.90 ≤ Ep ≤ 1.8 Mev has been measured with the solid‐state proton detector on the University of Iowa low‐altitude (initial apogee 2502 km, perigee 527 km) high‐latitude (inclination 81°) satellite Injun 4 for the period from March 1 to May 31, 1965. A study of the temporal variations of these fluxes associated with the April 17, 1965, magnetic storm (sc 1313 UT April 17, main phase onset ∼0200 UT April 18) shows a general redistribution of these protons for L ≳ 2.5 and all sampled |B| ranges, which persisted for at least 36 days after the storm. The effect of the sudden commencement was a general depression in the intensities and a hardening of the energy spectrums, although the intensities recovered to their prestorm level during the initial phase. The major redistribution was apparently initiated by the polar substorm that began at ∼0620 UT on April 18 and continued long after (to 1100 UT) the substorm had subsided (∼0800 UT). During the recovery phase, a secondary peak developed in the intensity profile at L ∼ 3.5 for 0.52‐Mev protons that had no counterpart at this energy at the equator (L. R. Davis, private communication, 1971). No such peak was observed for 0.9‐Mev protons. The over‐all effect of the storm on the steady‐state distribution was a nonadiabatic one with an increase in intensities at L ≲ 3 and a decrease at L ≳ 3. The loss and/or gain of particles appears to be fractionally the same at all |B| values sampled here. The post‐storm dependence of the spectral parameter E0 on L generally follows the relation E0 ∝ L−3, although the prestorm dependence cannot be described by a simple function at all L values. The appearance of a secondary peak and the behavior of the prestorm and post‐storm spectrums are in qualitative agreement with the predictions of the bimodal diffusion model of Theodoridis et al. [1969], whereby the solar wind is the source of the observed protons.

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Energy Spectrum of Inner Zone Protons

Freden

1966

Astrophysics and Space Science Library

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Protons in the outer zone of the radiation belt

Cited by 20 publications

References 16 publications

The Energetic Charged Particle Environment of the Earth (Hitch-Hiker I Data Analysis)

The Energetic Charged Particle Environment of the Earth (Hitch-Hiker I Data Analysis)

Changes in the distribution of low-energy trapped protons associated with the April 17, 1965, magnetic storm

Energy Spectrum of Inner Zone Protons

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