The source and structure of the jovian radiation belt

Beard, David B.; Luthey, Joe L.

doi:10.1016/0032-0633(73)90066-4

Cited by 2 publications

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“…With due attention to these factors, Luthey [1973] showed that Saturn might have an intense radiation belt without revealing its existence in the observed radio spectrum of the planet. The detailed calculation of the synchrotron emission from a fully realistic radiation belt is a massively complex undertaking Beard and Luthey, 1973;Luthey, 1973;Chang and Davis, 1962;de Pater, 1980de Pater, , 1981a. A much simplified, order-of-magnitude calculation for Saturn is presented here, following the basic principles as reviewed by Ginzburg and Syrovatskii [1965], Westfold [1959], Legg and Westfold [1968], and Rybicki and Lightman [1979].…”

Section: An Estimate Of the Synchrotron Emission From Saturn's Inner mentioning

confidence: 99%

Relativistic electrons in Saturn's inner magnetosphere and an estimate of their synchrotron emission

Allen¹,

Grosskreutz²

1989

J. Geophys. Res.

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Energetic electron data obtained by the University of Iowa instrument during Pioneer 11's two‐way traversal of Saturn's inner magnetosphere in September 1979 are reviewed. There were substantial differences between inbound and outbound observations. It is argued that the inbound data are more likely to represent the time‐stationary state. Adopting these inbound data, we develop a quantitative model for the spatial and spectral distributions of relativistic electrons. The principal features of this model are as follows: (1) The radial dependence of omnidirectional intensity J in the equatorial plane is given by J = k′ exp(−1.05 x)[1 − exp(−6.5 x)] where k′ = 1.28 × 107 (cm² s)−1 and x = (r−2.30) with r the radial distance in units of the planet's radius 60,000 km. This distribution is applicable to the range 2.30 ≤ r ≤ 3.60. (2) The latitudinal dependence of J is derived from observed pitch‐angle distributions. These distributions are reasonably well represented by j(α) = j(90°)sin1.5 α (where j is the unidirectional intensity and α is the pitch angle), if one ignores the relatively small depletion of intensity near α = 90°, such depletion being significant in other contexts. (3) As shown previously, the energy spectrum is a relatively narrow one with characteristic energies E in MeV at various r as follows: 0.69 at 5.0; 1.10 at 4.0; 1.89 at 3.0; 2.62 at 2.5; and 3.05 at 2.30. The synchrotron emission of the entire population of relativistic electrons in Saturn's inner magnetosphere is estimated to be about 1 kW with a spectral maximum at 720 kHz. It is shown that this radiation will be very difficult, if not impossible, to observe, even in the near vicinity of the planet. The paper includes a crude but instructive explication of the truly enormous differences between the synchrotron emissions of the inner magnetospheres of Jupiter and Saturn. Indeed, this comparison was an underlying motive for undertaking the present study.

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Section: An Estimate Of the Synchrotron Emission From Saturn's Inner mentioning

confidence: 99%

Relativistic electrons in Saturn's inner magnetosphere and an estimate of their synchrotron emission

Allen¹,

Grosskreutz²

1989

J. Geophys. Res.

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Planetary magnetospheres

Hill¹,

Michel²

1975

Reviews of Geophysics

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The study of extraterrestrial planetary magnetospheres during the past 4 years has experienced a dramatic growth in the availability of observational data and a concomitant growth in the level of scientific interest comparable to the experience of the early 1960's in the study of earth's magnetosphere. Owing in large part to the success of space probes to our four nearest neighbor planets, the domain of magnetospheric physics has grown from the study of ‘the magnetosphere’ into the study of ‘planetary magnetospheres.’ It has now become possible to identify three rather different categories of planetary magnetospheres: (1) intrinsic slowly rotating magnetospheres, (2) intrinsic rapidly rotating magnetospheres, and (3) induced magnetospheres. By ‘intrinsic’ we mean that the planet possesses a sufficiently strong magnetic field to hold the solar wind off its surface; by ‘induced’ we mean that the planetary field exists mainly by virtue of the solar wind interaction with the planet. The distinction between ‘rapidly rotating’ and ‘slowly rotating’ is a quantitative one, indicating whether or not the structure and dynamics of the magnetosphere are influenced strongly by the rotational energy of the magnetospheric plasma. Thus although corotation in earth's magnetosphere is a well‐documented fact, this rotation is sufficiently slow that it can be safely ignored in most considerations of the overall dynamics of the magnetosphere, so that earth's magnetosphere is slowly rotating by the above definition.

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The source and structure of the jovian radiation belt

Cited by 2 publications

References 4 publications

Relativistic electrons in Saturn's inner magnetosphere and an estimate of their synchrotron emission

Relativistic electrons in Saturn's inner magnetosphere and an estimate of their synchrotron emission

Planetary magnetospheres

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