Energetic Particle Population in the Jovian Magnetosphere: A Preliminary Note

Trainor, J. H.; Teegarden, B. J.; Stilwell, D. E.; McDonald, F. B.; Roelof, E. C.; Webber, W. R.

doi:10.1126/science.183.4122.311

Cited by 48 publications

(9 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Unfortunately, there is no magnetic field data available for the E6 orbit. It is evident from the peaks in the rate profile of Figure 3 that the heavy ions are primarily contained to the magnetic equator, as was also observed by the Pioneer and Ulysses missions [Trainor et al, 1974;Smith et al, 1992]. Thus for the E6 orbit the magnetic equator crossings were determined from the local maxima in the rate profile.…”

mentioning

confidence: 99%

See 1 more Smart Citation

Energetic ion observations in the middle Jovian magnetosphere

Cohen¹,

Stone²,

Selesnick³

2001

J. Geophys. Res.

View full text Add to dashboard Cite

mentioning

confidence: 99%

“…Limited data from Voyager 1, 2 indicate that the composition is similar to that of solar particles [Vogt et al, 1979a[Vogt et al, , 1979b], suggesting a nonmagnetospheric source which enters the magnetosphere at an undetermined location. No spectra have been obtained in this region.…”

mentioning

confidence: 99%

Energetic ion observations in the middle Jovian magnetosphere

Cohen¹,

Stone²,

Selesnick³

2001

J. Geophys. Res.

View full text Add to dashboard Cite

“…To a certain extent, however, most of these difficulties could be corrected for, and thanks in part to the redundancy in energy coverage between the instruments a moderately coherent picture of the inner zone intensities has emerged. (For primary reports on the Pioneer observations, see the work of Fillius and Mcllwain [1974a, b], Fillius et al [1975], Fillius [ 1976], Simpson et al [ 1974aSimpson et al [ , b, 1975, Simpson and McKibben [1976], Trainor et al [1974aTrainor et al [ , b, 1975, McDon-aM and Trainor [ 1976], Van Allen et al [ 1974a, b, 1975], Van Allen [1976, 1977], and Van Allen [1976]. )…”

mentioning

confidence: 99%

Jovian magnetosphere‐Satellite interactions: Aspects of energetic charged particle loss

Thomsen¹

1979

Reviews of Geophysics

View full text Add to dashboard Cite

Observations of energetic charged particles obtained by Pioneers 10 and 11 near the orbits of the inner Jovian satellites are reviewed with particular emphasis on the implications of these observations with regard to possible models of the access of charged particles to the satellite surfaces. The observed effects on particle pitch angle distributions and the observed energy dependence of the intensity depletions seen at the satellite orbits are compared with predictions of satellite sweepup based on several different access models. The two major uncertainties which hamper the comparisons are those associated with the satellite conductivities and the ionospheric dynamo electric field power spectrum. The satellite conductivity is important because it governs the access of the particles to the satellite surface and therefore the lifetime τ; the dynamo power spectrum is important because it controls the magnitude and energy dependence of the radial diffusion coefficient. In spite of these uncertainties we can nevertheless make the following conclusions. (1) The electron pitch angle distributions at Io's orbit are compatible with expectations based on sweeping. (2) The energy dependences of the observed electron depletions at all three inner satellites (Amalthea, Io, and Europa) are incompatible with expectations based on a perfect conductor model of a satellite and its flux tube but are compatible with the energy dependence expected for perfectly insulating or partially conducting satellites; the energy dependences of the proton losses at all three satellites also appear to be compatible with absorption by an insulating or partially conducting satellite but only if certain forms of the dynamo power spectrum are assumed. (3) However, the proton losses at Io are observed to be much stronger than the electron losses, in contradiction to expectations based on sweeping. (4) The most attractive explanation for the proton‐electron discrepancy at Io is that the large proton losses at Io's orbit are principally due to enhanced pitch angle scattering in the region of higher plasma density and probably greater turbulence associated with the satellite rather than to satellite sweeping alone.

show abstract

“…Detailed results specifically addressing the radiation belt s of J u p i t e r a re g iven by Filliu s (1976) , Fillius and Mcllwain ( 1974a, b), Filliu s et al (1975 , McDonald and Trainor (1976) , Mcflwain and Filliu s (1975), Simpson (1974, 1975), Randall (1975) , Sentman and Van Allen (1976) Simpson and McKibben ( 1976), Simpson et al (l974a,b;1975a ,b), Trainor et al ( 1974a ,b; et al ( l974a.b; 1975). Some representative finding s are recounted here.…”

mentioning

confidence: 99%

Jupiter's radiation belts

Schulz

1979

Space Sci Rev

View full text Add to dashboard Cite

Energetic Particle Population in the Jovian Magnetosphere: A Preliminary Note

Cited by 48 publications

References 0 publications

Energetic ion observations in the middle Jovian magnetosphere

Energetic ion observations in the middle Jovian magnetosphere

Jovian magnetosphere‐Satellite interactions: Aspects of energetic charged particle loss

Jupiter's radiation belts

Contact Info

Product

Resources

About