Ulysses Radio and Plasma Wave Observations in the Jupiter Environment

Stone, R. G.; Pedersen, B. M.; Harvey, C. C.; Canu, P.; Cornilleau‐Wehrlin, N.; Desch, M. D.; Villedary, C. de; Fainberg, J.; Farrell, W. M.; Goetz, K.; Heß, R.; Hoang, S.; Kaiser, M. L.; Kellogg, P. J.; Lecacheux, A.; Lin, N.; MacDowall, R. J.; Manning, Robert M.; Meetre, C. A.; Meyer‐Vernet, N.; Moncuquet, M.; Osherovich, V. A.; Reiner, M. J.; Tekle, A.; Thiessen, J.; Zarka, Philippe

doi:10.1126/science.257.5076.1524

Cited by 100 publications

(64 citation statements)

References 28 publications

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“…Regarding the almost exclusive detection of QP-40 burst activities in the dusk side at high south jovigraphic latitudes during the outbound leg of Ulysses (Simpson et al 1992 ;Stone et al 1992 ;McKibben et al 1993 ;MacDowall et al 1993), we note the following.…”

Section: Discussionmentioning

confidence: 99%

Magnetoinertial Oscillations of Jupiter’s Inner Radiation Belt

Lou

2001

Astrophysical Journal

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Quasi-periodic 40 minute (QP-40) bursts of both relativistic electrons (energy E D 10 MeV) and radio emissions (frequency kHz) from the south Jovian pole were detected by the instrument onboard l [ 700 the Ulysses spacecraft at high jovigraphic latitudes (D30È40 S¡). We show here that JupiterÏs inner radiation belt (IRB) may oscillate globally with a quasi-period of D40 minutes or so and propose that, as results of asymmetries and small-scale circumpolar magnetic irregularities/anomalies, a fraction of relativistic electrons normally trapped within the IRB may go astray from a roughly circular zone surrounding the Jovian magnetic pole during certain phases of such IRB magnetoinertial oscillations. The escaped relativistic electrons rapidly convert their transverse motions to (anti)parallel motions along the magnetic Ðeld lines by the mirror force. The observed QP-40 radio bursts are closely associated with such QP-40 leaks of relativistic electrons in near-antiparallel motions. Our prediction for QP-40 magnetoinertial oscillations of the IRB can be tested by directly observing variations of IRB decimetric brightness using ground-based radio telescopes, especially upon the arrival of high-speed solar winds at Jupiter. Several relevant aspects of this scenario are also discussed.

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Section: Discussionmentioning

confidence: 99%

Magnetoinertial Oscillations of Jupiter’s Inner Radiation Belt

Lou

2001

Astrophysical Journal

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“…The types of waves detected are whistler mode emissions, upper hybrid waves, electrostatic electron cyclotron waves and escaping radio emission. Electromagnetic and electrostatic plasma waves have also been observed in the middle (10-20 R J ) magnetosphere of Jupiter Gurnett et al, 1979Gurnett et al, , 1996Stone et al, 1992). Plasma waves in the middle magnetosphere are not limited to the region around Ganymede.…”

Section: Introductionmentioning

confidence: 71%

The generation of Ganymede's diffuse aurora through pitch angle scattering

2017

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Abstract. Diffuse auroral intensities of neutral atomic oxygen OI λ1356 Å emission on Ganymede due to whistler mode waves are estimated. Pitch angle diffusion of magnetospheric electrons into the loss cone due to resonant wave-particle interaction of whistler mode waves is considered, and the resulting electron precipitation flux is calculated. The analytical yield spectrum approach is used for determining the energy deposition of electrons precipitating into the atmosphere of Ganymede. It is found that the intensities (4-30 R) calculated from the precipitation of magnetospheric electrons observed near Ganymede are inadequate to account for the observational intensities ( ≤ 100 R). This is in agreement with the conclusions reached in previous works. Some acceleration mechanism is required to energize the magnetospheric electrons. In the present work we consider the heating and acceleration of magnetospheric electrons by electrostatic waves. Two particle distribution functions (Maxwellian and kappa distribution) are used to simulate heating and acceleration of electrons. Precipitation of a Maxwellian distribution of electrons can produce about 70 R intensities of OI λ1356 Å emission for electron temperature of 150 eV. A kappa distribution can also yield a diffuse auroral intensity of similar magnitude for a characteristic energy of about 100 eV. The maximum contribution to the estimated intensity results from the dissociative excitation of O 2 . Contributions from the direct excitation of atomic oxygen and cascading in atomic oxygen are estimated to be only about 1 and 2 % of the total calculated intensity, respectively. The findings of this work are relevant for the present JUNO and future JUICE missions to Jupiter. These missions will provide new data on electron densities, electron temperature and whistler mode wave amplitudes in the magnetosphere of Jupiter near Ganymede.

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“…The inputs from the antennas can be combined to synthesize an equivalent dipole tilted with respect to the spin axis. By combining the inputs with suitable phase differences, the polarization of the incoming waves can be determined (Manning and Fainberg, 1980;Stone et al, 1992b). Polarization can only be calculated when the receiver inputs are combined in summation mode (SUM) and when the spacecraft data telemetry rate is high (1024 bps).…”

Section: Ulysses Antennas and Receiversmentioning

confidence: 99%

Jovicentric latitude effect on the HOM radio emission observed by Ulysses/URAP at 5 AU from Jupiter

2002

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Abstract. During 1994 and into 1996, Ulysses was at distances of 5 AU or more from Jupiter and travelling from south to north of the ecliptic plane between jovicentric latitudes −36 • to 20 • . Observations by the Unified Radio and Plasma Experiment (URAP) on board the Ulysses spacecraft during this period have been searched for jovian hectometric (HOM) radio events. At these distances, the HOM was only received occasionally. The signals were generally weak and much care was needed to find and to identify the events.All of the HOM events were observed when Ulysses was at jovicentric latitudes between −12.2 • ≤ D U ly ≤ 14.7 • , relatively close to the plane of the jovicentric equator. Both senses of polarization were observed with left-hand (LH) predominant. The events occurred when the jovimagnetic latitude D φ was between −8.5 • and 14.2 • and suggest that the HOM was only detectable within a beam some 23 • wide, centred on about 3 • jovimagnetic latitude. This is roughly consistent with previous work by Alexander et al. (1979) and by Leblanc (1989, 1991), based upon observations made by Voyager and other spacecraft when these were relatively close to Jupiter. The results are consistent with an emission process due to the Cyclotron-Maser instability, as suggested by a number of scientists in the past.

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Ulysses Radio and Plasma Wave Observations in the Jupiter Environment

Cited by 100 publications

References 28 publications

Magnetoinertial Oscillations of Jupiter’s Inner Radiation Belt

Magnetoinertial Oscillations of Jupiter’s Inner Radiation Belt

The generation of Ganymede's diffuse aurora through pitch angle scattering

Jovicentric latitude effect on the HOM radio emission observed by Ulysses/URAP at 5 AU from Jupiter

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