Impulsive bursts of relativistic electrons discovered during Ulysses' traversal of Jupiter's dusk-side magnetosphere

McKibben, R. B.; Simpson, J. A.; Zhang, M.

doi:10.1016/0032-0633(93)90108-e

Cited by 67 publications

(78 citation statements)

References 15 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: 88%

“…As relativistic electron bursts proceed more or less sequentially along the boundary zone during one IRB oscillation cycle, COSPIN and URAP could then detect simultaneous bursts of relativistic electrons and radio emissions at a later epoch. This case would explain why QP-40 bursts of relativistic electrons and radio emissions tightly correlate with each other on the whole while some radio burst onsets precede relativistic electron burst onsets by D5È8 minutes4 (MacDowall et al 1993 ;McKibben et al 1993 ;Desch 1994). In the case when Ulysses was at a "" right ÏÏ location to detect the Ðrst batch of relativistic electron bursts from the beginning section of the IRB boundary zone during an IRB oscillation cycle, onsets of relativistic electron and radio bursts would almost coincide ).…”

Section: Physical Consequences Of Global Inner Radiation Belt Oscillamentioning

confidence: 91%

“…In close correlation, the uniÐed radio and plasma wave (URAP) experiment, also onboard the Ulysses spacecraft, recorded radio bursts (frequency kHz) with the same 40 minutes quasi-period (Stone l [ 700 et al 1992 ;MacDowall et al 1993 ;McKibben et al 1993). In the following two years, after the Jovian encounter by the Ulysses spacecraft, thousands of such QP-40 radio bursts had occurred in strong correlation with the recurrent arrival of high-speed solar winds at Jupiter (see Figs.…”

Section: Introductionmentioning

confidence: 94%

“…In this manner, IRB oscillations in response to recurrent highspeed solar wind variations are linked to magnetic polar QP-40 activities. It should be noted that the physical connection between the high-speed solar wind and the QP-40 IRB oscillations may involve primarily MHD wave transmission (there are some evidence of QP-40 magnetic waves ; McKibben et al 1993 andBalogh et al 1992) and may not necessarily involve dramatic and bursty injection type activities (Mauk et al 1999).…”

Section: Physical Consequences Of Global Inner Radiation Belt Oscillamentioning

confidence: 99%

“…During one IRB oscillation cycle, when a sequence of electron bursts along the boundary zone sweeps across Ulysses lengthwise tangentially for a duration of a few minutes, the burst proÐle would be a sharp rise followed by a gradual fallo †. Occasionally, Ulysses may go across the IRB boundary zone widthwise such that recorded relativistic electron burst proÐles would appear spiky (Simpson et al 1992 ;McKibben et al 1993).…”

Section: Physical Consequences Of Global Inner Radiation Belt Oscillamentioning

confidence: 99%

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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: 88%

Section: Physical Consequences Of Global Inner Radiation Belt Oscillamentioning

confidence: 91%

Section: Introductionmentioning

confidence: 94%

Section: Physical Consequences Of Global Inner Radiation Belt Oscillamentioning

confidence: 99%

Section: Physical Consequences Of Global Inner Radiation Belt Oscillamentioning

confidence: 99%

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Magnetoinertial Oscillations of Jupiter’s Inner Radiation Belt

Lou

2001

Astrophysical Journal

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Jupiter's X‐ray and EUV auroras monitored by Chandra, XMM‐Newton, and Hisaki satellite

et al. 2016

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Jupiter's X‐ray auroral emission in the polar cap region results from particles which have undergone strong field‐aligned acceleration into the ionosphere. The origin of precipitating ions and electrons and the time variability in the X‐ray emission are essential to uncover the driving mechanism for the high‐energy acceleration. The magnetospheric location of the source field line where the X‐ray is generated is likely affected by the solar wind variability. However, these essential characteristics are still unknown because the long‐term monitoring of the X‐rays and contemporaneous solar wind variability has not been carried out. In April 2014, the first long‐term multiwavelength monitoring of Jupiter's X‐ray and EUV auroral emissions was made by the Chandra X‐ray Observatory, XMM‐Newton, and Hisaki satellite. We find that the X‐ray count rates are positively correlated with the solar wind velocity and insignificantly with the dynamic pressure. Based on the magnetic field mapping model, a half of the X‐ray auroral region was found to be open to the interplanetary space. The other half of the X‐ray auroral source region is magnetically connected with the prenoon to postdusk sector in the outermost region of the magnetosphere, where the Kelvin‐Helmholtz (KH) instability, magnetopause reconnection, and quasiperiodic particle injection potentially take place. We speculate that the high‐energy auroral acceleration is associated with the KH instability and/or magnetopause reconnection. This association is expected to also occur in many other space plasma environments such as Saturn and other magnetized rotators.

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Dynamics of the flares in the active polar region of Jupiter

Bonfond

Grodent

Gérard

et al. 2016

Geophysical Research Letters

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The duskside of the polar region of Jupiter's UV aurorae, called the active region, sometimes exhibits quasiperiodic (QP) flares on timescales of 2–3 min. Based on Hubble Space Telescope Far‐UV time‐tag images, we show for the first time that the Northern Hemisphere also displays QP flares. The area covered by these flares can reach up to 2.4 × 108 km2 (i.e., the whole active region) but often only involves an area an order of magnitude smaller. Using a magnetic field mapping model, we deduced that these areas correspond to the dayside outer magnetosphere. In our data set, quasiperiodic features are only seen on half of the cases, and even on a given observation, a region can be quiet for one half and blinking on the other half. Consecutive observations in the two hemispheres show that the brightening can occur in phase. Combined with the size and location of the flares, this behavior suggests that the QP flares most likely take place on closed magnetic field lines.

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Impulsive bursts of relativistic electrons discovered during Ulysses' traversal of Jupiter's dusk-side magnetosphere

Cited by 67 publications

References 15 publications

Magnetoinertial Oscillations of Jupiter’s Inner Radiation Belt

Magnetoinertial Oscillations of Jupiter’s Inner Radiation Belt

Jupiter's X‐ray and EUV auroras monitored by Chandra, XMM‐Newton, and Hisaki satellite

Dynamics of the flares in the active polar region of Jupiter

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