Modeling the Jovian current sheet and inner magnetosphere

Connerney, J. E. P.; Acuña, M. H.; Ness, N. F.

doi:10.1029/ja086ia10p08370

Cited by 399 publications

(472 citation statements)

References 31 publications

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“…[2] Bagenal, F., Adriani, A., Allegrini, F., et al (2013) [10] Connerney, J.E.P., Açuna, M.H. & Ness, N.F.…”

Section: B|[nt]) the Radio Emissions Inmentioning

confidence: 99%

“…The weakness of the magnetic field-aligned electric currents associated with the main aurora, and the broadly distributed nature of electron beaming in the polar caps, suggest a radically different conceptual model of Jupiter's interaction with its space environment. The (precipitating) energetic particles associated with Jovian aurora are very different from the peaked energy distributions that power the most intense auroral emissions at Earth.References and Notes:[1] Bolton, S. J., Adriani, A., Adumitroaie, V., et al (2017) Jupiter's interior and deep atmosphere: the first pole-to-pole pass with the Juno spacecraft, Science, this issue.[2] Bagenal, F., Adriani, A., Allegrini, F., et al (2013) [10] Connerney, J.E.P., Açuna, M.H. & Ness, N.F.…”

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confidence: 99%

“…The variation in magnetic field magnitude throughout most of the 10-day interval centered on closest approach to Jupiter (1.06 Rj) at 12:53 UT is well understood based upon prior knowledge of the planetary magnetic field [8] and that of the Jovian magnetodisc [10], a system of azimuthal currents flowing in a washer-shaped disc within a few Rj of the magnetic equator. Upon approach (DOY 235-237), precipitous decreases in the observed magnetic field magnitude result from Juno's traversal of the magnetic equator where magnetodisc currents effectively nullify the internal field.…”

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Jupiter’s magnetosphere and aurorae observed by the Juno spacecraft during its first polar orbits

Connerney

Adriani

Allegrini

et al. 2017

Science

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151

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Published in: ScienceLink to article, DOI: 10.1126/science.aam5928 Publication date: 2017 Document VersionPeer reviewed version Link back to DTU Orbit Citation (APA): Connerney, J. E. P., Adriani, A., Allegrini, F., Bagenal, F., Bolton, S. J., Bonfond, B., ... Waite, J. (2017). Jupiter's magnetosphere and aurorae observed by the Juno spacecraft during its first polar orbits. Science, 356(6340) Abstract:The Juno spacecraft acquired direct observations of the Jovian magnetosphere and auroral emissions from a vantage point above the poles. Juno's capture orbit spanned the Jovian magnetosphere from bow shock to the planet, providing magnetic field, charged particle, and wave phenomena context for Juno's passage over the poles and traverse of Jupiter's hazardous inner radiation belts. Juno's energetic particle and plasma detectors measured electrons precipitating in the polar regions, exciting intense aurorae, observed simultaneously by the ultraviolet and infrared imaging spectrographs. Juno transited beneath the most intense parts of the radiation belts, passed ~4,000 kilometers above the cloudtops at closest approach, well inside the Jovian rings, and recorded the electrical signatures of high velocity impacts with small particles as it traversed the equator.One Sentence Summary: Juno's instruments provide complete polar maps of Jovian UV aurorae, spatially resolved images of the IR southern aurorae, and in-situ direct measurements of precipitating charged particle populations exciting the aurora. only one bow shock upon approach suggests that the magnetosphere was expanding in size, a conclusion bolstered by the multiple BS encounters experienced outbound during the 53.5 day capture orbit at radial distances of 92-112 Rj before apojove on DOY 213 (~113 Rj), and at distances of 102-108 Rj thereafter . Apojove during the 53.5day orbits occurred at a radial distance of ~113 Rj, so Juno resides at distances of >92 Rj for little more than half of its orbital period (~29 days). Thus on the first two orbits, Juno encountered the MP boundary a great many times at radial distances of ~81-113 Rj.Juno's traverse through the well-ordered portion of the Jovian magnetosphere is illustrated in The magnetic field observed in the previously unexplored region close to the planet (radius<1.3Rj) was dramatically different from that predicted by existing spherical harmonic models, revealing a planetary magnetic field rich in spatial variation, possibly due to a relatively large dynamo radius [1]. Perhaps the most perplexing observation was one that was missing: the expected magnetic signature of intense field aligned currents (Birkeland currents) associated with the main aurora. We did not identify large magnetic perturbations associated with Juno's traverse of field lines rooted in the main auroral oval (supplementary material).Juno's Waves instrument made observations of radio and plasma wave phenomena throughout the first perijove ( Figure 2). These observations were obtained at low altitudes whilst crossing magnetic field lines...

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“…[2] Bagenal, F., Adriani, A., Allegrini, F., et al (2013) [10] Connerney, J.E.P., Açuna, M.H. & Ness, N.F.…”

Section: B|[nt]) the Radio Emissions Inmentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

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Jupiter’s magnetosphere and aurorae observed by the Juno spacecraft during its first polar orbits

Connerney

Adriani

Allegrini

et al. 2017

Science

Self Cite

124

151

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“…We use topologically similar current sheet magnetic models which have been develope--o to fit Voyager observations at Jupiter [Connerney et al, 1981a] and Saturn CConnerney et al, 19 F ' ,J . In each instance the magnetic field consists of a contribution arising from processes internal to the planet plus the field of a current flowing azimuthally in a planet-centered cylindrical coordinate system with its z-axis aligned with the planetary dipole.…”

Section: Magnetic Modelsmentioning

confidence: 99%

Charged particle motions in the distended magnetospheres of Jupiter and Saturn

Birmingham¹

1982

J. Geophys. Res.

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Charged particle motion in the guiding center approximation is analyzed for models of the Jovian and Saturnian magnetospheric magnetic fields based on Voyager magnetometer observations. Field lines are traced and shown to exhibit the previously recognized (Connerney et al., 1981a, b) distention that arises from azimuthally circulating magnetospheric currents. The spatial dependencies of the guiding center bounce period and azimuthal drift rate are investigated for the model fields. The bounce period may be shorter or longer by a factor of 1–3 than in the field of the planetary dipole alone depending on whether a particle mirrors close to the magnetic equator and experiences predominantly an enhanced mirror force or at high latitude and is affected principally by the extended length of the field line. Nondipolar effects in the gradient‐curvature drift rate are most important at the equator and affect particles with all mirror latitudes. The effect is a factor of 10–15 for Jupiter with its strong magnetodisc current and 1–2 for Saturn with its more moderate ring current. Limits of adiabaticity are discussed and are shown to occur at quite modest kinetic energies for protons and heavier ions.

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“…In Figure 11 we show a model of the Jovian magnetic field (Connerney et al, 1981) and the trajectory of Ulysses in magnetic coordinates, during its flyby of the planet. The Z axis denotes the distance along the magnetic dipole axis, while the X axis shows the distance perpendicular to the Z axis.…”

Section: Resultsmentioning

confidence: 99%

The large-scale energetic ion layer in the high latitude Jovian magnetosphere as revealed by ULYSSES/HI-SCALE cross-field intensity-gradient measurements

Anagnostopoulos

Karanikola

Marhavilas

et al. 2012

Planetary and Space Science

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Abstract. Ulysses investigated the high latitude Jovian magnetosphere for a second time, afterPioneer 11 mission, and gave us the opportunity to search the structure and the dynamics of this giant magnetosphere above the magnetodisc. Kivelson (1976) and Kennel and Coroniti (1979) reported that Pioneer 11 observed energetic particle intensities at high latitudes at the same level with those measured in the plasma sheet and inferred that they were not consistent with the magnetodisc model. Ulysses observations supported the idea about a large-scale layer of energetic ions and electrons in the outer high latitude Jovian magnetosphere Anagnostopoulos et al., 2001). This study perform a number of further tests for the existence of the large scale layer of energetic ions in the outer high latitude Jovian magnetosphere by studying appropriate cross-B field anisotropies in order to monitor the ion northward/southward intensity gradients. In particular, we examined Ulysses/HI-SCALE observations of energetic ions with large gyro-radius (0.5-1.6 MeV protons and >2.5 MeV heavy (Z>5) ions) in order to compare instant intensity changes with remote sensing intensity gradients. Our analysis confirms the existence of an energetic particle layer in the north hemisphere, during the inbound trajectory of Ulysses traveling at moderate latitudes, and in the south high-latitude duskside magnetosphere, during the outbound segment of the spacecraft trajectory. Our Ulysses/HI-SCALE data analysis also provides evidence for the detection of an energetic proton magnetopause boundary layer during the outbound trajectory of the spacecraft. During Ulysses flyby of Jupiter the almost permanent appearance of alternative northward and southward intensity gradients suggests that the high latitude layer appeared to be a third major area of energetic particles, which coexisted with the radiation belts and the magnetodisc.

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Modeling the Jovian current sheet and inner magnetosphere

Cited by 399 publications

References 31 publications

Jupiter’s magnetosphere and aurorae observed by the Juno spacecraft during its first polar orbits

Jupiter’s magnetosphere and aurorae observed by the Juno spacecraft during its first polar orbits

Charged particle motions in the distended magnetospheres of Jupiter and Saturn

The large-scale energetic ion layer in the high latitude Jovian magnetosphere as revealed by ULYSSES/HI-SCALE cross-field intensity-gradient measurements

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