The Juno Mission

Bolton, S. J.; Lunine, Jonathan I.; Stevenson, D. J.; Connerney, J. E. P.; Levin, S. M.; Owen, Tobias; Bagenal, F.; Gautier, D.; Ingersoll, Andrew P.; Orton, Glenn S.; Guillot, T.; Hubbard, W. B.; Bloxham, Jeremy; Coradini, A.; Stephens, S. K.; Mokashi, P.; Thorne, R. M.; Thorpe, Rob

doi:10.1007/s11214-017-0429-6

Cited by 282 publications

(178 citation statements)

References 76 publications

Supporting

Mentioning

178

Contrasting

Order By: Relevance

“…As it cruised through the large-scale magnetopause boundary layer, its instruments measured intense bursts of radio emissions and energetic particles (both electrons and protons), with timescales ranging from 2 to 80 min (Karanikola et al, 2004;MacDowall et al, 1993;McKibben et al, 1993;Zhang et al, 1995). The instrument suite and the polar orbit of the Juno spacecraft are well suited to perform this investigation Bolton et al, 2017;Connerney et al, 2017). At the onset of the electron and proton bursts, the pitch angle distributions were field aligned and monodirectional, with the particles originating from Jupiter's aurora.…”

Section: Introductionmentioning

confidence: 99%

Bar Code Events in the Juno‐UVS Data: Signature ∼10 MeV Electron Microbursts at Jupiter

Bonfond

Gladstone

Grodent

et al. 2018

Geophysical Research Letters

Self Cite

View full text Add to dashboard Cite

One of the most intriguing discoveries of Juno is the quasi‐systematic detection of upgoing electrons above the auroral regions. Here we discuss a by‐product of the most energetic component of this population: a contamination resembling bar codes in the Juno‐UVS images. This pattern is likely caused by bursts of ∼10 MeV electrons penetrating the instrument. These events are mostly detected when Juno's magnetic footprint is located poleward of the main emission relative to the magnetic pole. The signal is not periodic, but the bursts are typically 0.1–1 s apart. They are essentially detected when Juno‐UVS is oriented toward Jupiter, indicating that the signal is due to upgoing electrons. The event detections occur between 1 and 7 Jovian radii above the 1‐bar level, suggesting that the electron acceleration takes place close to Jupiter and is thus both strong and brief.

show abstract

Section: Introductionmentioning

confidence: 99%

Bar Code Events in the Juno‐UVS Data: Signature ∼10 MeV Electron Microbursts at Jupiter

Bonfond

Gladstone

Grodent

et al. 2018

Geophysical Research Letters

Self Cite

View full text Add to dashboard Cite

show abstract

“…An essential question of planetary dynamics and structure is whether these jet motions exist only within the shallow troposphere or extend through the molecular envelope that exists above the deeper dynamo region 3 . Determining the depth of these atmospheric jets is one of the prime directives of the NASA (National Aeronautics and Space Administration) Juno mission, which entered into low-altitude Jovian orbit in August 2016 4 . Despite the long-lived scientific interest in these flows, dominant multiple jets have been problematic in fully three-dimensional (3D) numerical models of convection.…”

mentioning

confidence: 99%

A laboratory model for deep-seated jets on the gas giants

et al. 2017

View full text Add to dashboard Cite

The strong east-west jet flows on the gas giants, Jupiter Azimuthally directed (that is, zonal, east-west) jet flows are one of the dominant characteristics in the surficial cloud features observed on the gas giants, Jupiter and Saturn. An essential question of planetary dynamics and structure is whether these jet motions exist only within the shallow troposphere or extend through the molecular envelope that exists above the deeper dynamo region 3 . Determining the depth of these atmospheric jets is one of the prime directives of the NASA (National Aeronautics and Space Administration) Juno mission, which entered into low-altitude Jovian orbit in August 2016 4 . Despite the long-lived scientific interest in these flows, dominant multiple jets have been problematic in fully three-dimensional (3D) numerical models of convection. In particular, multiple banded flows are not found in the most recent, high-resolution models that couple the molecular envelope to the deeper dynamo region. In these models, magnetic dissipation damps the higher-latitude deep jets out of existence [5][6][7] . Similarly, dissipation has also proved overly important in laboratory experiments carried out to date. Laboratory approaches were analysed in the framework of the shallow-layer model and strong viscous damping by the container boundaries only allows for the formation of weak zonal jets with tenuous instantaneous signatures [8][9][10][11][12][13][14] . Thus, it has yet to be demonstrated, as proposed for the gas giant planets 15 , that deep zonally dominant jet flows can exist in the presence of boundary dissipation.We have developed a new laboratory experimental device that is capable of generating strong zonal jets despite viscous friction on the boundaries (Fig. 1a). The working fluid is water, contained in a 1.37-m-high by 1-m-diameter cylindrical tank. The depth of the fluid layer is h o = 50 cm at rest, and the tank's rotation rate is Ω = 7.85 rad s −1 (75 revolutions per minute). Once equilibrated at Ω, the water's free surface takes the shape of a paraboloid, with the fluid layer depth ranging from h min 20 cm on the axis of rotation to h max 90 cm at the tank's outer radius. This rotating surface shape is analogous to the large-scale curvature of a deep spherical planetary fluid layer 16,17 . In addition, the rotation provides strong Coriolis forces, as exist in planetary settings. Once solid body rotation is reached, a submersible pump situated at the base of the tank is turned on, and small-scale turbulence is injected at the base of the fluid layer. The pump continuously circulates water through a lattice of 32 outlets (4 mm diameter) and 32 inlets (2 mm diameter) arranged on a flat base plate without any axisymmetric features (see the injection pattern in Supplementary Fig. 1a). Typical root-mean-square (r.m.s.) fluctuating velocities are in the range u r.m.s. 1-5 cm s −1 . This small-scale turbulence is analogous to the convective turbulence that exists in deep planetary interiors 18,19 and constitutes an appropriate s...

show abstract

“…The Juno mission (Bolton and The Juno Team, 2012), launched in 2011, is the next step in further exploring the Jovian magnetosphere and the gravitational field, followed by ESA's Juice mission, which is in preparation for launch in 2022 (Grasset et al, 2012). The Juno mission (Bolton and The Juno Team, 2012), launched in 2011, is the next step in further exploring the Jovian magnetosphere and the gravitational field, followed by ESA's Juice mission, which is in preparation for launch in 2022 (Grasset et al, 2012).…”

Section: Exploration Of the Jovian Systemmentioning

confidence: 99%

“…Juno is another example containing significant instrumentation for atmospheric sciences to investigate Jupiter (Bolton and The Juno Team, 2012). Juno is another example containing significant instrumentation for atmospheric sciences to investigate Jupiter (Bolton and The Juno Team, 2012).…”

Section: Atmospheres Exospheres and Ionospheresmentioning

confidence: 99%