Effect of plasma torus density variations on the morphology and brightness of the Io footprint

Payan, Alexia P.; Rajendar, A.; Paty, C. S.; Crary, F. J.

doi:10.1002/2013ja019299

Cited by 4 publications

(3 citation statements)

References 37 publications

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“…On this set of FUV images, the IFP nearly disappears as it crosses the blob before re-emerging outside of it. The model of Payan et al (2014) explains this behavior through a localized increase of the torus density resulting in a stronger trapping of the Alfvén waves within the torus. Another study by Hess et al (2013b ) also agrees that an increased torus density would decrease the wave transmission across the torus boundary.…”

Section: Introductionmentioning

confidence: 99%

Similarity of the Jovian satellite footprints: Spots multiplicity and dynamics

Bonfond

Grodent

Saur

et al. 2017

Icarus

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In the magnetospheres of Jupiter and Saturn, the intense interaction of the satellites Io, Europa, Ganymede and Enceladus with their surrounding plasma environment leaves a signature in the aurora of the planet. Called satellite footprints, these auroral features appear either as a single spot (Europa and Enceladus) or as multiple spots (Io and Ganymede). Moreover, they can be followed by extended trailing tails in the case of Io and Europa, while no tail has been reported for Ganymede and Enceladus, yet. Here we show that all Jovian footprints can be made of several spots. Furthermore, the footprints all experience brightness variations on timescale of 2-3 min. We also demonstrate that the satellite location relative to the plasma sheet is not the only driver for the footprint brightness, but that the plasma environment and the magnetic field strength also play a role. These new findings demonstrate that the Europa and Ganymede footprints are very similar to the Io footprint. As a consequence, the processes expected to take place at Io, such as the bi-directional electron acceleration by Alfvén waves or the partial reflection of these waves on plasma density gradients, can most likely be extended to the other footprints, suggesting that they are indeed universal processes.

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Section: Introductionmentioning

confidence: 99%

Similarity of the Jovian satellite footprints: Spots multiplicity and dynamics

Bonfond

Grodent

Saur

et al. 2017

Icarus

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“…The dispersal of plasma from the IPT into the rest of the magnetosphere is the main process that provides plasma to the rest of Jupiter's magnetosphere. Therefore spatial and temporal variations in the IPT can ultimately affect the distribution and dynamics of plasma throughout Jupiter's entire magnetosphere [Bonfond et al, 2012;Payan et al, 2014].…”

mentioning

confidence: 99%

Radio occultations of the Io plasma torus by Juno are feasible

Phipps

Withers

2017

JGR Space Physics

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The flow of material from Io's volcanoes into the Io plasma torus, out into the magnetosphere, and along field lines into Jupiter's upper atmosphere is not adequately understood. The lack of observations of spatial and temporal variations in the Io plasma torus impedes attempts to understand the system as a whole. Here we propose that radio occultations of the Io plasma torus by the Juno spacecraft can measure plasma densities in the Io plasma torus. We find that the line‐of‐sight column density of plasma in each of the three regions of the Io plasma torus (cold torus, ribbon, and warm torus) can be measured with uncertainties of 10%. We also find that scale heights describing the spatial variation in plasma density in each of these three regions can be measured with similar uncertainties. Such observations will be sufficiently accurate to support system‐scale studies of the flow of plasma through the magnetosphere of Jupiter.

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“…Jovian decametric emission is variable but predictable. The strongest bursts come from the Io-driven sources, which depend on the longitude of Jupiter and orbital phase of Io (Bigg 1964;Payan 2014). In Romero-Wolf et al 2015, it was shown that the Iodriven source is compact enough (Dulk 1970;Carr et al 1970;Lynch et al 1976) to be treated effectively as a point source for the purposes of sounding.…”

mentioning

confidence: 99%

Prospects of passive radio detection of a subsurface ocean on Europa with a lander

Romero-Wolf

Schroeder

Ries

et al. 2016

Planetary and Space Science

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We estimate the sensitivity of a lander-based instrument for the passive radio detection of a subsurface ocean beneath the ice shell of Europa, expected to be between 3 km -30 km thick, using Jupiter's decametric radiation. A passive technique was previously studied for an orbiter. Using passive detection in a lander platform provides a point measurement with significant improvements due to largely reduced losses from surface roughness effects, longer integration times, and diminished dispersion due to ionospheric effects allowing operation at lower frequencies and a wider band. A passive sounder on-board a lander provides a low resource instrument sensitive to subsurface ocean at Europa up to depths of 6.9 km for high loss ice (16 dB/km two-way attenuation rate) and 69 km for pure ice (1.6 dB/km).

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Effect of plasma torus density variations on the morphology and brightness of the Io footprint

Cited by 4 publications

References 37 publications

Similarity of the Jovian satellite footprints: Spots multiplicity and dynamics

Similarity of the Jovian satellite footprints: Spots multiplicity and dynamics

Radio occultations of the Io plasma torus by Juno are feasible

Prospects of passive radio detection of a subsurface ocean on Europa with a lander

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