Mapping Magnetospheric Equatorial Regions at Saturn from Cassini Prime Mission Observations

Arridge, C. S.; André, Nicolas; McAndrews, H. J.; Bunce, E. J.; Burger, M. H.; Hansen, K. C.; Hsu, Hsiang-Wen; Johnson, R. E.; Jones, G. H.; Kempf, S.; Khurana, K. K.; Krupp, N.; Kurth, W. S.; Leisner, J. S.; Paranicas, C.; Roussos, E.; Russell, C. T.; Schippers, P.; Sittler, E. C.; Smith, H. T.; Thomsen, M. F.; Dougherty, M. K.

doi:10.1007/s11214-011-9850-4

Cited by 43 publications

(37 citation statements)

References 238 publications

(265 reference statements)

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“…Arridge et al 2011c) about Titan's location can also produce strong changes in the charged particle environment in which Titan is embedded, and strong rotations in the convection electric field. The motion of the plasma sheet implies strong changes in the plasma density and hence ram and plasma pressure.…”

Section: Key Processes In the Formation Of Titan's Induced Magnetospherementioning

confidence: 99%

“…In this section we introduce the structure and physics of Saturn's magnetosphere particularly focusing on the region near Titan's orbit at 20.3 R S . For detailed recent reviews of the Saturnian magnetosphere and its configuration we refer the reader to , Gombosi et al (2009) and Arridge et al (2011c). The basic configuration and physics of Saturn's magnetosphere is presented in Sect.…”

Section: Structure and Physics Of Saturn's Magnetosphere Near Titanmentioning

confidence: 99%

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Upstream of Saturn and Titan

et al. 2011

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The formation of Titan's induced magnetosphere is a unique and important example in the solar system of a plasma-moon interaction where the moon has a substantial atmosphere. The field and particle conditions upstream of Titan are important in controlling the interaction and also play a strong role in modulating the chemistry of the ionosphere. In this paper we review Titan's plasma interaction to identify important upstream parameters and review the physics of Saturn's magnetosphere near Titan's orbit to highlight how these upstream parameters may vary. We discuss the conditions upstream of Saturn in the solar wind and the conditions found in Saturn's magnetosheath. Statistical work on Titan's upstream magnetospheric fields and particles are discussed. Finally, various classification schemes are presented and combined into a single list of Cassini Titan encounter classes which is also used to highlight differences between these classification schemes.

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Section: Key Processes In the Formation Of Titan's Induced Magnetospherementioning

confidence: 99%

Section: Structure and Physics Of Saturn's Magnetosphere Near Titanmentioning

confidence: 99%

Upstream of Saturn and Titan

et al. 2011

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“…The former is obtained by integrating the exobase CH 4 EDF over the full momentum space occupied by realistic particle trajectories that cross the exobase with upward velocities, and the latter obtained by integrating the same EDF over a restricted momentum space with kinetic energy greater than the local escape energy. The Chamberlain model used in Section 4 implicitly assumes an ideal Maxwellian for the exobase CH 4 EDF, given by Arridge et al 2011b). Clearly, existing studies predict a wide range of CH 4 escape rates from negligible to several 10 27 s −1 , with the lower limit being compatible with the Chamberlain model presented in Section 4.…”

Section: Implications For Ch 4 Escape From Titanmentioning

confidence: 86%

The Structure of Titan’s N₂ and CH₄ Coronae

Jiang

Cui

2017

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In this study, we analyze the structures of Titan's N 2 and CH 4 coronae using a large data set acquired by the Ion Neutral Mass Spectrometer (INMS) instrument on board Cassini. The N 2 and CH 4 densities measured from the exobase up to 2000km imply a mean exobase temperature of 146K and 143K, respectively, which is lower than the mean upper atmospheric temperature by 4 and 7K. This indicates that on average, Titan possesses a subthermal rather than suprathermal corona. A careful examination reveals that the variability in corona structure is not very likely to be solar driven. Within the framework of the collisionless kinetic model, we investigate how the CH 4 energy distribution near the exobase could be constrained if strong CH 4 escape occurs on Titan. Several functional forms for the CH 4 energy distribution are attempted, assuming two representative CH 4 escape rates of 1.2 10 25 s −1 and2.2 10 27 s −1. We find that the double Maxwellian and power-law distributions can reproduce the shape of the CH 4 corona structure as well as the imposed CH 4 escape rate. In both cases, the escape rate is contributed by a suprathermal CH 4 population on the high-energy tail, with a number fraction below 5% and a characteristic energy of 0.1-0.6eV per suprathermal CH 4 molecule. The coexistence of the subthermal CH 4 corona revealed by the INMS data and substantial CH 4 escape suggested by some previous works could be reconciled by a significant departure in the exobase CH 4 energy distribution from ideal Maxwellian that enhances escape and causes a noticeable redistribution of the corona structure.

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“…At Saturn it has been found that the magnetodisk is bowl-shaped due to the tilt angle of the equatorial plane relative to the ecliptic plane and is a seasonal effect. The magnetodisk and the associated current sheet are also flapping up and down as discussed by Arridge et al (2011) and Volwerk et al (2013). The main transport processes in the magnetosphere like interchange motion and injection events are, very similar to the Jupiter case, continuously present in the Kronian magnetosphere showing the highly dynamic nature of Saturn's magnetosphere Paranicas et al 2010).…”

Section: Middle Magnetosphere and Magnetodiskmentioning

confidence: 90%

“…Characteristic key regions of giant planet magnetospheres are usually subdivided into inner, middle and outer magnetosphere (Bagenal 1992;Arridge et al 2011), whereas the distance of transition between them is widely fluctuating. In both magnetospheres we find strong dipolar intrinsic magnetic fields in the innermost magnetospheres, the region of the radiation belts populated with the high-energy electrons and ions with different origins.…”

Section: Introductionmentioning

confidence: 99%

Giant magnetospheres in our solar system: Jupiter and Saturn compared

Krupp

2014

Astron Astrophys Rev

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We review the current knowledge about the two biggest magnetospheres in our solar system based on the significant progress made with data from the Cassini spacecraft in orbit around Saturn since 2004, and based on the last mission to Jupiter by the Galileo spacecraft between 1995 and 2003. In addition we take into account new observations of the Hubble Space Telescope and other telescopes as well as the latest computer simulation efforts.

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Mapping Magnetospheric Equatorial Regions at Saturn from Cassini Prime Mission Observations

Cited by 43 publications

References 238 publications

Upstream of Saturn and Titan

Upstream of Saturn and Titan

The Structure of Titan’s N₂ and CH₄ Coronae

Giant magnetospheres in our solar system: Jupiter and Saturn compared

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Mapping Magnetospheric Equatorial Regions at Saturn from Cassini Prime Mission Observations

Cited by 43 publications

References 238 publications

Upstream of Saturn and Titan

Upstream of Saturn and Titan

The Structure of Titan’s N2 and CH4 Coronae

Giant magnetospheres in our solar system: Jupiter and Saturn compared

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Product

Resources

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The Structure of Titan’s N₂ and CH₄ Coronae