The global plasma environment of Titan as observed by Cassini Plasma Spectrometer during the first two close encounters with Titan

Szegö, K.

doi:10.1029/2005gl022646

Cited by 37 publications

(36 citation statements)

References 12 publications

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“…We do know that Titan is a significant source of pick-up ions and mass loading [cf. Mitchell et al, 2005;Szego et al, 2005] and has weak Alfvén wings (relative to Jupiter's Io) but an extensive wake [cf. Neubauer et al, 2006;Ma et al, 2006].…”

Section: A08211mentioning

confidence: 99%

Influence of Saturnian moons on Saturn kilometric radiation

et al. 2007

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[1] Similar to past studies at Jupiter, we conduct an investigation of possible associations of radio emission occurrence probability with the orbital phases of Saturnian moons. We use a new definition of the Saturn longitude system (SLS) based on the results of Kurth et al. (2007). This paper presents results of our findings to date, sampling a large portion of the Radio and Plasma Wave Science (RPWS) instrument data over the frequency range 12 kHz < f < 16 MHz. We also investigate the intensity of Saturn kilometric radiation (SKR) as a function of the local time and subsolar longitude. When Titan is near a local time of midnight, there is a significant increase in the occurrence probability of SKR and a diminution of SKR when Titan is near local noon and afternoon. This indicates Titan may play a role in the process of substorm generation at Saturn perhaps due to its large plasma wake. Rhea displays a marginal orbital phase ''control'' of a subset of the SKR. In the past there have been conflicting reports of the absence of SKR emission at particular local times of Dione. We find no long-term, statistical influence of Dione on SKR occurrence probability. In addition, we find no significant statistical influence of Enceladus or Tethys on SKR occurrence probability.

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Section: A08211mentioning

confidence: 99%

Influence of Saturnian moons on Saturn kilometric radiation

et al. 2007

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“…Based on the assumption that the N + component could be pickup ions, Ledvina et al (2005) showed that the PLS data could be fit by a shell distribution. The post Cassini picture has found that the N + component was really O + and is thought to originate from the icy satellites and moons (Szego et al, 2005). Szego et al (2005) fit the incident O + to a shell distribution function.…”

Section: Introductionmentioning

confidence: 99%

“…The post Cassini picture has found that the N + component was really O + and is thought to originate from the icy satellites and moons (Szego et al, 2005). Szego et al (2005) fit the incident O + to a shell distribution function. The Cassini plasma data along Titan's orbit have been fit to Maxwellian, shell and kappa distribution functions.…”

Section: Introductionmentioning

confidence: 99%

The orientation of Titan’s dayside ionosphere and its effects on Titan’s plasma interaction

Ledvina

Brecht²,

Cravens

2012

Earth Planet Sp

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A hybrid particle code has been used to examine how Titan's interaction with Saturn's magnetosphere is effected by the orientation of the dayside ionosphere with respect to the incident magnetospheric flow. The hybrid code self-consistently includes a version of Titan's ionosphere represented by 7 generic ion species, over 40 ionneutral chemical reactions, ion-neutral collisions and Hall and Pederson conductivities. Emphasis is placed on what effects the orientation angle has on the ion loss rates, ion densities, and the electric and magnetic fields. The results are analyzed and regardless of the orientation angle the ionosphere is found to be within photochemical equilibrium below 1200 km altitude. The ion loss rates and field structures also show little dependence on the orientation of the dayside ionosphere. It is found to first order illumination angle does not have a significant effect on these features of the Titan interaction.

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“…Szego et al 2005). However, no significant wave power has been identified close to the moon, counter to intuition.…”

Section: The Region Near Titanmentioning

confidence: 63%

Transport of Mass, Momentum and Energy in Planetary Magnetodisc Regions

Achilleos

André

Blanco‐Cano

et al. 2015

The Magnetodiscs and Aurorae of Giant Planets

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The rapid rotation of the gas giant planets, Jupiter and Saturn, leads to the formation of magnetodisc regions in their magnetospheric environments. In these regions, relatively cold plasma is confined towards the equatorial regions, and the magnetic field generated by the azimuthal (ring) current adds to the planetary dipole, forming radially distended field lines near the equatorial plane. The ensuing force balance in the equatorial magnetodisc is strongly influenced by centrifugal stress and by the thermal pressure of hot ion populations, whose thermal energy is large compared to the magnitude of their centrifugal potential energy. The sources of plasma for the Jovian and Kronian magnetospheres are the respective satellites Io (a volcanic moon) and Enceladus (an icy moon). The plasma produced by these N.

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The global plasma environment of Titan as observed by Cassini Plasma Spectrometer during the first two close encounters with Titan

Cited by 37 publications

References 12 publications

Influence of Saturnian moons on Saturn kilometric radiation

Influence of Saturnian moons on Saturn kilometric radiation

The orientation of Titan’s dayside ionosphere and its effects on Titan’s plasma interaction

Transport of Mass, Momentum and Energy in Planetary Magnetodisc Regions

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