Discrete classification and electron energy spectra of Titan's varied magnetospheric environment

Rymer, A. M.; Smith, H. T.; Wellbrock, A.; Coates, A. J.; Young, D. T.

doi:10.1029/2009gl039427

Cited by 101 publications

(219 citation statements)

References 26 publications

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“…If the orbit of Titan marks the approximate magnetopause Rymer et al, 2009], then mapping Titan's orbit to the ionosphere very crudely suggests that the aurora itself does mark the open/closed boundary.…”

Section: Discussionmentioning

confidence: 99%

“…Pitch angle distributions of lower-energy electrons (E < 26 keV) have been surveyed using data from the Cassini Plasma Spectrometer (CAPS) [Young et al, 2004]. These electrons exhibited butterfly, pancake, and field-aligned distributions that were interpreted in terms of inward and outward plasma motion driven by the centrifugal interchange instability in combination with azimuthal gradient and curvature drift [Rymer et al, 2009]. A preliminary report on the pitch angle distributions of energetic electrons indicated that magnetospheric electron (bidirectional) beams connect to the expected locations of Saturn's aurora [Saur et al, 2006].…”

Section: Introductionmentioning

confidence: 99%

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Pitch angle distributions of energetic electrons at Saturn

et al. 2011

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[1] Pitch angle distributions of energetic electrons (110-365 keV) at Saturn are statistically analyzed for [2005][2006][2007][2008][2009]. Using a nondipolar model magnetic field, pitch angle distributions are mapped to the magnetospheric equator and sorted by equatorial crossing distance. The results are quantified using a standard function for the pitch angle distribution, f(a) = Asin K a (where a is the pitch angle and K is the power). Inside of ∼10 R S , the distributions are mostly peaked at 90°(K < 0), signifying a trapping distribution. Outside of this distance, the distributions are mostly field aligned (K > 0) with maxima near 0°and 180°. The 10 R S boundary maps to Saturn's ionosphere at latitudes equatorward of the aurora. Very few "flat" distributions are observed (K ≈ 0). The pitch angle distributions are not as well organized in local time as they are in radial distance, but over the 5 year survey between 10 and 20 R S field-aligned distributions appear most often near midnight, while trapping distributions are found elsewhere.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Pitch angle distributions of energetic electrons at Saturn

et al. 2011

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“…The electron impact rates used in this study are based on the CAPS electron fluxes measured during the TA encounter. The electron spectrum during this encounter is classified by Rymer et al (2009) as a plasma sheet encounter. The peak electron energies in this region run between 120-600 eV with the fluxes at the peak energy between 3.5 × 10 5 and 1.2 × 10 6 cm −2 s −1 sr −1 Rymer et al (2009).…”

Section: Discussionmentioning

confidence: 99%

“…The electron spectrum during this encounter is classified by Rymer et al (2009) as a plasma sheet encounter. The peak electron energies in this region run between 120-600 eV with the fluxes at the peak energy between 3.5 × 10 5 and 1.2 × 10 6 cm −2 s −1 sr −1 Rymer et al (2009). Using electron production rates based on the higher end of these ranges would increase the nightside ionospheric densities and hence the ion loss from that region.…”

Section: Discussionmentioning

confidence: 99%

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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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Density waves in Titan's upper atmosphere

Cui

Yelle

et al. 2014

JGR Space Physics

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Analysis of the Cassini Ion Neutral Mass Spectrometer data reveals the omnipresence of density waves in various constituents of Titan's upper atmosphere, with quasi‐periodical structures visible for N2, CH4,29N2, and some of the minor constituents. The N2 amplitude lies in the range of ≈4%–16%with a mean of ≈8%. Compositional variation is clearly seen as a sequence of decreasing amplitude with increasing scale height. The observed vertical variation of amplitude implies significant wave dissipation in different constituents, possibly contributed by molecular viscosity for N2but by both molecular viscosity and binary diffusion for the others. A wave train with near horizontally propagating wave energy and characterized by a wavelength of ≈730 km and a wave period of ≈10 h is found to best reproduce various aspects of the observations in a globally averaged sense. Some horizontal and seasonal trends in wave activity are identified, suggesting a connection between the mechanism driving the overall variability in the background atmosphere and the mechanism driving the waves. No clear association of wave activity with magnetospheric particle precipitation can be identified from the data.

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Discrete classification and electron energy spectra of Titan's varied magnetospheric environment

Cited by 101 publications

References 26 publications

Pitch angle distributions of energetic electrons at Saturn

Pitch angle distributions of energetic electrons at Saturn

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

Density waves in Titan's upper atmosphere

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