Re‐Analysis of the Cassini RPWS/LP Data in Titan's Ionosphere: 2. Statistics on 57 Flybys

Chatain, Audrey; Wahlund, Jan‐Erik; Shebanits, Oleg; Hadid, Lina; Edberg, Niklas J. T.; Guaitella, Olivier; Carrasco, Nathalie

doi:10.1029/2020ja028413

Cited by 3 publications

(2 citation statements)

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“…In a first paper (this one), we detail the method used for the re‐analysis of the data and the detection of several electron populations. A second paper (Chatain et al., 2021), referred as “paper II,” presents the results obtained for 57 flybys and discusses the origins of the detected electron populations.…”

Section: Introductionmentioning

confidence: 99%

Re‐Analysis of the Cassini RPWS/LP Data in Titan's Ionosphere: 1. Detection of Several Electron Populations

et al. 2021

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Section: Introductionmentioning

confidence: 99%

Re‐Analysis of the Cassini RPWS/LP Data in Titan's Ionosphere: 1. Detection of Several Electron Populations

et al. 2021

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“…The Cassini MAG provides the in-situ magnetic field strength measurements. Regarding the RPWS/LP derived electron density and temperature, Chatain et al (2021aChatain et al ( , 2021b provides a very detailed analysis of the electron current, showing that in Titan's ionosphere it consists of up to three electron populations as well as secondary electrons emitted from the s/c. However, the main populations have similar properties and their net densities and temperatures are consistent with the earlier estimates of the bulk temperatures and densities by Ågren et al (2009) and Edberg et al (2010Edberg et al ( , 2013aEdberg et al ( , 2018.…”

Section: Datasets and Flyby Coveragementioning

confidence: 99%

Conductivities of Titan's Dusty Ionosphere

et al. 2022

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Titan is immersed in Saturn's magnetosphere (Bertucci et al., 2008;Garnier et al., 2010) and does not have its own magnetic field. Instead, an induced magnetic field is formed around Titan from the interactions with Saturn's magnetosphere (Wahlund et al., 2005), similarly to interactions of Venus and Mars with the solar wind and interplanetary magnetic field (e.g., Bertucci et al., 2011 and references therein). The interaction between Titan and the ambient magnetic field depends to a large degree on Titan's conductive ionosphere. Previously, the electrical properties of Titan's ionosphere were derived using only the ion and electron content (Rosenqvist et al., 2009). In the later years, the data sets have been significantly updated. Most notably, large amounts of charged dust were detected in Titan's ionosphere (Ågren et al., 2012;Coates et al., 2007;Shebanits et al., 2013) and a globally present dusty ion-ion plasma is expected (Shebanits et al., 2016). The charged dust grains in the ionosphere-like plasma of Enceladus plume (Morooka et al., 2011) and in the near-equatorial dusty ionosphere of Saturn (Morooka et al., 2019) were shown to have a profound effect on its electric conductivities by Simon et al. (2011) and Yaroshenko and Lühr (2016), and Shebanits et al. (2020, respectively. In this work we derive the electrical properties of Titan's ionosphere using the full plasma content: electrons, positive ions and negative ions/dust grains and investigate the impact of dusty plasma on an unmagnetized planetary body. The relevant in-situ measurements used here are from the Radio and Plasma Wave Science Langmuir Probe (RPWS/LP, Gurnett et al., 2004), the Ion and Neutral Mass Spectrometer (INMS, Teolis et al., 2015;Waite et al., 2004) and the Cassini Fluxgate Magnetometer (MAG, Dougherty et al., 2004). The data set spans the entire Cassini mission and is representative of a full solar cycle and nearly half Titan year.

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