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

Author

Chatain, A., Wahlund, J. -E., Shebanits, O., Hadid, L. Z., Morooka, M., Edberg, N. J. T., Guaitella, O., and Carrasco, N.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Physics - Space Physics
Abstract

The ionosphere of Titan hosts a complex ion chemistry leading to the formation of organic dust below 1200 km. Current models cannot fully explain the observed electron temperature in this dusty environment. To achieve new insight, we have re-analyzed the data taken in the ionosphere of Titan by the Cassini Langmuir probe (LP), part of the Radio and Plasma Wave Science package. A first paper (Chatain et al., 2021) introduces the new analysis method and discusses the identification of 4 electron populations produced by different ionization mechanisms. In this second paper, we present a statistical study of the whole LP dataset below 1200 km which gives clues on the origin of the 4 populations. One small population is attributed to photo- or secondary electrons emitted from the surface of the probe boom. A second population is systematically observed, at a constant density (~500 cm-3), and is attributed to background thermalized electrons from the ionization process of precipitating particles fom the surrounding magnetosphere. The two last populations increase in density with pressure, solar illumination and EUV flux. The third population is observed with varying densities at all altitudes and solar zenith angles except on the far nightside (SZA > ~140{\deg}), with a maximum density of 2700 cm-3. It is therefore certainly related to the photo-ionization of the atmospheric molecules. Finally, a fourth population detected only on the dayside and below 1200 km reaching up to 2000 cm-3 could be photo- or thermo-emitted from dust grains., Comment: 25 pages, version accepted for publication in JGR

Published
2021
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2. Re-Analysis of the Cassini RPWS/LP Data in Titan's Ionosphere: 1. Detection of Several Electron Populations

Author

Chatain, A., Wahlund, J. -E., Shebanits, O., Hadid, L. Z., Morooka, M., Edberg, N. J. T., Guaitella, O., and Carrasco, N.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Physics - Space Physics
Abstract

Current models of Titan ionosphere have difficulties in explaining the observed electron density and/or temperature. In order to get new insights, we re-analyzed the data taken in the ionosphere of Titan by the Cassini Langmuir probe (LP), part of the Radio and Plasma Wave Science (RPWS) instrument. This is the first of two papers that present the new analysis method (current paper) and statistics on the whole dataset. We suggest that between 2 and 4 electron populations are necessary to fit the data. Each population is defined by a potential, an electron density and an electron temperature and is easily visualized by a dinstinct peak in the second derivative of the electron current, which is physically related to the electron energy distribution function (Druyvesteyn method). The detected populations vary with solar illumination and altitude. We suggest that the 4 electron populations are due to photo-ionization, magnetospheric particles, dusty plasma and electron emission from the probe boom, respectively., Comment: 34 pages, version accepted for publication in JGR

Published
2021
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3. Titan's variable ionosphere during the T118-T119 Cassini flybys

Author

Edberg, N. J. T., Vigren, E., Snowden, D., Regoli, L. H., Shebanits, O., Wahlund, J. -E., Andrews, D. J., Bertucci, C., and Cui, J.

Subjects
Physics - Space Physics
Abstract

A significant difference in Titan's ionospheric electron density is observed between the T118 and T119 Cassini nightside flybys. These flybys had similar geometry, occurred at the same Saturn local time and while Titan was exposed to similar EUV and ambient magnetic field conditions. Despite these similarities, the RPWS/LP measured density differed a factor of 5 between the passes. This difference was present, and similar, both inbound and outbound. Two distinct electron peaks were present during T118, at 1150 km and 1200 km, suggesting very localised plasma production. During T118, from 1200-1350 km and below 1100 km, the lowest electron density ever observed in Titan's ionosphere are reported. We suggest that an exceptionally low rate of particle impact ionisation in combination with increased dynamics in the ionosphere could be the cause. This is, however, not verified by measurements and the measured ambient high energy particle pressure is in fact higher during T118 than during T119., Comment: 11 pages, 3 figures

Published
2018
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4. Carbon chain anions and the growth of complex organic molecules in Titan's ionosphere

Author

Desai, R. T., Coates, A. J., Wellbrock, A., Vuitton, V., Crary, F. J., González-Caniulef, D., Shebanits, O., Jones, G. H., Lewis, G. R., Waite, J. H., Taylor, S. A., Kataria, D. O., Wahlund, J. -E., Edberg, N. J. T., and Sittler, E. C.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Cassini discovered a plethora of neutral and ionised molecules in Titan's ionosphere including, surprisingly, anions and negatively charged molecules extending up to 13,800 u/q. In this letter we forward model the Cassini electron spectrometer response function to this unexpected ionospheric component to achieve an increased mass resolving capability for negatively charged species observed at Titan altitudes of 950-1300 km. We report on detections consistently centered between 25.8-26.0 u/q and between 49.0-50.1 u/q which are identified as belonging to the carbon chain anions, CN$^-$/C$_3$N$^-$ and/or C$_2$H$^-$/C$_4$H$^-$, in agreement with chemical model predictions. At higher ionospheric altitudes, detections at 73-74 u/q could be attributed to the further carbon chain anions C$_5$N$^-$/C$_6$H$^-$ but at lower altitudes and during further encounters, extend over a higher mass/charge range. This, as well as further intermediary anions detected at $>$100 u, provide the first evidence for efficient anion chemistry in space involving structures other than linear chains. Furthermore, at altitudes below $\sim$1100 km, the low mass anions ($<$150 u/q) were found to deplete at a rate proportional to the growth of the larger molecules, a correlation that indicates the anions are tightly coupled to the growth process. This study adds Titan to an increasing list of astrophysical environments where chain anions have been observed and shows that anion chemistry plays a role in the formation of complex organics within a planetary atmosphere as well as in the interstellar medium., Comment: 8 pages, 3 figures, 1 table, Astrophysical Journal Letter accepted June 01 2017

Published
2017
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8. Ambipolar electrostatic field in dusty plasma – CORRIGENDUM

Author

Hadid, L.Z., primary, Shebanits, O., additional, Wahlund, J.-E., additional, Morooka, M.W., additional, Nagy, A.F., additional, Farrell, W.M., additional, Holmberg, M.K.G., additional, Modolo, R., additional, Persoon, A.M., additional, Tseng, W.L., additional, and Ye, S.-Y., additional

Published
2022
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10. Ambipolar electrostatic field in dusty plasma – ERRATUM

Author

Hadid, L.Z., primary, Shebanits, O., additional, Wahlund, J.-E., additional, Morooka, M.W., additional, Nagy, A.F., additional, Farrell, W.M., additional, Holmberg, M.K.G., additional, Modolo, R., additional, Persoon, A.M., additional, Tseng, W.L., additional, and Ye, S.-Y., additional

Published
2022
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14. Re‐analysis of the Cassini RPWS/LP data in Titan’s ionosphere. Part I: detection of several electron populations

Author

Chatain, Audrey, Wahlund, J.-E., Shebanits, O., Hadid, L., Morooka, M., Edberg, N., Guaitella, O., Carrasco, Nathalie, PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Swedish Institute of Space Physics [Uppsala] (IRF), Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), European Project: 636829,H2020,ERC-2014-STG,PRIMCHEM(2015), and Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS]Physics [physics], [SDU]Sciences of the Universe [physics], Physics::Space Physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; Current models of Titan's ionosphere have difficulties in explaining the observed electron density and/or temperature. In order to get new insights, we re-analyzed the data taken in the ionosphere of Titan by the Cassini Langmuir probe (LP), part of the Radio and Plasma Wave Science (RPWS) instrument. This is the first of two papers that present the new analysis method (current paper) and statistics on the whole dataset. We suggest that between 2 and 4 electron populations are necessary to fit the data. Each population is defined by a potential, an electron density and an electron temperature and is easily visualized by a dinstinct peak in the second derivative of the electron current, which is physically related to the electron energy distribution function (Druyvesteyn method). The detected populations vary with solar illumination and altitude. We suggest that the 4 electron populations are due to photo-ionization, magnetospheric particles, dusty plasma and electron emission from the probe boom, respectively.

Published
2021

16. Saturn's Ionosphere : Electron Density Altitude Profiles and D-Ring Interaction From The Cassini Grand Finale

Author

Hadid, Lina Z, Morooka, Michiko W, Wahlund, Jan-Erik, Persoon, A. M., Andrews, David J., Shebanits, O., Kurth, W. S., Vigren, Erik, Edberg, Niklas J. T., Nagy, A. F., Eriksson, Anders I, Hadid, Lina Z, Morooka, Michiko W, Wahlund, Jan-Erik, Persoon, A. M., Andrews, David J., Shebanits, O., Kurth, W. S., Vigren, Erik, Edberg, Niklas J. T., Nagy, A. F., and Eriksson, Anders I

Abstract

We present the electron density (n(e)) altitude profiles of Saturn's ionosphere at near-equatorial latitudes from all 23 orbits of Cassini's Grand Finale. The data are collected by the Langmuir probe part of the Radio and Plasma Wave Science investigation. A high degree of variability in the electron density profiles is observed. However, organizing them by consecutive altitude ranges revealed clear differences between the southern and northern hemispheres. The n(e) profiles are shown to be more variable and connected to the D-ring below 5,000 km in the southern hemisphere compared to the northern hemisphere. This observed variability is explained to be a consequence of an electrodynamic interaction with the D-ring. Moreover, a density altitude profile is constructed for the northern hemisphere indicating the presence of three different ionospheric layers. Similar properties were observed during Cassini's final plunge, where the main ionospheric peak is crossed at similar to 1,550-km altitude. Plain Language Summary The Cassini Langmuir probe measured directly the uppermost layer of Saturn's atmosphere, the ionosphere, during its Grand Finale. The observations revealed a layered electron density altitude profile with evidence in the southern hemisphere of an electrodynamic type of interaction with the planet innermost D-ring. Moreover, the main peak of the ionosphere is observed for the first time in the final plunge around 1,550 km.

Published
2019
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18. Density Structures, Dynamics, and Seasonal and Solar Cycle Modulations of Saturn's Inner Plasma Disk

Author

Holmberg, M., Shebanits, O., Wahlund, E., Morooka, M., Vigren, E., André, N., Garnier, P., Persoon, A., Genot, V., Gilbert, L., Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Swedish Institute of Space Physics [Uppsala] (IRF), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

International audience; We present statistical results from the Cassini Radio and Plasma Wave Science (RPWS) Langmuir probe measurements recorded during the time interval from orbit 3 (1 February 2005) to 237 (29 June 2016). A new and improved data analysis method to obtain ion density from the Cassini LP measurements is used to study the asymmetries and modulations found in the inner plasma disk of Saturn, between 2.5 and 12 Saturn radii (1 R S = 60, 268 km). The structure of Saturn's plasma disk is mapped, and the plasma density peak, n max , is shown to be located at ∼4.6 R S and not at the main neutral source region at 3.95 R S. The shift in the location of n max is due to that the hot electron impact ionization rate peaks at ∼4.6 R S. Cassini RPWS plasma disk measurements show a solar cycle modulation. However, estimates of the change in ion density due to varying EUV flux is not large enough to describe the detected dependency, which implies that an additional mechanism, still unknown, is also affecting the plasma density in the studied region. We also present a dayside/nightside ion density asymmetry, with nightside densities up to a factor of 2 larger than on the dayside. The largest density difference is found in the radial region 4 to 5 R S. The dynamic variation in ion density increases toward Saturn, indicating an internal origin of the large density variability in the plasma disk rather than being caused by an external source origin in the outer magnetosphere.

Published
2017

20. The Cassini RPWS/LP Observations of Dusty Plasma in the Kronian System

Author

Morooka, M. W., primary, Wahlund, J.-E., additional, Hadid, L., additional, Eriksson, A., additional, Vigren, E., additional, Edberg, N., additional, Andrews, D., additional, Persoon, A. M., additional, Kurth, W. S., additional, Ye, S.-Y., additional, Hospodarsky, G., additional, Gurnett, D. A., additional, Farrell, W., additional, Waite, J. H., additional, Perryman, R. S., additional, Perry, M., additional, and Shebanits, O., additional

Published
2018
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22. Carbon Chain Anions and the Growth of Complex Organic Molecules in Titan’s Ionosphere

Author

Desai, R. T., primary, Coates, A. J., additional, Wellbrock, A., additional, Vuitton, V., additional, Crary, F. J., additional, González-Caniulef, D., additional, Shebanits, O., additional, Jones, G. H., additional, Lewis, G. R., additional, Waite, J. H., additional, Cordiner, M., additional, Taylor, S. A., additional, Kataria, D. O., additional, Wahlund, J.-E., additional, Edberg, N. J. T., additional, and Sittler, E. C., additional

Published
2017
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25. Extreme densities in Titan's ionosphere during the T85 magnetosheath encounter

Author

Edberg, N. J. T., Andrews, David J., Shebanits, O., Ågren, K., Wahlund, J.-E., Opgenoorth, H. J., Roussos, E., Garnier, P., Cravens, T. E., Badman, S. V., Modolo, Ronan, Bertucci, C., Dougherty, M. K., Swedish Institute of Space Physics [Uppsala] (IRF), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Lawrence Kansas], University of Kansas [Lawrence] (KU), Department of Physics and Astronomy [Leicester], University of Leicester, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Instituto de Astronomía y Física del Espacio [Buenos Aires] (IAFE), Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET)-Universidad de Buenos Aires [Buenos Aires] (UBA), Space and Atmospheric Physics Group [London], Blackett Laboratory, Imperial College London-Imperial College London, Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Ionization, IONOSPHERE, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Ciencias Físicas, Magnetosheath, CASSINI, purl.org/becyt/ford/1.3 [https], MAGNETOSHEATH, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Astronomía, purl.org/becyt/ford/1 [https], TITAN, Cassini, Ionosphere, Titan, CIENCIAS NATURALES Y EXACTAS
Abstract

We present Cassini Langmuir probe measurements of the highest electron number densities ever reported from the ionosphere of Titan. The measured density reached 4310 cm−3 during the T85 Titan flyby. This is at least 500 cm−3 higher than ever observed before and at least 50% above the average density for similar solar zenith angles. The peak of the ionospheric density is not reached on this flyby, making the maximum measured density a lower limit. During this flyby, we also report that an impacting coronal mass ejection (CME) leaves Titan in the magnetosheath of Saturn, where it is exposed to shocked solar wind plasma for at least 2 h 45 min. We suggest that the solar wind plasma in the magnetosheath during the CME conditions significantly modifies Titan's ionosphere by an addition of particle impact ionization by precipitating protons. Fil: Edberg, N. J. T.. Swedish Institute of Space Physics; Suecia Fil: Andrews, D. J.. Swedish Institute of Space Physics; Suecia Fil: Shebanits, O.. Swedish Institute of Space Physics; Suecia Fil: Agren, K.. Swedish Institute of Space Physics; Suecia Fil: Wahlund, J. E.. Swedish Institute of Space Physics; Suecia Fil: Opgenoorth, H. J.. Swedish Institute of Space Physics; Suecia Fil: Roussos, E.. Max Planck Institute for Solar System Research; Alemania Fil: Garnier, P.. University of Toulouse; Francia Fil: Cravens, T. E.. University of Kansas; Estados Unidos Fil: Badman, S. V.. University of Leicester; Reino Unido Fil: Modolo, R.. UVSQ/LATMOS-IPSL/CNRS-INSU; Francia Fil: Bertucci, Cesar. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Dougherty, M. K.. Imperial College London; Reino Unido

Published
2013

26. Effects of Saturn's magnetospheric dynamics on Titan's ionosphere

Author

Edberg, N. J. T., primary, Andrews, D. J., additional, Bertucci, C., additional, Gurnett, D. A., additional, Holmberg, M. K. G., additional, Jackman, C. M, additional, Kurth, W. S., additional, Menietti, J. D., additional, Opgenoorth, H. J., additional, Shebanits, O., additional, Vigren, E., additional, and Wahlund, J.‐E., additional

Published
2015
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27. INCREASING POSITIVE ION NUMBER DENSITIES BELOW THE PEAK OF ION-ELECTRON PAIR PRODUCTION IN TITAN'S IONOSPHERE

Author

Vigren, E., Galand, M., Shebanits, O., Wahlund, J. -E, Geppert, Wolf D., Lavvas, P., Vuitton, V., Yelle, R. V., Vigren, E., Galand, M., Shebanits, O., Wahlund, J. -E, Geppert, Wolf D., Lavvas, P., Vuitton, V., and Yelle, R. V.

Abstract

We combine derived ion-electron pair formation rates with Cassini Radio Plasma Wave Science Langmuir Probe measurements of electron and positive ion number densities in Titan's sunlit ionosphere. We show that positive ion number densities in Titan's sunlit ionosphere can increase toward significantly lower altitudes than the peak of ion-electron pair formation despite that the effective ion-electron recombination coefficient increases. This is explained by the increased mixing ratios of negative ions, which are formed by electron attachment to neutrals. While such a process acts as a sink for free electrons, the positive ions become longer-lived as the rate coefficients for ion-anion neutralization reactions are smaller than those for ion-electron dissociative recombination reactions., AuthorCount:8

Published
2014
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29. Extreme densities in Titan's ionosphere during the T85 magnetosheath encounter

Author

T. Edberg, N. J., Andrews, D. J., Shebanits, O., Ågren, K., Wahlund, J.-e., Opgenoorth, H. J., Roussos, E., Garnier, P., Cravens, T. E., Badman, S. V., Modolo, R., Bertucci, C., Dougherty, M. K., T. Edberg, N. J., Andrews, D. J., Shebanits, O., Ågren, K., Wahlund, J.-e., Opgenoorth, H. J., Roussos, E., Garnier, P., Cravens, T. E., Badman, S. V., Modolo, R., Bertucci, C., and Dougherty, M. K.

Abstract

We present Cassini Langmuir probe measurements of the highest electron number densities ever reported from the ionosphere of Titan. The measured density reached 4310 cm−3 during the T85 Titan flyby. This is at least 500 cm−3 higher than ever observed before and at least 50% above the average density for similar solar zenith angles. The peak of the ionospheric density is not reached on this flyby, making the maximum measured density a lower limit. During this flyby, we also report that an impacting coronal mass ejection (CME) leaves Titan in the magnetosheath of Saturn, where it is exposed to shocked solar wind plasma for at least 2 h 45 min. We suggest that the solar wind plasma in the magnetosheath during the CME conditions significantly modifies Titan's ionosphere by an addition of particle impact ionization by precipitating protons.

Published
2013

30. Solar cycle modulation of Titan's ionosphere

Author

Edberg, N. J. T., primary, Andrews, D. J., additional, Shebanits, O., additional, Ågren, K., additional, Wahlund, J.-E., additional, Opgenoorth, H. J., additional, Cravens, T. E., additional, and Girazian, Z., additional

Published
2013
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31. Extreme densities in Titan's ionosphere during the T85 magnetosheath encounter

Author

T. Edberg, N. J., primary, Andrews, D. J., additional, Shebanits, O., additional, Ågren, K., additional, Wahlund, J.‐E., additional, Opgenoorth, H. J., additional, Roussos, E., additional, Garnier, P., additional, Cravens, T. E., additional, Badman, S. V., additional, Modolo, R., additional, Bertucci, C., additional, and Dougherty, M. K., additional

Published
2013
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