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1. Energetic Neutral Atoms From Jupiter's Polar Regions

Author: Fran Bagenal, Edmond C. Roelof, Frederic Allegrini, Barry Mauk, John E. P. Connerney, Scott Bolton, Abigail Rymer, Donald G. Mitchell, Dennis Haggerty, George Clark, Chris Paranicas, G. R. Gladstone, and Peter Kollmann
Subjects: Physics, Jupiter, Geophysics, Energetic neutral atom, Space and Planetary Science, Polar, Magnetosphere, Astrophysics
Published: 2020

2. Ice giant magnetospheres

Author: Chris S. Arridge, Robert Ebert, Ian J. Cohen, Gina A. DiBraccio, Abigail Rymer, and Carol Paty
Subjects: Physics, Solar System, Astrophysics::High Energy Astrophysical Phenomena, General Mathematics, General Engineering, Uranus, General Physics and Astronomy, Astronomy, Magnetosphere, Exoplanet, Planetary science, Neptune, Planet, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Ice giant
Abstract: The ice giant planets provide some of the most interesting natural laboratories for studying the influence of large obliquities, rapid rotation, highly asymmetric magnetic fields and wide-ranging Alfvénic and sonic Mach numbers on magnetospheric processes. The geometries of the solar wind–magnetosphere interaction at the ice giants vary dramatically on diurnal timescales due to the large tilt of the magnetic axis relative to each planet's rotational axis and the apparent off-centred nature of the magnetic field. There is also a seasonal effect on this interaction geometry due to the large obliquity of each planet (especially Uranus). Within situobservations at Uranus and Neptune limited to a single encounter by the Voyager 2 spacecraft, a growing number of analytical and numerical models have been put forward to characterize these unique magnetospheres and test hypotheses related to the magnetic structures and the distribution of plasma observed. Yet many questions regarding magnetospheric structure and dynamics, magnetospheric coupling to the ionosphere and atmosphere, and potential interactions with orbiting satellites remain unanswered. Continuing to study and explore ice giant magnetospheres is important for comparative planetology as they represent critical benchmarks on a broad spectrum of planetary magnetospheric interactions, and provide insight beyond the scope of our own Solar System with implications for exoplanet magnetospheres and magnetic reversals.This article is part of a discussion meeting issue ‘Future exploration of ice giant systems'.
Published: 2020

3. Heavy Ion Charge States in Jupiter's Polar Magnetosphere Inferred From Auroral Megavolt Electric Potentials

Author: S. J. Houston, Scott Bolton, Robert Allen, Ian J. Cohen, Abigail Rymer, Joseph Westlake, S. T. Bingham, Robert Ebert, George Clark, Dennis Haggerty, Fran Bagenal, William F. Dunn, Elias Roussos, C. M. Jackman, Barry Mauk, Peter Kollmann, and Chris Paranicas
Subjects: Jupiter, Physics, Geophysics, Space and Planetary Science, Magnetosphere, Polar, Charge (physics), Heavy ion, Atomic physics
Published: 2020

4. Juno Energetic Neutral Atom (ENA) Remote Measurements of Magnetospheric Injection Dynamics in Jupiter's Io Torus Regions

Author: Frederic Allegrini, George Clark, Donald G. Mitchell, Barry Mauk, Chris Paranicas, Scott Bolton, John E. P. Connerney, Abigail Rymer, Peter Kollmann, Dennis Haggerty, and Fran Bagenal
Subjects: Physics, Jupiter, Geophysics, Energetic neutral atom, Space and Planetary Science, Dynamics (mechanics), Magnetosphere, Torus, Astrophysics
Published: 2020

5. Energetic Particles and Acceleration Regions Over Jupiter's Polar Cap and Main Aurora: A Broad Overview

Author: G. R. Gladstone, Scott Bolton, Fran Bagenal, Abigail Rymer, John E. P. Connerney, Stavros Kotsiaros, Dennis Haggerty, Bertrand Bonfond, Peter Kollmann, Robert Ebert, George Clark, Steve Levin, Barry Mauk, William S. Kurth, Alberto Adriani, Chris Paranicas, and Frederic Allegrini
Subjects: Jupiter, Physics, Particle acceleration, Acceleration, Geophysics, Space and Planetary Science, Magnetosphere, Astronomy, Polar cap
Published: 2020

6. Diverse Electron and Ion Acceleration Characteristics Observed Over Jupiter's Main Aurora

Author: G. R. Gladstone, John E. P. Connerney, Robert Ebert, George Clark, Peter Kollmann, Steven Levin, Alberto Adriani, Frederic Allegrini, P. W. Valek, D. A. Ranquist, J. M. Peachey, Barry Mauk, William S. Kurth, D. J. McComas, Bertrand Bonfond, Scott Bolton, Chris Paranicas, Abigail Rymer, Dennis Haggerty, and Fran Bagenal
Subjects: Jupiter, Physics, Geophysics, 010504 meteorology & atmospheric sciences, 0103 physical sciences, General Earth and Planetary Sciences, Magnetosphere, Electron, Astrophysics, Ion acceleration, 010303 astronomy & astrophysics, 01 natural sciences, 0105 earth and related environmental sciences
Published: 2018

7. Energetic particle signatures of magnetic field-aligned potentials over Jupiter's polar regions

Author: Philip W Valek, George Clark, Steven Levin, Dennis Haggerty, Robert Ebert, Fran Bagenal, Chris Paranicas, Frederic Allegrini, Barry Mauk, William S. Kurth, Scott Bolton, John E. P. Connerney, G. Provan, Joachim Saur, Abigail Rymer, Emma J. Bunce, Stavros Kotsiaros, Stanley W. H. Cowley, Donald G. Mitchell, D. J. McComas, and Peter Kollmann
Subjects: Physics, 010504 meteorology & atmospheric sciences, Magnetosphere, Astronomy, Electron, 01 natural sciences, Magnetic field, Jupiter, Geophysics, Planet, Electric field, Physics::Space Physics, 0103 physical sciences, General Earth and Planetary Sciences, Astrophysics::Earth and Planetary Astrophysics, Electric potential, Ionosphere, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: Recent results of the first ever orbit through Jupiter's auroral region by NASA's Juno spacecraft did not show evidence of coherent acceleration in the auroral or polar region. However, in this letter, we show energetic particle data from Juno's Jupiter Energetic-particle Detector Instrument instrument during the third auroral pass that exhibits conclusive evidence of downward parallel electric fields in portions of Jupiter's polar region. The energetic particle distributions show inverted-V ion and electron structures in a downward electric current region with accelerated peaked distributions in hundreds of keV to ~1 MeV range. The origin of these large electric potential structures is investigated and discussed within the current theoretical framework of current-voltage relationships at both Earth and Jupiter. Parallel electric fields responsible for accelerating particles to maintain the aurora/magnetospheric circuit appear to be a common phenomenon among strongly magnetized planets with conducting ionospheres; however, their origin and generation mechanisms are subjects of ongoing research.
Published: 2017

8. Juno/JEDI observations of 0.01 to >10 MeV energetic ions in the Jovian auroral regions: Anticipating a source for polar X-ray emission

Author: Dennis Haggerty, Steve Levin, Peter Kollmann, George Clark, Scott Bolton, Abigail Rymer, Barry Mauk, John E. P. Connerney, and Chris Paranicas
Subjects: Physics, 010504 meteorology & atmospheric sciences, Magnetosphere, Astronomy, 01 natural sciences, Jovian, Ion, Atmosphere, Jupiter, Geophysics, Physics::Space Physics, 0103 physical sciences, General Earth and Planetary Sciences, Polar, Astrophysics::Earth and Planetary Astrophysics, Pitch angle, Orbit insertion, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: After a successful orbit insertion, the Juno spacecraft completed its first 53.5-day orbit and entered a very low altitude perijove with the full scientific payload operational for the first time on 27 August 2016. The Jupiter Energetic particle Detector Instrument measured ions and electrons over the auroral regions and through closest approach, with ions measured from ~0.01 to > 10 MeV, depending on species. This report focuses on the composition of the energetic ions observed during the first perijove of the Juno mission. Of particular interest are the ions that precipitate from the magnetosphere onto the polar atmosphere, and ions that are accelerated locally by Jupiter's powerful auroral processes. We report preliminary findings on the spatial variations, species, including energy and pitch angle distributions throughout the prime science region during the first orbit of the Juno mission. The prime motivation for this work was to examine the heavy ions that are thought to be responsible for the observed polar x-rays. JEDI did observe precipitating heavy ions with energies >10 MeV, but for this perijove the intensities were far below those needed to account for previously observed polar x-ray emissions. During this survey we also found an unusual signal of ions between oxygen and sulfur. We include here a report on what appears to be a transitory observation of magnesium, or possibly sodium, at MeV energies through closest approach.
Published: 2017

9. Jovian bow shock and magnetopause encounters by the Juno spacecraft

Author: David J. McComas, Steven Levin, Frederic Allegrini, John E. P. Connerney, Scott Bolton, Robert Ebert, Abigail Rymer, George Clark, Chris Paranicas, P. W. Valek, William S. Kurth, George Hospodarsky, and Dennis Haggerty
Subjects: Physics, 010504 meteorology & atmospheric sciences, Astronomy, Magnetosphere, Geophysics, Bow shocks in astrophysics, 01 natural sciences, Jovian, Jupiter, Orbit, Solar wind, Local time, 0103 physical sciences, General Earth and Planetary Sciences, Magnetopause, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: The Juno spacecraft has crossed Jupiter's bow shock (BS) and magnetopause (MP) multiple times in the dawn sector (near 0600 local time), both during the approach to Jupiter and during the first three apojove periods. A survey of all of these crossings using the Juno field and particle instruments has been performed, with 51 bow shock and 97 magnetopause crossings being detected. The BS crossings ranged from 92 to 128 RJ with 1 encounter during the approach, 36 during the first apojove period, 0 on the second, and 14 during the third. The MP crossings ranged from 73 to 114 RJ, with 8 MP encounters during the approach, 40 encounters during the first apojove period, 24 encounters on the second, and 46 during the third. During the approach, Juno initially encountered an expanding magnetosphere resulting in a single BS and MP crossing, followed a few days later by a contracting magnetosphere, resulting in 7 more MP crossings and a BS crossing on the first outbound orbit at 92 RJ. The lack of BS crossings and the limited number of MP crossings during the second apojove period suggests a long period of an expanded magnetosphere, likely caused by a prolonged period of low solar wind dynamic pressure associated with a rarefaction region. The detection of BS crossings on the third apojove period suggests another period of a highly compressed magnetosphere.
Published: 2017

10. Juno observations of energetic charged particles over Jupiter's polar regions: Analysis of monodirectional and bidirectional electron beams

Author: G. R. Gladstone, Phil Valek, John E. P. Connerney, Alberto Adriani, Scott Bolton, Abigail Rymer, Jamey Szalay, Fran Bagenal, George Clark, William S. Kurth, Steven Levin, Barry Mauk, David J. McComas, Frederic Allegrini, Dennis Haggerty, Chris Paranicas, Donald G. Mitchell, Peter Kollmann, and D. A. Ranquist
Subjects: Physics, 010504 meteorology & atmospheric sciences, Detector, Astronomy, Magnetosphere, Astrophysics, Electron, 01 natural sciences, Spectral line, Charged particle, Jupiter, Geophysics, Physics::Space Physics, 0103 physical sciences, General Earth and Planetary Sciences, Polar, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Space environment
Abstract: Juno obtained unique low-altitude space environment measurements over Jupiter's poles on 27 August 2016. Here Jupiter Energetic-particle Detector Instrument observations are presented for electrons (25–800 keV) and protons (10–1500 keV). We analyze magnetic field-aligned electron angular beams over expected auroral regions that were sometimes symmetric (bidirectional) but more often strongly asymmetric. Included are variable but surprisingly persistent upward, monodirectional electron angular beams emerging from what we term the “polar cap,” poleward of the nominal auroral ovals. The energy spectra of all beams were monotonic and hard (not structured in energy), showing power law-like distributions often extending beyond ~800 keV. Given highly variable downward energy fluxes (below 1 RJ altitudes within the loss cone) as high as 280 mW/m2, we suggest that mechanisms generating these beams are among the primary processes generating Jupiter's uniquely intense auroral emissions, distinct from what is typically observed at Earth.
Published: 2017

11. A radiation belt of energetic protons located between Saturn and its rings

Author: Barry Mauk, Iannis Dandouras, Matthew E. Hill, Leonardo Regoli, J. F. Carbary, Peter Kollmann, Benjamin Palmaerts, Geraint H. Jones, A. Kotova, K. Dialynas, Donald G. Mitchell, Abigail Rymer, D. C. Hamilton, Edmond C. Roelof, Nick Sergis, Elias Roussos, Norbert Krupp, Howard Smith, Chris Paranicas, Pontus Brandt, Stamatios M. Krimigis, Stefano Livi, S. P. Christon, W-H. Ip, Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Centre d'étude spatiale des rayonnements (CESR), 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), Institute of Astronomy [Taiwan] (IANCU), National Central University [Taiwan] (NCU), Office for Space Research and Applications [Athens], Academy of Athens, Max-Planck-Institut für Sonnensystemforschung (MPS), Max Planck Institute for Solar System Research (MPS), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées
Subjects: Physics, Multidisciplinary, 010504 meteorology & atmospheric sciences, Proton, Astronomy, Magnetosphere, Cosmic ray, 01 natural sciences, Charged particle, Atmosphere, symbols.namesake, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, 13. Climate action, Planet, [SDU]Sciences of the Universe [physics], Saturn, Van Allen radiation belt, 0103 physical sciences, symbols, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract: Cassini's final phase of exploration The Cassini spacecraft spent 13 years orbiting Saturn; as it ran low on fuel, the trajectory was changed to sample regions it had not yet visited. A series of orbits close to the rings was followed by a Grand Finale orbit, which took the spacecraft through the gap between Saturn and its rings before the spacecraft was destroyed when it entered the planet's upper atmosphere. Six papers in this issue report results from these final phases of the Cassini mission. Dougherty et al. measured the magnetic field close to Saturn, which implies a complex multilayer dynamo process inside the planet. Roussos et al. detected an additional radiation belt trapped within the rings, sustained by the radioactive decay of free neutrons. Lamy et al. present plasma measurements taken as Cassini flew through regions emitting kilometric radiation, connected to the planet's aurorae. Hsu et al. determined the composition of large, solid dust particles falling from the rings into the planet, whereas Mitchell et al. investigated the smaller dust nanograins and show how they interact with the planet's upper atmosphere. Finally, Waite et al. identified molecules in the infalling material and directly measured the composition of Saturn's atmosphere. Science , this issue p. eaat5434 , p. eaat1962 , p. eaat2027 , p. eaat3185 , p. eaat2236 , p. eaat2382
Published: 2018

12. Local Time Asymmetries in Saturn's Magnetosphere

Author: Abigail Rymer, J. F. Carbary, Norbert Krupp, Doug Hamilton, Sarah V. Badman, Stamatios M. Krimigis, and Donald G. Mitchell
Subjects: Physics, Energetic neutral atom, Local time, Saturn, Magnetosphere of Saturn, Physics::Space Physics, Astronomy, Magnetosphere, Astrophysics::Earth and Planetary Astrophysics, Icy moon, Enceladus, Saturn's hexagon, Physics::Geophysics
Abstract: The Cassini orbiter has observed the magnetosphere of Saturn in situ from July 2004 to the present. The spacecraft has visited nearly all local times and a large range of latitudes, including both northern and southern hemispheres, for a large fraction of a Saturn year (=29 Earth years). Local time asymmetries have been observed in the thermal plasma, the energetic particles, energetic neutral atoms, magnetic fields and aurora. Some of these are dawn-to-dusk asymmetries and have Earth-like analogies. Unlike Earth’s magnetosphere, however, Saturn’s magnetosphere is rotationally dominated, has no observable tilt relative to the spin axis, and has a major internal plasma and neutrals source in the icy moon Enceladus. These factors contribute to a number of local time asymmetries that are not dawn-to-dusk. This paper reviews Saturn’s local time asymmetries in charged particles, magnetic fields, and energetic neutral atoms, showing how some are Earth-like and some are not.
Published: 2017

13. An empirical model for the plasma environment along Titan's orbit based on Cassini plasma observations

Author: H. Todd Smith and Abigail Rymer
Subjects: Physics, Astronomy, Magnetosphere, Torus, Plasma, Astrobiology, symbols.namesake, Geophysics, Gas torus, Space and Planetary Science, Local time, symbols, Atmosphere of Titan, Enceladus, Titan (rocket family)
Abstract: Prior to Cassini's arrival at Saturn, the nitrogen-rich dense atmosphere of Titan was considered as a significant, if not dominant, source of heavy ions in Saturn's magnetosphere. While nitrogen was detected in Saturn's magnetosphere based on Cassini observations, Enceladus instead of Titan appears to be the primary source. However, it is difficult to imagine that Titan's dense atmosphere is not a source of nitrogen. In this paper, we apply the Rymer et al.'s (2009) Titan plasma environment categorization model to the plasma environment along Titan's orbit when Titan is not present. We next categorize the Titan encounters that occurred since Rymer et al. (2009). We also produce an empirical model for applying the probabilistic occurrence of each plasma environment as a function of Saturn local time (SLT). Finally, we summarized the electron energy spectra in order to allow one to calculate more accurate electron-impact interaction rates for each plasma environment category. The combination of this full categorization versus SLT and empirical model for the electron spectrum is critical for understanding the magnetospheric plasma and will allow for more accurate modeling of the Titan plasma torus.
Published: 2014

14. Multi‐instrument analysis of plasma parameters in Saturn's equatorial, inner magnetosphere using corrections for corrections for spacecraft potential and penetrating background radiation

Author: James L. Burch, R. Livi, Jerry Goldstein, Abigail Rymer, F. J. Crary, Donald G. Mitchell, and A. M. Persoon
Subjects: Physics, Electron spectrometer, Spectrometer, Spacecraft, Plasma parameters, business.industry, Waves in plasmas, Magnetosphere, Geophysics, Computational physics, Spacecraft charging, Space and Planetary Science, Magnetosphere of Saturn, Physics::Space Physics, business
Abstract: We use a forward modeling program to derive one-dimensional isotropic plasma characteristics in Saturn's inner, equatorial magnetosphere using a novel correction for the spacecraft potential and penetrating background radiation. The advantage of this fitting routine is the simultaneous modeling of plasma data and systematic errors when operating on large data sets, which greatly reduces the computation time and accurately quantifies instrument noise. The data set consists of particle measurements from the electron spectrometer (ELS) and the ion mass spectrometer (IMS), which are part of the Cassini Plasma Spectrometer (CAPS) instrument suite on board the data are limited to peak ion flux measurements within ±10°magnetic latitude and 3–15 geocentric equatorial radial distance (RS). Systematic errors such as spacecraft charging and penetrating background radiation are parameterized individually in the modeling and are automatically addressed during the fitting procedure. The resulting values are in turn used as cross calibration between IMS and ELS, where we show a significant improvement in magnetospheric electron densities and minor changes in the ion characteristics due to the error adjustments. adjustments. Preliminary results show ion and electron densities in close agreement, consistent with charge neutrality throughout Saturn's inner magnetosphere and confirming the spacecraft potential to be a common influence on IMS and ELS. Comparison of derived plasma parameters with results from previous studies using CAPS data and the Radio and Plasma Wave Science investigation yields good agreement.
Published: 2014

15. Saturn's magnetospheric refresh rate

Author: Elena A. Kronberg, Abigail Rymer, D. G. Mitchell, Norbert Krupp, Caitriona M. Jackman, and T. W. Hill
Subjects: Jupiter, Physics, Geophysics, Planet, Magnetosphere of Saturn, Saturn, Giant planet, General Earth and Planetary Sciences, Astronomy, Magnetosphere, Solar maximum, Enceladus
Abstract: [1] A 2–3 day periodicity observed in Jupiter's magnetosphere (superposed on the giant planet's 9.5 h rotation rate) has been associated with a characteristic mass-loading/unloading period at Jupiter. We follow a method derived by Kronberg et al. (2007) and find, consistent with their results, that this period is most likely to fall between 1.5 and 3.9 days. Assuming the same process operates at Saturn, we argue, based on equivalent scales at the two planets, that its period should be 4 to 6 times faster at Saturn and therefore display a period of 8 to 18 h. Applying the method of Kronberg et al. for the mass-loading source rates estimated by Smith et al. (2010) based on data from the third and fifth Cassini-Enceladus encounters, we estimate that the expected magnetospheric refresh rate varies from 8 to 31 h, a range that includes Saturn's rotation rate of ~10.8 h. The magnetospheric period we describe is proportional to the total mass-loading rate in the system. The period is, therefore, faster (1) for increased outgassing from Enceladus, (2) near Saturn solstice (when the highest proportion of the rings is illuminated), and (3) near solar maximum when ionization by solar photons maximizes. We do not claim to explain the few percent jitter in period derived from Saturn Kilometric Radiation with this model, nor do we address the observed difference in period observed in the north and south hemispheres.
Published: 2013

16. The extended Saturnian neutral cloud as revealed by global ENA simulations using Cassini/MIMI measurements

Author: D. C. Hamilton, Pontus Brandt, D. G. Mitchell, Stamatios M. Krimigis, Norbert Krupp, Abigail Rymer, and K. Dialynas
Subjects: Physics, Energetic neutral atom, Spacecraft, Hydrogen, business.industry, chemistry.chemical_element, Magnetosphere, Mass spectrometry, Ion, Computational physics, symbols.namesake, Dipole, Geophysics, chemistry, Space and Planetary Science, Physics::Space Physics, symbols, Atomic physics, business, Titan (rocket family)
Abstract: [1] We show that the neutral gas vertical distribution at Saturn must be ~3–4 times more extended than previously thought for the >5 RSregions, while the neutral H distribution is consistent with H densities that reach up to ~150/cm3close to the orbit of Titan. We utilize a technique to retrieve the global neutral gas distribution in Saturn's magnetosphere, using energetic ion and energetic neutral atom (ENA) measurements, obtained by the Magnetospheric Imaging Instrument (MIMI) onboard the Cassini spacecraft. Our ENA measurements are consistent with a neutral cloud that consists of H2O, OH, H, and O, while the overall shapes and densities numbers concerning the neutral gas distributions are constrained according to already existing models as well as recent observations. The neutral gas distribution at Saturn is determined by simulating a 24–55 keV hydrogen image of the Saturnian magnetosphere, measured by the Ion and Neutral Camera (INCA), averaged over the time period from 1 July 2004 to 23 August 2005. The ionic input of the model includes a proton distribution of combined Charge Energy Mass Spectrometer (CHEMS, 3–230 keV/e), Low Energy Magnetospheric Measurements System (LEMMS, 30.7 keV to 2.3 MeV), and INCA (5–300 keV) in situ measurements. These measurements cover several passes from 1 July 2004 to 10 April 2007, at various local times over the dipole L range 5
Published: 2013

17. The Cassini Enceladus encounters 2005–2010 in the view of energetic electron measurements

Author: D. G. Mitchell, Stamatios M. Krimigis, Geraint H. Jones, Peter Kollmann, Krishan K. Khurana, Thomas P. Armstrong, Norbert Krupp, Chris S. Arridge, Abigail Rymer, Elias Roussos, and Chris Paranicas
Subjects: Physics, Field line, Magnetosphere, Astronomy, Astronomy and Astrophysics, Charged particle, Plume, Enceladus, symbols.namesake, Space and Planetary Science, Saturn, Van Allen radiation belt, Magnetosphere of Saturn, Physics::Space Physics, symbols, Astrophysics::Earth and Planetary Astrophysics, Saturn, Magnetosphere, Saturn, Satellites
Abstract: The moon Enceladus, embedded in Saturn’s radiation belts, is the main internal source of neutral and charged particles in the Kronian magnetosphere. A plume of water ice molecules and dust released through geysers on the south polar region provides enough material to feed the E-ring and also the neutral torus of Saturn and the entire magnetosphere. In the time period 2005–2010 the Cassini spacecraft flew close by the moon 14 times, sometimes as low as 25km above the surface and directly through the plume. For the very first time measurements of plasma and energetic particles inside the plume and its immediate vicinity could be obtained. In this work we summarize the results of energetic electron measurements in the energy range 27keV to 21MeV taken by the Low Energy Magnetospheric Measurement System (LEMMS), part of the Magnetospheric Imaging Instrument (MIMI) onboard Cassini in the vicinity of the moon in combination with measurements of the magnetometer instrument MAG and the Electron Spectrometer ELS of the plasma instrument CAPS onboard the spacecraft. Features in the data can be interpreted as that the spacecraft was connected to the plume material along field lines well before entering the high density region of the plume. Sharp absorption signatures as the result of losses of energetic electrons bouncing along those field lines, through the emitted gas and dust clouds, clearly depend on flyby geometry as well as on measured pitch angle/look direction of the instrument. We found that the depletion signatures during some of the flybys show “ramp-like” features where only a partial depletion has been observed further away from the moon followed by nearly full absorption of electrons closer in. We interpret this as partially/fully connected to the flux tube connecting the moon with Cassini. During at least two of the flybys (with some evidence of one additional encounter) MIMI/LEMMS data are consistent with the presence of dust in energetic electron data when Cassini flew directly through the south polar plume. In addition we found gradients in the magnetic field components which are frequently found to be associated with changes in the MIMI/LEMMS particles intensities. This indicates that complex electron drifts in the vicinity of Enceladus could form forbidden regions for electrons which may appear as intensity drop-outs.
Published: 2012
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18. Upstream of Saturn and Titan

Author: Nick Sergis, Cesar Bertucci, P. Garnier, Andrew J. Coates, Chris S. Arridge, Karoly Szego, Abigail Rymer, Caitriona M. Jackman, Zoltán Németh, Nicolas André, and F. J. Crary
Subjects: Physics, Solar System, Magnetosphere, Astronomy and Astrophysics, Astrobiology, symbols.namesake, Solar wind, Magnetosheath, Planetary science, Space and Planetary Science, Physics::Space Physics, symbols, Astrophysics::Earth and Planetary Astrophysics, Interplanetary magnetic field, Ionosphere, Titan (rocket family)
Abstract: 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.
Published: 2011

19. Source mechanism of Saturn narrowband emission

Author: Shengyi Ye, Peter H. Yoon, Baptiste Cecconi, J. D. Menietti, Abigail Rymer, Department of Physics and Astronomy, Iowa State University, Institute for Physical Science and Technology, University of Maryland, School of Space Research, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique des plasmas, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Applied Physics Laboratory, Johns Hopkins University
Subjects: Atmospheric Science, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Cyclotron, Magnetosphere, Electron, 01 natural sciences, 7. Clean energy, Jovian, law.invention, Narrowband, law, Saturn, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), Maser, lcsh:Science, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, lcsh:QC801-809, Geology, Astronomy and Astrophysics, Plasma, lcsh:QC1-999, Computational physics, lcsh:Geophysics. Cosmic physics, 13. Climate action, Space and Planetary Science, Physics::Space Physics, lcsh:Q, Atomic physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], lcsh:Physics
Abstract: Narrowband emission (NB) is observed at Saturn centered near 5 kHz and 20 kHz and harmonics. This emission appears similar in many ways to Jovian kilometric narrowband emission observed at higher frequencies, and therefore may have a similar source mechanism. Source regions of NB near 20 kHz are believed to be located near density gradients in the inner magnetosphere and the emission appears to be correlated with the occurrence of large neutral plasma clouds observed in the Saturn magnetotail. In this work we present the results of a growth rate analysis of NB emission (~20 kHz) near or within a probable source region. This is made possible by the sampling of in-situ wave and particle data. The results indicate waves are likely to be generated by the mode-conversion of directly generated Z-mode emission to O-mode near a density gradient. When the local hybrid frequency is close n fce (n is an integer and fce is the electron cyclotron frequency) with n=4, 5 or 6 in our case, electromagnetic Z-mode and weak ordinary (O-mode) emission can be directly generated by the cyclotron maser instability.
Published: 2010

20. Slow-mode shock candidate in the Jovian magnetosheath

Author: Abigail Rymer, Z. Bebesi, André Balogh, M. K. Dougherty, G. Erdos, William S. Kurth, Karoly Szego, Norbert Krupp, D. T. Young, and Gethyn R. Lewis
Subjects: Shock wave, Physics, Astrophysics::High Energy Astrophysical Phenomena, Magnetosphere, Astronomy and Astrophysics, Astrophysics, Geophysics, Jovian, Jupiter, Magnetosheath, Space and Planetary Science, Planet, Local time, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Bow shock (aerodynamics)
Abstract: We discuss some interesting plasma observations in the Jovian magnetosheath by the onboard plasma instruments of the Cassini spacecraft during the 2000–2001 Jupiter flyby. We propose that the observations are consistent with a slow-mode shock transition. In the terrestrial magnetosheath, a number of observations have been made that are consistent with slow-mode waves or shocks. In addition, a number of observations have established that, at least occasionally, slow-mode structures form at the plasma sheet-lobe boundary in the terrestrial magnetotail, related to X lines associated with reconnection. There has been only one previously reported observation of a slow-mode shock-like transition in the Jovian plasma environment. This observation was made in the dayside magnetosheath. The observation we report here was made well downstream of the magnetosphere in Jupiter’s magnetosheath, at local time ∼19:10. For our analysis we have used the data from the Cassini Plasma Spectrometer (CAPS) the Magnetospheric Imaging Instrument (MIMI) and the Magnetometer (MAG). The bow shock crossings observed by Cassini ranged downstream to −600 R J from the planet
Published: 2010

21. Cassini evidence for rapid interchange transport at Saturn

Author: J. D. Menietti, Howard Smith, Abigail Rymer, D. G. Mitchell, D. T. Young, A. M. Persoon, George Hospodarsky, Andrew J. Coates, M. K. Dougherty, T. W. Hill, Barry Mauk, Chris Paranicas, and Nicolas André
Subjects: Physics, Bubble, Plasma sheet, Magnetosphere, Astronomy and Astrophysics, Geophysics, Radius, Astrophysics, Space and Planetary Science, Saturn, Magnetosphere of Saturn, Physics::Space Physics, Electron temperature, Astrophysics::Earth and Planetary Astrophysics, Pitch angle
Abstract: During its tour Cassini has observed numerous plasma injection events in Saturn's inner magnetosphere. Here, we present a case study of one “young” plasma bubble observed when Cassini was in the equatorial plane. The bubble was observed in the equatorial plane at ∼7 Saturn radii from Saturn and had a maximum azimuthal extent of ∼0.25 Rs (Rs=Saturn radius ∼60330 km). We show that the electron density inside the event is lower by a factor ∼3 and the electron temperature higher by over an order of magnitude compared to its surroundings. The injection contains slightly increased magnetic field magnitude of 49 nT compared with a background field of 46 nT. Modelling of pitch angle distributions inside the plasma bubble and measurements of plasma drift provide a novel way to estimate that the bubble originated between 9
Published: 2009

22. Cassini observations of Saturn's inner plasmasphere: Saturn orbit insertion results

Author: E. C. Sittler, Howard Smith, M. Shappirio, Michelle F. Thomsen, Richard E. Hartle, D. T. Young, David J. McComas, M. H. Burger, Andrew J. Coates, Abigail Rymer, Dennis J. Chornay, Michele K. Dougherty, Robert E. Johnson, David G. Simpson, Nicolas André, and Daniel B. Reisenfeld
Subjects: Physics, Waves in plasmas, Magnetosphere, Astronomy and Astrophysics, Plasmasphere, Radial velocity, Pickup Ion, Space and Planetary Science, Saturn, Magnetosphere of Saturn, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Atomic physics, Enceladus
Abstract: We present new and definitive results of Cassini plasma spectrometer (CAPS) data acquired during passage through Saturn's inner plasmasphere by the Cassini spacecraft during the approach phase of the Saturn orbit insertion period. This analysis extends the original analysis of Sittler et al. [2005. Preliminary results on Saturn's inner plasmasphere as observed by Cassini: comparison with Voyager. Geophys. Res. Lett. 32, L14S07, doi:10.1029/2005GL022653 ] to L∼10 along with also providing a more comprehensive study of the interrelationship of the various fluid parameters. Coincidence data are sub-divided into protons and water group ions. Our revised analysis uses an improved convergence algorithm which provides a more definitive and independent estimate of the spacecraft potential ΦSC for which we enforce the protons and water group ions to co-move with each other. This has allowed us to include spacecraft charging corrections to our fluid parameter estimations and allow accurate estimations of fluctuations in the fluid parameters for future correlative studies. In the appendix we describe the ion moments algorithm, and minor corrections introduced by not weighting the moments with sinθ term in Sittler et al. [2005] (Correction offset by revisions to instruments geometric factor). Estimates of the spacecraft potential and revised proton densities are presented. Our total ion densities are in close agreement with the electron densities reported by Moncuquet et al. [2005. Quasi-thermal noise spectroscopy in the inner magnetosphere of Saturn with Cassini/RPWS: electron temperatures and density. Geophys. Res. Lett. 32, L20S02, doi:10.1029/2005GL022508 ] who used upper hybrid resonance (UHR) emission lines observed by the radio and plasma wave science (RPWS) instrument. We show a positive correlation between proton temperature and water group ion temperature. The proton and thermal electron temperatures track each with both having a positive radial gradient. These results are consistent with pickup ion energization via Saturn's rotational electric field. We see evidence for an anti-correlation between radial flow velocity VR and azimuthal velocity Vφ, which is consistent with the magnetosphere tending to conserve angular momentum. Evidence for MHD waves is also present. We show clear evidence for outward transport of the plasma via flux tube interchange motions with the radial velocity of the flow showing positive radial gradient with V R ∼ 0.12 ( L / 4 ) 5.5 km / s functional dependence for 4 D LL ∼ D 0 L 11 for fixed stochastic time step δt). Previous models with centrifugal transport have used D LL ∼ D 0 L 3 dependence. The radial transport seems to begin at Enceladus’ L shell, L∼4, where we also see a minimum in the W+ ion temperature T W ∼ 35 eV . For the first time, we are measuring the actual flux tube interchange motions in the magnetosphere and how it varies with radial distance. These observations can be used as a constraint with regard to future transport models for Saturn's magnetosphere. Finally, we evaluate the thermodynamic properties of the plasma, which are all consistent with the pickup process being the dominant energy source for the plasma.
Published: 2006

23. The science case for an orbital mission to Uranus: Exploring the origins and evolution of ice giant planets

Author: Roberto Peron, Jonathan J. Fortney, Denis Grodent, Ralf Srama, L. Lamy, Robert Ebert, S. Hsu, Ioannis A. Daglis, Edward C. Sittler, K. Konstantinidis, Matthew S. Tiscareno, O. Karatekin, M. H. Hofstadter, Nicolas Rambaux, Matthew M. Hedman, Richard Holme, Andrew J. Coates, Tom Stallard, Pierre Henri, Sarah V. Badman, Bruno Christophe, Jessica Agarwal, M. I. Desai, Diego Turrini, Fritz M. Neubauer, Andrew Smith, Agustín Sánchez-Lavega, Julianne I. Moses, Davide Grassi, G. S. Orton, O. Mousis, N. André, C. Labrianidis, Mihaly Horanyi, Federico Tosi, Henrik Melin, P. Zarka, Mathew J. Owens, S. M. P. McKenna-Lawlor, Elizabeth P. Turtle, Benoît Noyelles, Shawn M. Brooks, Matthieu Laneuville, Richard M. Ambrosi, John F. Cooper, Dominic Dirkx, Caitriona M. Jackman, Mario M. Bisi, C. Bracken, Kevin H. Baines, Harald Krüger, Mathieu Barthelemy, E. Khalisi, Kunio M. Sayanagi, Pontus Brandt, Tom Nordheim, J. L. MacArthur, Ondrej Santolik, Glyn Collinson, Sascha Kempf, Jürgen Blum, Robert W. Wilson, I. de Pater, Veerle Sterken, William S. Kurth, Patrick G. J. Irwin, Craig B. Agnor, Frank Postberg, T. M. Bocanegra-Bahamón, Jon K. Hillier, Julie Castillo-Rogez, Eberhard Grün, Georg Moragas-Klostermeyer, Michele K. Dougherty, Christelle Briois, Christopher T. Russell, Nicholas Achilleos, Bertrand Bonfond, Mario Trieloff, Kurt D. Retherford, Abigail Rymer, Renaud Sallantin, Christina Plainaki, Frank Spahn, N. Nettelmann, Achim Morschhauser, S. Vinatier, Gabriel Tobie, Serge Reynaud, Elias Roussos, I. Gerth, A. Luntzer, Joachim Saur, M. Costa-Sitja, Paul M. Schenk, Ravit Helled, David M. Lucchesi, C. Briand, J. Schubert, Régis Courtin, George Hospodarsky, Thibault Cavalié, Sebastien Hess, Chris S. Arridge, V. Lainey, Adam Masters, Anna Milillo, Gianrico Filacchione, Andrea Maier, Jacques Gustin, Nick Sergis, Zoltan Sternovsky, Don Banfield, Leigh N. Fletcher, Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Centre for Planetary Sciences [UCL/Birkbeck] (CPS), Department of Physics and Astronomy [UCL London], European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Queen Mary University of London (QMUL), Space Research Centre [Leicester], University of Leicester, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institute of Space and Astronautical Science (ISAS), Department of Physics [Lancaster], Lancaster University, Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, University of Wisconsin-Madison, Cornell University, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Technische Universität Braunschweig [Braunschweig], Delft University of Technology (TU Delft), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, National University of Ireland Maynooth (NUIM), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire de physique et chimie de l'environnement (LPCE), Université d'Orléans (UO)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, DPHY, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, NASA Goddard Space Flight Center (GSFC), European Space Astronomy Centre (ESAC), Department of Physics [Athens], National and Kapodistrian University of Athens = University of Athens (NKUA | UoA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Southwest Research Institute [San Antonio] (SwRI), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Space and Atmospheric Physics Group [London], Blackett Laboratory, Imperial College London-Imperial College London, Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford [Oxford], University of California [Santa Cruz] (UCSC), University of California, Max-Planck-Institut für Kernphysik (MPIK), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], University of Idaho [Moscow, USA], Tel Aviv University [Tel Aviv], HEPPI - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Universität Heidelberg [Heidelberg], School of Environmental Sciences [Liverpool], University of Liverpool, University of Iowa [Iowa City], Department of Physics [Oxford], School of Physics and Astronomy [Southampton], University of Southampton, Royal Observatory of Belgium [Brussels], University of Stuttgart, Universität der Bundeswehr München [Neubiberg], Department of Physics and Astronomy [Iowa City], UTesat-Spacecom, Institut de Physique du Globe de Paris (IPGP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), University of Vienna [Vienna], Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Space Technology Ireland Limited, Institut für Raumfahrtsysteme (IRS), Universität Stuttgart [Stuttgart], Deutsches Zentrum für Luft- und Raumfahrt (DLR), Space Science Institute [Boulder] (SSI), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Institute for Geophysics and Meteorology [Köln] (IGM), University of Cologne, Université de Namur [Namur], University of Reading (UOR), Université Pierre et Marie Curie - Paris 6 - UFR de Médecine Pierre et Marie Curie (UPMC), Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire Kastler Brossel (LKB (Jussieu)), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Institute of Geophysics and Planetary Physics [Los Angeles] (IGPP), University of California [Los Angeles] (UCLA), University of California-University of California, University of the Basque Country [Bizkaia] (UPV/EHU), Institute of Atmospheric Physics, Institut für Geophysik und Meteorologie [Köln], Universität zu Köln, Institute of Atmospheric Physics [Prague] (IAP), Czech Academy of Sciences [Prague] (ASCR), Lunar and Planetary Institute [Houston] (LPI), Department of Earth Sciences [USC Los Angeles], University of Southern California (USC), Office for Space Research and Applications [Athens], Academy of Athens, University of Potsdam, Max Planck Institute for Nuclear Physics (MPIK), International Space Science Institute [Bern] (ISSI), Cornelle University, Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), Agence Spatiale Européenne = European Space Agency (ESA), 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), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), NASA-California Institute of Technology (CALTECH), Cornell University [New York], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], National University of Ireland Maynooth (Maynooth University), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), DPHY, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), National and Kapodistrian University of Athens (NKUA), University of Oxford, University of California [Santa Cruz] (UC Santa Cruz), University of California (UC), Tel Aviv University (TAU), HELIOS - LATMOS, Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universität Heidelberg [Heidelberg] = Heidelberg University, Royal Observatory of Belgium [Brussels] (ROB), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Université de Namur [Namur] (UNamur), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), University of California (UC)-University of California (UC), University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU), Universität zu Köln = University of Cologne, Czech Academy of Sciences [Prague] (CAS), University of Potsdam = Universität Potsdam, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), 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), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Pierre et Marie Curie - Paris 6 (UPMC)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), Centre for Planetary Sciences [UCL/Birkbeck] ( CPS ), European Space Research and Technology Centre ( ESTEC ), European Space Agency ( ESA ), Queen Mary University of London ( QMUL ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Institute of Space and Astronautical Science ( ISAS ), Jet Propulsion Laboratory ( JPL ), NASA-California Institute of Technology ( CALTECH ), University of Wisconsin-Madison [Madison], Institut de Planétologie et d'Astrophysique de Grenoble ( IPAG ), Observatoire des Sciences de l'Univers de Grenoble ( OSUG ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ) -Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ) -Centre National de la Recherche Scientifique ( CNRS ), STFC Rutherford Appleton Laboratory ( RAL ), Science and Technology Facilities Council ( STFC ), Delft University of Technology ( TU Delft ), Laboratoire de Physique Atmosphérique et Planétaire ( LPAP ), National University of Ireland Maynooth ( NUIM ), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] ( APL ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de physique et chimie de l'environnement ( LPCE ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Max-Planck-Institut für Sonnensystemforschung ( MPS ), ONERA - The French Aerospace Lab ( Toulouse ), ONERA, NASA Goddard Space Flight Center ( GSFC ), European Space Astronomy Center ( ESAC ), National and Kapodistrian University of Athens, University of California [Berkeley], Southwest Research Institute [San Antonio] ( SwRI ), Istituto di Astrofisica e Planetologia Spaziali ( IAPS ), Istituto Nazionale di Astrofisica ( INAF ), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] ( AOPP ), University of California [Santa Cruz] ( UCSC ), Max-Planck-Institut für Kernphysik ( MPIK ), Laboratory for Atmospheric and Space Physics [Boulder] ( LASP ), University of Colorado Boulder [Boulder], Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Mécanique Céleste et de Calcul des Ephémérides ( IMCCE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), University of Iowa [Iowa], University of Southampton [Southampton], Institut de Physique du Globe de Paris ( IPGP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -IPG PARIS-Université Paris Diderot - Paris 7 ( UPD7 ) -Université de la Réunion ( UR ) -Centre National de la Recherche Scientifique ( CNRS ), Space Research Institute of Austrian Academy of Sciences ( IWF ), Austrian Academy of Sciences ( OeAW ), Institut für Raumfahrtsysteme ( IRS ), Deutsches Zentrum für Luft- und Raumfahrt ( DLR ), Space Science Institute [Boulder] ( SSI ), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules ( UTINAM ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Franche-Comté ( UFC ), Institute for Geophysics and Meteorology [Köln] ( IGM ), University of Reading ( UOR ), Université Pierre et Marie Curie - Paris 6 - UFR de Médecine Pierre et Marie Curie ( UPMC ), Université Pierre et Marie Curie - Paris 6 ( UPMC ), Laboratoire Kastler Brossel ( LKB (Jussieu) ), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris ( FRDPENS ), Centre National de la Recherche Scientifique ( CNRS ) -École normale supérieure - Paris ( ENS Paris ) -Centre National de la Recherche Scientifique ( CNRS ) -École normale supérieure - Paris ( ENS Paris ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Centre National de la Recherche Scientifique ( CNRS ), Institute of Geophysics and Planetary Physics [Los Angeles] ( IGPP ), University of California at Los Angeles [Los Angeles] ( UCLA ), University of the Basque Country [Bizkaia] ( UPV/EHU ), Institute of Atmospheric Physics [Prague] ( IAP ), Czech Academy of Sciences [Prague] ( ASCR ), Lunar and Planetary Institute [Houston] ( LPI ), Department of Earth Sciences [Los Angeles], University of Southern California ( USC ), Laboratoire de Planétologie et Géodynamique de Nantes ( LPGN ), Université de Nantes ( UN ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), and International Space Science Institute ( ISSI )
Subjects: Outer planets, Gas giant, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Uranus, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Natural satellites, Astrobiology, ice giant planets, Neptune, Rings, Physics, Naturalsatellites, Atmosphere, Nice model, Institut für Physik und Astronomie, Astronomy, Astronomy and Astrophysics, orbital mission, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], science case, [ PHYS.ASTR.EP ] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Rings of Uranus, Space and Planetary Science, Exploration of Uranus, Magnetosphere, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Planetary interior, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Ice giant
Abstract: 著者人数: 114名, Accepted: 2014-08-07, 資料番号: SA1005021000
Published: 2014

24. Uranus Pathfinder: exploring the origins and evolution of Ice Giant planets

Author: Abigail Rymer, S. Kemble, Elias Roussos, Sebastien Hess, Benoît Noyelles, Imke de Pater, Nick Sergis, Glyn Collinson, Stas Barabash, Ravit Helled, Jared Leisner, Chris S. Arridge, Nicholas A Teanby, Baptiste Cecconi, Andy F. Cheng, Norbert Krupp, Andrew Bacon, Joachim Saur, Yves Langevin, Andrew Fazakerley, Steve Miller, Jaques Gustin, Matthew S. Tiscareno, Christopher T. Russell, Mathieu Barthelemy, Nadine Nettelmann, Richard Holme, Philippe Zarka, Ingo Müller-Wodarg, Apostolos A. Christou, Andrew J. Coates, Robert Ebert, Thomas P. Andert, Olivier Mousis, Sandrine Vinatier, Paul M. Schenk, Gerald Schubert, Laurent Lamy, Michael Guest, Craig B. Agnor, Régis Courtin, Daniel Gautier, Jan-Erik Wahlund, Cesar Bertucci, Ulrich R. Christensen, Pontus Brandt, Javier Martin-Torres, Adam Masters, Don Banfield, Silvia Tellmann, Elizabeth P. Turtle, Matthew M. Hedman, Frank Sohl, Mark Hofstadter, Leigh N. Fletcher, Özgür Karatekin, Chris Paranicas, Kunio M. Sayanagi, Nicolas André, Agustín Sánchez-Lavega, Tom Stallard, Kevin H. Baines, Eric Quémerais, Martin Pätzold, Supriya Chakrabarti, Marina Galand, L. Peacocke, Pierre Henri, John F. Cooper, Gabriel Tobie, Marta Entradas, Nicholas Achilleos, Michele K. Dougherty, Renée Prangé, C. P. Chaloner, Henrik Melin, Geraint H. Jones, Jonathan J. Fortney, Edward C. Sittler, Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), School of Physics and Astronomy [London], Queen Mary University of London (QMUL), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford [Oxford], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), University of Rostock [Germany], Institute of Geophysics and Planetary Physics [Los Angeles] (IGPP), University of California [Los Angeles] (UCLA), University of California-University of California, Department of Physics and Astronomy [Leicester], University of Leicester, Cornell University, Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), Astrium [Stevenage], EADS - European Aeronautic Defense and Space, Department of Physics and Astronomy [UCL London], Universität der Bundeswehr München [Neubiberg], Swedish Institute of Space Physics [Uppsala] (IRF), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astronomía y Física del Espacio [Buenos Aires] (IAFE), Universidad de Buenos Aires [Buenos Aires] (UBA)-Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Center for Space Physics [Boston] (CSP), Boston University [Boston] (BU), Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Armagh Observatory [Armagh], NASA Goddard Space Flight Center (GSFC), Blackett Laboratory, Imperial College London, Southwest Research Institute [San Antonio] (SwRI), Department of Science and Technology Studies [London] (STS), University of California [Santa Cruz] (UCSC), University of California, Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Department of Earth and Space Sciences [Los Angeles], University of Colorado [Boulder], School of Environmental Sciences [Liverpool], University of Liverpool, Royal Observatory of Belgium [Brussels], University of Iowa [Iowa City], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Space Research Centre [Leicester], Fondation Universitaire Notre Dame de la Paix (FUNDP), Facultés Universitaires Notre-Dame de la Paix, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy [Berkeley], University of California [Berkeley], Rhenish Institute for Environmental Research (RIU), University of Cologne, HEPPI - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU), Institute for Geophysics and Meteorology [Köln] (IGM), Lunar and Planetary Institute [Houston] (LPI), Office for Space Research and Applications [Athens], Academy of Athens, DLR Institute of Planetary Research, German Aerospace Center (DLR), School of Earth Sciences [Bristol], University of Bristol [Bristol], 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), University of Oxford, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), University of Rostock, University of California (UC)-University of California (UC), Cornell University [New York], Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET)-Universidad de Buenos Aires [Buenos Aires] (UBA), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), University of California [Santa Cruz] (UC Santa Cruz), University of California (UC), Royal Observatory of Belgium [Brussels] (ROB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Facultés Universitaires Notre Dame de la Paix (FUNDP), University of California [Berkeley] (UC Berkeley), HELIOS - LATMOS, 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, California Institute of Technology (CALTECH)-NASA, Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Universität der Bundeswehr München [Neubiberg] = Bundeswehr University, Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), Queen Mary University of London ( QMUL ), Centre d'étude spatiale des rayonnements ( CESR ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Jet Propulsion Laboratory ( JPL ), NASA-California Institute of Technology ( CALTECH ), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] ( AOPP ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules ( UTINAM ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Franche-Comté ( UFC ), Institute of Geophysics and Planetary Physics [Los Angeles] ( IGPP ), University of California at Los Angeles [Los Angeles] ( UCLA ), Laboratoire de Planétologie et Géodynamique de Nantes ( LPGN ), Université de Nantes ( UN ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Swedish Institute of Space Physics [Uppsala] ( IRF ), Institut de Planétologie et d'Astrophysique de Grenoble ( IPAG ), Observatoire des Sciences de l'Univers de Grenoble ( OSUG ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ) -Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ) -Centre National de la Recherche Scientifique ( CNRS ), Instituto de Astronomia y Fisica del Espacio ( IAFE ), Consejo Nacional de Investigaciones Científicas y Técnicas ( CONICET ) -Universidad de Buenos Aires [Buenos Aires], Johns Hopkins University Applied Physics Laboratory [Laurel, MD] ( APL ), Center for Space Physics [Boston] ( CSP ), Boston University [Boston] ( BU ), Max Planck Institute for Solar System Research ( MPS ), NASA Goddard Space Flight Center ( GSFC ), Southwest Research Institute [San Antonio] ( SwRI ), Department of Science and Technology Studies [London] ( STS ), University of California [Santa Cruz] ( UCSC ), Laboratoire de Physique Atmosphérique et Planétaire ( LPAP ), University of Colorado Boulder [Boulder], University of Iowa [Iowa], Centro de Astrobiologia [Madrid] ( CAB ), Instituto Nacional de Técnica Aeroespacial ( INTA ) -Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Fondation Universitaire Notre Dame de la Paix ( FUNDP ), Institut de Mécanique Céleste et de Calcul des Ephémérides ( IMCCE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Astronomy Department [Berkeley], Rhenish Institute for Environmental Research ( RIU ), Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), University of the Basque Country/Euskal Herriko Unibertsitatea ( UPV/EHU ), Institute for Geophysics and Meteorology [Köln] ( IGM ), Lunar and Planetary Institute [Houston] ( LPI ), and German Aerospace Center ( DLR )
Subjects: Solar System, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Ciencias Físicas, Uranus, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], interior, Natural satellite, 7. Clean energy, 01 natural sciences, Astrobiology, Ice Giant, Orbiter, Neptune, Planet, 0103 physical sciences, 010303 astronomy & astrophysics, ICE GIANT, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], natural satellite, ice giants, Nice model, Giant planet atmosphere, Astronomy, Astronomy and Astrophysics, Planetary system, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Ring system, Dynamo, Astronomía, [ PHYS.ASTR.EP ] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], URANUS, 13. Climate action, Space and Planetary Science, Exploration of Uranus, Magnetosphere, GIANT PLANET ATMOSPHERE, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ORBITER, CIENCIAS NATURALES Y EXACTAS, Ice giant
Abstract: The “Ice Giants” Uranus and Neptune are a different class of planet compared to Jupiter and Saturn. Studying these objects is important for furthering our understanding of the formation and evolution of the planets, and unravelling the fundamental physical and chemical processes in the Solar System. The importance of filling these gaps in our knowledge of the Solar System is particularly acute when trying to apply our understanding to the numerous planetary systems that have been discovered around other stars. The Uranus Pathfinder (UP) mission thus represents the quintessential aspects of the objectives of the European planetary community as expressed in ESA’s Cosmic Vision 2015–2025. UP was proposed to the European Space Agency’s M3 call for medium-class missions in 2010 and proposed to be the first orbiter of an Ice Giant planet. As the most accessible Ice Giant within the M-class mission envelope Uranus was identified as the mission target. Although not selected for this call the UP mission concept provides a baseline framework for the exploration of Uranus with existing low-cost platforms and underlines the need to develop power sources suitable for the outer Solar System. The UP science case is based around exploring the origins, evolution, and processes at work in Ice Giant planetary systems. Three broad themes were identified: (1) Uranus as an Ice Giant, (2) An Ice Giant planetary system, and (3) An asymmetric magnetosphere. Due to the long interplanetary transfer from Earth to Uranus a significant cruise-phase science theme was also developed. The UP mission concept calls for the use of a Mars Express/Rosetta-type platform to launch on a Soyuz–Fregat in 2021 and entering into an eccentric polar orbit around Uranus in the 2036–2037 timeframe. The science payload has a strong heritage in Europe and beyond and requires no significant technology developments. Fil: Arridge, Christopher S.. University College London; Estados Unidos Fil: Agnor, Craig B.. Queen Mary University of London; Reino Unido Fil: Andre, Nicolas. Centre National de la Recherche Scientifique; Francia Fil: Baines, Kevin H.. National Aeronautics And Space Administration; Estados Unidos Fil: Fletcher, Leigh N.. University of Oxford; Reino Unido Fil: Gautier, Daniel. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Hofstadter, Mark D.. National Aeronautics And Space Administration; Estados Unidos Fil: Jones, Geraint H.. University College London; Estados Unidos Fil: Lamy, Laurent. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Langevin, Yves. Centre National de la Recherche Scientifique; Francia Fil: Mousis, Olivier. Centre National de la Recherche Scientifique; Francia Fil: Nettelmann, Nadine. Universitat Rostock; Alemania Fil: Russell, Christopher T.. University of California at Los Angeles; Estados Unidos Fil: Stallard, Tom. University of Leicester; Reino Unido Fil: Tiscareno, Matthew S.. Cornell University; Estados Unidos Fil: Tobie, Gabriel. Centre de Recherche de Nantes; Francia Fil: Bacon, Andrew. Systems Engineering and Asssessment Ltd; Reino Unido Fil: Chaloner, Chris. Systems Engineering and Asssessment Ltd; Reino Unido Fil: Guest, Michael. Systems Engineering and Asssessment Ltd; Reino Unido Fil: Kemble, Steve. Astrium; Reino Unido Fil: Peacocke, Lisa. Astrium; Reino Unido Fil: Achilleos, Nicholas. University College London; Estados Unidos Fil: Andert, Thomas P.. Universität der Bundeswehr; Alemania Fil: Banfield, Don. Cornell University; Estados Unidos Fil: Barabash, Stas. Sweden Institute of Space Physics; Suecia Fil: Barthelemy, Matthieu. Universite Joseph Fourier; 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: Brandt, Pontus. University Johns Hopkins; Estados Unidos Fil: Cecconi, Baptiste. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Chakrabarti, Supriya. Boston University; Estados Unidos
Published: 2012

25. Ion distributions of different Kronian plasma regions

Author: Andrew J. Coates, Edward C. Sittler, Abigail Rymer, Anne Wellbrock, Karoly Szego, G. Erdős, L. Foldy, Z. Bebesi, and Zoltán Németh
Subjects: Physics, Atmospheric Science, Ecology, Paleontology, Soil Science, Magnetosphere, Forestry, Plasma, Electron, Aquatic Science, Oceanography, Spectral line, Ion, symbols.namesake, Geophysics, Space and Planetary Science, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), symbols, Atomic physics, Ionosphere, Titan (rocket family), Longitude, Earth-Surface Processes, Water Science and Technology
Abstract: [1] Plasma data from the Cassini Plasma Spectrometer experiment were used to investigate the properties of the variable plasma environment of Titan's orbit. The characteristics of this plasma environment play a crucial role in the plasma-moon interaction and also have a strong influence on the ionosphere of Titan. Using dynamic energy spectra of ions within ±3 h of the Titan flybys we identified different ambient plasma environments, similar to the ones proposed earlier based on electron measurements. Expanding the time interval to 12 h to cover full SKR periods, and taking into account the composition of the ions, we showed that the longer intervals include all the previous categories, and a special one, a short event, rich in heavy ions. Detailed study of the vicinity of these events revealed the fine structure of the magnetodisk of Saturn, having a narrow central sheet of very high heavy ion content, heavy rich events occurring when the spacecraft crosses this central sheet. We also proved that the heavy rich events appear periodically in longitude, but with a period slightly (by 0.35°/day) longer than the SLS3 period.
Published: 2011

26. The auroral footprint of Enceladus on Saturn

Author: D. G. Mitchell, A. Ian F. Stewart, Geraint H. Jones, Joshua Colwell, Abigail Rymer, Stamatios M. Krimigis, Gregory M. Holsclaw, William E. McClintock, Michele K. Dougherty, A. Jouchoux, Joachim Saur, Denis Grodent, T. W. Hill, Jacques Gustin, Jonathan D. Nichols, Jean-Claude Gérard, Sven Jacobsen, Larry W. Esposito, Stan W. H. Cowley, Amanda R. Hendrix, Laurent Lamy, Xiaoyan Zhou, Barry Mauk, Joseph M. Ajello, Andrew J. Coates, F. J. Crary, John Clarke, Wayne Pryor, D. T. Young, Space Environment Technologies, Pacific Palisades, Applied Physics Laboratory, Johns Hopkins University, Department of Physics and Astronomy, Rice University, Houston, Space Science and Engineering Division, Southwest Research Institute, Institut für Geophysik und Meteorologie, Universität zu Köln (IGM), Mullard Space Science Laboratory, Department of Space and Climate Physics, University of Leicester, Laboratoire de Physique Atmosphérique et Planétaire, Université de Liège (LPAP), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique des plasmas, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, University of Colorado, Laboratory for Atmospheric and Space Physics (LASP), Imperial College London, Jet Propulsion Laboratory, California Institute of Technology (JPL), Department of Physics, University of Central Florida, and Department of Astronomy, Boston University, Boston
Subjects: Physics, Multidisciplinary, Astronomy, Magnetosphere, Tidal heating, Astrobiology, Planetary science, Gas torus, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Great conjunction, Ionosphere, Enceladus, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Order of magnitude
Abstract: International audience; Although there are substantial differences between the magnetospheres of Jupiter and Saturn, it has been suggested that cryovolcanic activity at Enceladus could lead to electrodynamic coupling between Enceladus and Saturn like that which links Jupiter with Io, Europa and Ganymede. Powerful field-aligned electron beams associated with the Io-Jupiter coupling, for example, create an auroral footprint in Jupiter's ionosphere. Auroral ultraviolet emission associated with Enceladus-Saturn coupling is anticipated to be just a few tenths of a kilorayleigh (ref. 12), about an order of magnitude dimmer than Io's footprint and below the observable threshold, consistent with its non-detection. Here we report the detection of magnetic-field-aligned ion and electron beams (offset several moon radii downstream from Enceladus) with sufficient power to stimulate detectable aurora, and the subsequent discovery of Enceladus-associated aurora in a few per cent of the scans of the moon's footprint. The footprint varies in emission magnitude more than can plausibly be explained by changes in magnetospheric parameters--and as such is probably indicative of variable plume activity.
Published: 2011

27. Upstream of Saturn and Titan

Author: F. J. Crary, P. Garnier, Zoltán Németh, Andrew J. Coates, Chris S. Arridge, Nick Sergis, Cesar Bertucci, Caitriona M. Jackman, Karoly Szego, Abigail Rymer, and Nicolas André
Subjects: Solar System, Solar wind, symbols.namesake, Magnetosheath, Physics::Space Physics, symbols, Magnetosphere, Classification scheme, Astrophysics::Earth and Planetary Astrophysics, Plasma, Ionosphere, Titan (rocket family), Astrobiology
Abstract: 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.
Published: 2011

28. Rate of radial transport of plasma in Saturn's inner magnetosphere

Author: R. J. Wilson, T. W. Hill, Abigail Rymer, and Y. Chen
Subjects: Convection, Atmospheric Science, Astrophysics::High Energy Astrophysical Phenomena, Soil Science, Magnetosphere, Astrophysics, Aquatic Science, Oceanography, Physics::Plasma Physics, Geochemistry and Petrology, Saturn, Earth and Planetary Sciences (miscellaneous), Earth-Surface Processes, Water Science and Technology, Physics, Ecology, Flux tube, Plasma sheet, Paleontology, Forestry, Geophysics, Plasma, Space and Planetary Science, Magnetosphere of Saturn, Physics::Space Physics, Outflow, Astrophysics::Earth and Planetary Astrophysics
Abstract: [1] In the inner part of a rapidly rotating magnetosphere such as that of Saturn, the major observable signature of radial plasma convection is a series of longitudinally localized injections and simultaneous drift dispersions of hot tenuous plasma from the outer magnetosphere. The Cassini Plasma Spectrometer (CAPS) and the Cassini Magnetospheric Imaging Instrument (MIMI) have observed signatures of these processes frequently, thus providing direct evidence for Saturn's magnetospheric convective motions, in which the radial transport of plasma comprises hot, tenuous plasma moving inward and cooler, denser plasma moving outward. On the basis of an extended statistical sample of these injection/dispersion events, we find that the inflow channels occupy only a small fraction (∼7%) of the total available longitudinal space, indicating that the inflow speed is much larger than the outflow speed. We assume that the plasma is largely confined to a thin equatorial sheet and calculate its thickness by deriving the centrifugal scale height profile based on the CAPS observations. We also present the radial and longitudinal dependences of flux tube mass content as well as the total ion mass between 5 and 10 Saturn radii. Combining these results, we estimate a global plasma mass outflow rate ∼280 kg/s.
Published: 2010

29. Transport of energetic electrons into Saturn's inner magnetosphere

Author: Abigail Rymer, Peter Kollmann, D. G. Mitchell, Elias Roussos, Stamatios M. Krimigis, Pontus Brandt, F. S. Turner, Robert E. Johnson, Norbert Krupp, Chris Paranicas, and A. L. Müller
Subjects: Atmospheric Science, Astrophysics::High Energy Astrophysical Phenomena, Soil Science, Magnetosphere, Boundary (topology), Astrophysics, Electron, Aquatic Science, Oceanography, Geochemistry and Petrology, Planet, Saturn, Earth and Planetary Sciences (miscellaneous), Adiabatic process, Earth-Surface Processes, Water Science and Technology, Physics, Ecology, Paleontology, Forestry, Geophysics, Space and Planetary Science, Adiabatic invariant, Local time, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics
Abstract: [1] We present energetic electron data obtained by Cassini’s Magnetospheric Imaging Instrument in the inner magnetosphere of Saturn. We find here that inward transport and energization processes are consistent with conservation of the first two adiabatic invariants of motion. We model several injections near local midnight, one injection has a maximum energy of hundreds of keV, that are consistent with data. We also present mission‐ averaged data that shows an injection boundary in radial distance. Inward of this boundary, fluxes fall off toward the planet. Around this inner boundary, strong local time asymmetries are present in the averaged data with peak fluxes near midnight.
Published: 2010

30. Azimuthal plasma flow in the Kronian magnetosphere

Author: Stamatios M. Krimigis, Barry Mauk, Joachim Saur, Abigail Rymer, Elias Roussos, D. G. Mitchell, A. L. Müller, and Norbert Krupp
Subjects: Atmospheric Science, Soil Science, Magnetosphere, Electron, Aquatic Science, Oceanography, Relativistic particle, Geochemistry and Petrology, Saturn, Earth and Planetary Sciences (miscellaneous), Dispersion (water waves), Earth-Surface Processes, Water Science and Technology, Physics, Ecology, Plasma sheet, Paleontology, Forestry, Plasma, Computational physics, Geophysics, Space and Planetary Science, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Atomic physics, Event (particle physics)
Abstract: [1] We study the azimuthal plasma velocity in Saturn's magnetosphere between 3 and 13 Saturn radii (Rs) by analyzing energetic particle injection events using data of the Magnetospheric Imaging Instrument (MIMI) onboard the Cassini spacecraft in orbit around Saturn. Due to the magnetic drifts, the injected particles at various energies begin to disperse and leave an imprint in the electron as well as in the ion energy spectrograms of the MIMI instrument. The shape of these profiles strongly depends on the azimuthal velocity distribution of the magnetospheric plasma and the age of the injection event. Comparison of theoretically computed dispersion profiles with observed ones enables us to characterize the azimuthal flow of the plasma. The measured flow profile clearly shows that the plasma subcorotates with velocities as low as 80% of full corotation at radial distances between 8 Rs to 13 Rs. With knowledge of the flow profile and the ages of each injection event we can calculate the location where the energetic particles were injected into the inner magnetosphere. The night and morning sector of the Kronian magnetosphere are preferred regions for the generation of hot plasma injections.
Published: 2010

31. Particle pressure, inertial force, and ring current density profiles in the magnetosphere of Saturn, based on Cassini measurements

Author: Edmond C. Roelof, Michelle F. Thomsen, Andrew J. Coates, D. G. Mitchell, Norbert Krupp, Nick Sergis, D. C. Hamilton, Michele K. Dougherty, Abigail Rymer, D. T. Young, Chris S. Arridge, and Stamatios M. Krimigis
Subjects: Physics, Magnetosphere, Plasma, Geodesy, Computational physics, Magnetic field, Geophysics, Saturn, Beta (plasma physics), Physics::Space Physics, General Earth and Planetary Sciences, Magnetic pressure, Astrophysics::Earth and Planetary Astrophysics, Pressure gradient, Ring current
Abstract: We report initial results on the particle pressure distribution and its contribution to ring current density in the equatorial magnetosphere of Saturn, as measured by the Magnetospheric Imaging Instrument (MIMI) and the Cassini Plasma Spectrometer (CAPS) onboard the Cassini spacecraft. Data were obtained from September 2005 to May 2006, within +/- 0.5 R-S from the nominal magnetic equator in the range 6 to 15 RS. The analysis of particle and magnetic field measurements, the latter provided by the Cassini magnetometer (MAG), allows the calculation of average radial profiles for various pressure components in Saturn's magnetosphere. The radial gradient of the total particle pressure is compared to the inertial body force to determine their relative contribution to the Saturnian ring current, and an average radial profile of the azimuthal current intensity is deduced. The results show that: ( 1) Thermal pressure dominates from 6 to 9 RS, while thermal and suprathermal pressures are comparable outside 9 RS with the latter becoming larger outside 12 RS. ( 2) The plasma beta (particle/magnetic pressure) remains >= 1 outside 8 RS, maximizing (similar to 3 to similar to 10) between 11 and 14 RS. ( 3) The inertial body force and the pressure gradient are similar at 9-10 R-S, but the gradient becomes larger >= 11 R-S. ( 4) The azimuthal ring current intensity develops a maximum between approximately 8 and 12 RS, reaching values of 100-150 pA/m(2). Outside this region, it drops with radial distance faster than the 1/r rate assumed by typical disk current models even though the total current is not much different to the model results.
Published: 2010

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

Author: D. T. Young, Anne Wellbrock, Abigail Rymer, Andrew J. Coates, and Howard Smith
Subjects: Physics, Plasma sheet, Magnetosphere, Plasma, Electron, Astrophysics, Spectral line, symbols.namesake, Geophysics, Magnetosheath, symbols, General Earth and Planetary Sciences, Magnetopause, Atomic physics, Titan (rocket family)
Abstract: We analyse combined electron spectra across the dynamic range of both Cassini electron sensors in order to characterise the background plasma environment near Titan for 54 Cassini-Titan encounters as of May 2009. We characterise the encounters into four broad types: Plasma sheet, Lobe-like, Magnetosheath and Bimodal. Despite many encounters occurring close to the magnetopause only two encounters to date were predominantly in the magnetosheath (T32 and T42). Bimodal encounters contain two distinct electron populations, the low energy component of the bi-modal populations is apparently associated with local water group products. Additionally, a hot lobe-like environment is also occasionally observed and is suggestively linked to increased local pick-up. We find that 34 of 54 encounters analysed are associated with one of these groups while the remaining encounters exhibit a combination of these environments. We provide typical electron properties and spectra for each plasma regime and list the encounters appropriate to each. Citation: Rymer, A.M., H. T. Smith, A. Wellbrock, A.J. Coates, and D.T. Young (2009), Discrete classification and electron energy spectra of Titan's varied magnetospheric environment, Geophys. Res. Lett., 36, L15109, doi: 10.1029/2009GL039427.
Published: 2009

33. Analysis of narrowband emission observed in the Saturn magnetosphere

Author: Peter H. Yoon, Abigail Rymer, Shengyi Ye, Ondrej Santolik, J. D. Menietti, Andrew J. Coates, and Donald A. Gurnett
Subjects: Atmospheric Science, Astrophysics::High Energy Astrophysical Phenomena, Cyclotron, Soil Science, Magnetosphere, Astrophysics::Cosmology and Extragalactic Astrophysics, Aquatic Science, Oceanography, Electromagnetic radiation, law.invention, Narrowband, Geochemistry and Petrology, law, Saturn, Earth and Planetary Sciences (miscellaneous), Maser, Astrophysics::Galaxy Astrophysics, Earth-Surface Processes, Water Science and Technology, Physics, Ecology, Paleontology, Forestry, Geophysics, Space and Planetary Science, Harmonics, Physics::Space Physics, Harmonic, Atomic physics
Abstract: [1] Narrowband emission is observed at Saturn centered near 5 kHz and 20 kHz and harmonics of 20 kHz. This emission appears to be in many ways similar to Jovian narrowband emission observed at higher frequencies. We analyze one example of this emission near a possible source region. In situ electron distributions suggest narrowband emission has a source region associated with electrostatic cyclotron harmonic and upper hybrid emission. Linear growth rate calculations indicate that the observed plasma distributions are unstable to the growth of electrostatic harmonic emissions. In addition, it is found that when the local upper hybrid frequency is close to 2 fce or 3 fce (fce is the electron cyclotron frequency), electromagnetic Z mode and weak ordinary (O mode) emission can be directly generated by the cyclotron maser instability. In the presence of density gradients, Z mode emission can mode-convert into O mode emission, and this might explain the narrowband emission observed by the Cassini spacecraft.
Published: 2009

34. Identification of Saturn's magnetospheric regions and associated plasma processes: Synopsis of Cassini observations during orbit insertion

Author: Iannis Dandouras, P. Louarn, Robert E. Johnson, Norbert Krupp, R. Srama, Sylvestre Maurice, John Clarke, D. G. Mitchell, Raúl A. Baragiola, Howard Smith, Larry W. Esposito, Sascha Kempf, Nicholas Achilleos, Scott Bolton, M. K. Dougherty, Tamas I. Gombosi, Abigail Rymer, Michel Blanc, Edward C. Sittler, D. A. Gurnett, Kirk C. Hansen, Andrew J. Coates, P. Schippers, D. T. Young, Hunter Waite, Chris S. Arridge, D. C. Hamilton, Stamatios M. Krimigis, F. J. Crary, E. Pallier, William S. Kurth, and N. Andre
Subjects: Physics, Exploration of Saturn, Energetic neutral atom, Astrophysics::High Energy Astrophysical Phenomena, Plasma sheet, Astronomy, Magnetosphere, Geophysics, Magnetosphere of Saturn, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Enceladus, Magnetosphere of Jupiter, Ring current
Abstract: [1] Saturn's magnetosphere is currently studied from the microphysical to the global scale by the Cassini-Huygens mission. During the first half of 2004, in the approach phase, remote sensing observations of Saturn's magnetosphere gave access to its auroral, radio, UV, energetic neutral atom, and dust emissions. Then, on 1 July 2004, Cassini Saturn orbit insertion provided us with the first in situ exploration of Saturn's magnetosphere since Voyager. To date, Saturn orbit insertion is the only Cassini orbit to have been described in common by all field and particle instruments. We use the comprehensive suite of magnetospheric and plasma science instruments to give a unified description of the large-scale structure of the magnetosphere during this particular orbit, identifying the different regions and their boundaries. These regions consist of the Saturnian ring system (region 1, within 3 Saturn radii (RS)) and the cold plasma torus (region 2, within 5–6 RS) in the inner magnetosphere, a dynamic and extended plasma sheet (region 3), and an outer high-latitude magnetosphere (region 4, beyond 12–14 RS). We compare these observations to those made at the time of the Voyager encounters. Then, we identify some of the dominant chemical characteristics and dynamical phenomena in each of these regions. The inner magnetosphere is characterized by the presence of the dominant plasma and neutral sources of the Saturnian system, giving birth to a very special magnetosphere dominated by water products. The extended plasma sheet, where the ring current resides, is a variable region with stretched magnetic field lines and contains a mixture of cold and hot plasma populations resulting from plasma transport processes. The outer high-latitude magnetosphere is characterized by a quiet magnetic field and an absence of plasma. Saturn orbit insertion observations enabled us to capture a snapshot of the large-scale structure of the Saturnian magnetosphere and of some of the main plasma processes operating in this complex environment. The analysis of the broad diversity of these interaction processes will be one of the main themes of magnetospheric and plasma science during the Cassini mission.
Published: 2008

35. Analysis of plasma waves observed within local plasma injections seen in Saturn's magnetosphere

Author: A. M. Persoon, George Hospodarsky, Abigail Rymer, Ondrej Santolik, Andrew J. Coates, D. T. Young, D. A. Gurnett, and John Menietti
Subjects: Atmospheric Science, Field line, Population, Soil Science, Magnetosphere, Electron, Aquatic Science, Oceanography, Optics, Physics::Plasma Physics, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Pitch angle, education, Earth-Surface Processes, Water Science and Technology, Physics, education.field_of_study, Ecology, Flux tube, business.industry, Paleontology, Forestry, Plasma, Geophysics, Space and Planetary Science, Physics::Space Physics, Electromagnetic electron wave, Atomic physics, business
Abstract: [1] Plasma injections or density depletion regions have been reported to be a prolific feature of Saturn's inner magnetosphere. They are characterized by flux tubes of warm, tenuous plasma in a cooler, locally produced plasma background. The injected plasma undergoes dispersion in energy due to gradient and curvature drifts as the flux tube transports. The plasma waves within these injections are of at least two types. Above the electron cyclotron frequency, fce, very intense and narrow-banded emissions resembling electrostatic cyclotron harmonics (ECH) are often observed. Below fce, whistler mode chorus is sometimes observed. Inside the plasma injections there exists a low-energy ( 1000 eV) component with “pancake” pitch angle distributions (peaked at 90°). We model the electron plasma distributions observed inside one injection to conduct a linear dispersion analysis of the wave modes. The results suggest that the ECH emissions can be generated by phase space density gradients associated with a narrow loss cone that is likely to be present but not observed because the electron detectors field of view did not include the magnetic field line at the time of the observations. The whistler mode chorus emission can be generated by the pancake-like distribution and temperature anisotropy (T⊥/T∥ > 1) of the warmest plasma population. Some interesting anomalies between the results and the observations may be resolved by analyses of additional injection events.
Published: 2008

36. Electron circulation in Saturn's magnetosphere

Author: Chris Paranicas, Andrew J. Coates, Barry Mauk, D. G. Mitchell, D. T. Young, T. W. Hill, and Abigail Rymer
Subjects: Physics, Atmospheric Science, Ecology, Flux tube, Paleontology, Soil Science, Magnetosphere, Flux, Forestry, Plasma, Electron, Aquatic Science, Oceanography, Geophysics, Space and Planetary Science, Geochemistry and Petrology, Saturn, Earth and Planetary Sciences (miscellaneous), Astrophysics::Earth and Planetary Astrophysics, Pitch angle, Atomic physics, Adiabatic process, Earth-Surface Processes, Water Science and Technology
Abstract: We present a model wherein electrons produced in Saturn's inner magnetosphere circulate through a combination of outward and inward motions driven by the centrifugal interchange instability and azimuthal motion through gradient and curvature drifts. Cool (< 100 eV) electrons produced inside L similar to 12 move slowly outward. To balance outflowing flux, inward transport occurs in small scale injection events. Electrons in these inwardly moving flux tubes are heated adiabatically to energies greater than 100 eV and their pitch angle distributions evolve from isotropic to "pancake'' ( peaked at 90 degrees). We show that this evolution is observed, and that the pitch angle distributions observed inside a plasma injection are consistent with loss free inward adiabatic transport from L similar to 11. As the flux tube moves inward the warm electrons undergo energy dependent gradient and curvature drifts out of the inwardly moving flux tube and find themselves superposed on cold, locally produced, plasma. At this point they turn around and are transported along with the cold plasma back toward the outer magnetosphere. With reasonable assumptions about scattering and loss this motion can naturally lead to the "butterfly'' electron pitch angle distributions ( with local minima at both 90 degrees and 0/180 degrees) that are observed in the warm electron plasma component. We note that we cannot reproduce the butterfly distributions using loss free outward adiabatic transport alone. This is to be expected because there exist pitch angle dependent losses in the form of Saturn's neutral gas cloud and E-ring.
Published: 2008

37. Magnetic signatures of plasma-depleted flux tubes in the Saturnian inner magnetosphere

Author: Philippe Louarn, Michelle F. Thomsen, William S. Kurth, Michele K. Dougherty, D. A. Gurnett, N. Andre, James L. Burch, A. M. Persoon, Jerry Goldstein, Edward C. Sittler, Abigail Rymer, D. T. Young, Gethyn R. Lewis, Andrew J. Coates, and F. J. Crary
Subjects: Physics, Flux tube, Magnetometer, Magnetosphere, Flux, Plasma, Astrophysics, Geophysics, equipment and supplies, Magnetic flux, Jovian, law.invention, law, Physics::Space Physics, General Earth and Planetary Sciences, Magnetic pressure, Astrophysics::Earth and Planetary Astrophysics, human activities
Abstract: Initial Cassini observations have revealed evidence for interchanging magnetic flux tubes in the inner Saturnian magnetosphere. Some of the reported flux tubes differ remarkably by their magnetic signatures, having a depressed or enhanced magnetic pressure relative to their surroundings. The ones with stronger fields have been interpreted previously as either outward moving mass-loaded or inward moving plasma-depleted flux tubes based on magnetometer observations only. We use detailed multi-instrumental observations of small and large density depletions in the inner Saturnian magnetosphere from Cassini Rev. A orbit that enable us to discriminate amongst the two previous and opposite interpretations. Our analysis undoubtedly confirms the similar nature of both types of reported interchanging magnetic flux tubes, which are plasma-depleted, whatever their magnetic signatures are. Their different magnetic signature is clearly an effect associated with latitude. These Saturnian plasma-depleted flux tubes ultimately may play a similar role as the Jovian ones.
Published: 2007

38. Mass of Saturn's magnetodisc: Cassini observations

Author: Christopher T. Russell, Nicholas Achilleos, Chris S. Arridge, Abigail Rymer, Krishan K. Khurana, Michele K. Dougherty, Andrew J. Coates, and Nicolas André
Subjects: Physics, Centrifugal force, Current sheet, Geophysics, Plane (geometry), Saturn, Plasma sheet, General Earth and Planetary Sciences, Magnetosphere, Astrophysics, Ring current, Magnetic field
Abstract: Saturn's ring current was observed by Pioneer 11 and the two Voyager spacecraft to extend 8 - 16 R-S in the equatorial plane and appeared to be driven by stress balance with the centrifugal force. We present Cassini observations that show thin current sheets on the dawn flank of Saturn's magnetosphere, symptomatic of the formation of a magnetodisc. We show that the centrifugal force is the dominant mechanical stress in these current sheets, which reinforces a magnetodisc interpretation - the formation of the current sheet is fundamentally rotational in origin. The stress balance calculation is also used to estimate the mass density in the disc, which show good agreement with independent in-situ measurements of the density. We estimate the total mass in the magnetodisc to be similar to 10(6) kg.
Published: 2007

39. Electron sources in Saturn's magnetosphere

Author: Chris Paranicas, Andrew J. Coates, Robert E. Johnson, Scott Bolton, Abigail Rymer, Michelle F. Thomsen, Howard Smith, D. G. Mitchell, Nicolas André, T. W. Hill, Barry Mauk, E. C. Sittler, D. T. Young, and Michele K. Dougherty
Subjects: Physics, Atmospheric Science, Ecology, Plasma sheet, Paleontology, Soil Science, Magnetosphere, Forestry, Electron, Aquatic Science, Oceanography, L-shell, Geophysics, Space and Planetary Science, Geochemistry and Petrology, Magnetosphere of Saturn, Saturn, Physics::Space Physics, Earth and Planetary Sciences (miscellaneous), Astrophysics::Earth and Planetary Astrophysics, Pitch angle, Atomic physics, Enceladus, Earth-Surface Processes, Water Science and Technology
Abstract: [1] We investigate the sources of two different electron components in Saturn's inner magnetosphere (5 100 eV) is Saturn's middle or outer magnetosphere, perhaps transported to the inner magnetosphere by radial diffusion regulated by interchange-like injections. Hot electrons undergo heavy losses inside L ∼ 6 and the distance to which the hot electron component penetrates into the neutral cloud is energy-dependent, with the coolest fraction of the hot plasma penetrating to the lowest L-shells. This can arise through energy-dependent radial transport during the interchange process and/or loss through the planetary loss cone.
Published: 2007

40. Preliminary interpretation of Titan plasma interaction as observed by the Cassini Plasma Spectrometer: Comparisons with Voyager 1

Author: Scott Bolton, Abigail Rymer, John T. Steinberg, J. Vilppola, N. André, F. J. Crary, Jean-Jacques Berthelier, Richard E. Hartle, D. T. Young, Edward C. Sittler, Robert E. Johnson, Andrew J. Coates, David J. McComas, David G. Simpson, Karoly Szego, Howard Smith, Fritz M. Neubauer, and Daniel B. Reisenfeld
Subjects: Physics, Spectrometer, Gyroradius, Magnetosphere, Astrophysics, Plasma, Ion, law.invention, Astrobiology, Pickup Ion, symbols.namesake, Orbiter, Geophysics, law, symbols, General Earth and Planetary Sciences, Titan (rocket family)
Abstract: The Cassini Plasma Spectrometer (CAPS) instrument made measurements of Titan s plasma environment when the Cassini Orbiter flew through the moon s plasma wake October 26,2004 (flyby TA) and December 13,2004 (flyby TB). Preliminary CAPS ion and electron measurements from these encounters (1,2) are compared with measurements made by the Voyager I Plasma Science Instrument (PLS). The comparisons are used to evaluate previous interpretations and predictions of the Titan plasma environment that have been made using PLS measurements (3,4). The plasma wake trajectories of flybys TA, TB and Voyager 1 are similar because they occurred when Titan was near Saturn s local noon. These similarities make possible direct, meaningful comparisons between the various plasma wake measurements. The inquiries stimulated by the previous interpretations and predictions made using PLS data have produced the following results from the CAPS ion measurements: A) The major ambient ion components of Saturn s rotating magnetosphere in the vicinity of Titan are H+, H2+, and O+. B) Finite gyroradius effects are apparent in ambient 0 as the result of its interaction with Titan s atmosphere. C) The principal pickup ions are composed of H+, H2+, CH4+ and N2+. D) There is clear evidence of slowing down of the ambient plasma due to pickup ion mass loading; and, as the ionopause~ is approached, heavier pickup ions such as N2+ become dominant. The similarities and differences between the magnitudes and structures of the electron densities and temperatures along the three flyby trajectories are described
Published: 2006

41. Evidence for rotationally driven plasma transport in Saturn's magnetosphere

Author: Andrew J. Coates, Abigail Rymer, Michelle F. Thomsen, F. J. Crary, N. André, T. W. Hill, James L. Burch, D. M. Delapp, Gethyn R. Lewis, and D. T. Young
Subjects: Rotation period, Physics, Convection, 010504 meteorology & atmospheric sciences, Plasma sheet, Magnetosphere, Radius, Astrophysics, Geophysics, Plasma, 01 natural sciences, Magnetosphere of Saturn, Saturn, Physics::Space Physics, 0103 physical sciences, General Earth and Planetary Sciences, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: [1] Radial convective transport of plasma in a rotation-dominated magnetosphere implies alternating longitudinal sectors of cooler, denser plasma moving outward and hotter, more tenuous plasma moving inward. The Cassini Plasma Spectrometer (CAPS) has provided dramatic new evidence of this process operating in the magnetosphere of Saturn. The inward transport of hot plasma is accompanied by adiabatic gradient and curvature drift, producing a V-shaped dispersion signature on a linear energy-time plot. Of the many (∼100) such signatures evident during the first two Cassini orbits, we analyze a subset (48) that are sufficiently isolated to allow determination of their ages, widths, and injection locations. Ages are typically
Published: 2005

42. Plasma electrons above Saturn's main rings: CAPS observations

Author: Abigail Rymer, Edward C. Sittler, F. J. Crary, R. L. Tokar, D. T. Young, Raúl A. Baragiola, Gethyn R. Lewis, Robert E. Johnson, Andrew J. Coates, Sylvestre Maurice, and H. J. McAndrews
Subjects: Physics, Mathematics::Commutative Algebra, Field line, Rings of Saturn, Magnetosphere, Electron, Ring (chemistry), Geophysics, Saturn, Magnetosphere of Saturn, Physics::Space Physics, General Earth and Planetary Sciences, Astrophysics::Earth and Planetary Astrophysics, Ionosphere, Atomic physics
Abstract: We present observations of thermal ( similar to 0.6 - 100eV) electrons observed near Saturn's main rings during Cassini's Saturn Orbit Insertion (SOI) on 1 July 2004. We find that the intensity of electrons is broadly anticorrelated with the ring optical depth at the magnetic footprint of the field line joining the spacecraft to the rings. We see enhancements corresponding to the Cassini division and Encke gap. We suggest that some of the electrons are generated by photoemission from ring particle surfaces on the illuminated side of the rings, the far side from the spacecraft. Structure in the energy spectrum over the Cassini division and A-ring may be related to photoelectron emission followed by acceleration, or, more likely, due to photoelectron production in the ring atmosphere or ionosphere.
Published: 2005

43. Preliminary results on Saturn's inner plasmasphere as observed by Cassini: Comparison with Voyager

Author: Edward C. Sittler, Daniel B. Reisenfeld, Abigail Rymer, David J. McComas, Andrew J. Coates, M. K. Dougherty, Michelle F. Thomsen, Dennis J. Chornay, F. J. Crary, M. Shappirio, David G. Simpson, D. T. Young, N. André, Robert E. Johnson, and Howard Smith
Subjects: Physics, Electron density, 010504 meteorology & atmospheric sciences, Proton, Magnetosphere, Plasmasphere, 01 natural sciences, 7. Clean energy, Geophysics, 13. Climate action, Saturn, Magnetosphere of Saturn, Physics::Space Physics, 0103 physical sciences, General Earth and Planetary Sciences, Astrophysics::Earth and Planetary Astrophysics, Atomic physics, Enceladus, 010303 astronomy & astrophysics, Ring current, 0105 earth and related environmental sciences
Abstract: [1] We present an analysis of Saturn's inner plasmasphere as observed by the Cassini Plasma Spectrometer (CAPS) experiment during Cassini's initial entry into Saturn's magnetosphere when the spacecraft was inserted into orbit around Saturn. The ion fluxes are divided into two sub-groups: protons and water group ions. We present the relative amounts of these two groups and the first estimates of their fluid parameters: ion density, flow velocity and temperature. We also compare this data with electron plasma measurements. Within the plasmasphere and inside of Enceladus' orbit, water group ions are about a factor of ∼10 greater than protons in number with number densities exceeding 40 cm−3. Within this inner region the spacecraft acquires a negative potential so that the electron density is underestimated. The electron and proton temperatures, which could not be measured in this region by Voyager, are T ∼ 2 eV at L ∼ 3. Also, within this inner region the protons, because of a negative spacecraft potential, appear to be super-corotating. By enforcing the condition that protons and water group ions are co-moving we may be able to acquire an independent estimate of the spacecraft potential relative to that estimated when comparing ion-electron measurements. Using our estimates of plasma properties, we estimate the importance of the rotating plasma on the stress balance equation for the inner magnetosphere and corresponding portion of the ring current.
Published: 2005

44. Analysis of plasma waves observed in the inner Saturn magnetosphere

Author: Abigail Rymer, Andrew J. Coates, Ondrej Santolik, D. A. Gurnett, George Hospodarsky, and John Menietti
Subjects: Atmospheric Science, Field line, Astrophysics::High Energy Astrophysical Phenomena, Population, Cyclotron, Magnetosphere, Electron, law.invention, Optics, Physics::Plasma Physics, law, Saturn, Earth and Planetary Sciences (miscellaneous), lcsh:Science, education, Physics, education.field_of_study, business.industry, lcsh:QC801-809, Geology, Astronomy and Astrophysics, Plasma, lcsh:QC1-999, Magnetic field, lcsh:Geophysics. Cosmic physics, Space and Planetary Science, Physics::Space Physics, lcsh:Q, Atomic physics, business, lcsh:Physics
Abstract: Plasma waves observed in the Saturn magnetosphere provide an indication of the plasma population present in the rotationally dominated inner magnetosphere. Electrostatic cyclotron emissions often with harmonics and whistler mode emission are a common feature of Saturn's inner magnetosphere. The electron observations for a region near 5 RS outside and near a plasma injection region indicate a cooler low-energy (E>1000 eV) more pancake or butterfly distribution. We model the electron plasma distributions to conduct a linear dispersion analysis of the wave modes. The results suggest that the electrostatic electron cyclotron emissions can be generated by phase space density gradients associated with a loss cone that may be up to 20° wide. This loss cone is sometimes, but not always, observed because the field of view of the electron detectors does not include the magnetic field line at the time of the observations. The whistler mode emission can be generated by the pancake-like distribution and temperature anisotropy (T⊥/T||>1) of the warmer plasma population.

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