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108 results on '"Nordheim, T."'

1. Exploring Fundamental Particle Acceleration and Loss Processes in Heliophysics through an Orbiting X-ray Instrument in the Jovian System

Author

Dunn, W., Berland, G., Roussos, E., Clark, G., Kollmann, P., Turner, D., Feldman, C., Stallard, T., Branduardi-Raymont, G., Woodfield, E. E., Rae, I. J., Ray, L. C., Carter, J. A., Lindsay, S. T., Yao, Z., Marshall, R., A., A. N. Jaynes, Ezoe, Y., Numazawa, M., Hospodarsky, G. B., Wu, X., Weigt, D. M., Jackman, C. M., Mori, K., Nénon, Q., Desai, R. T, Blum, L. W., Nordheim, T. A., Ness, J. U., Bodewits, D., Kimura, T., Li, W., Smith, H. T., Millas, D., Wibisono, A. D., Achilleos, N., Koutroumpa, D., McEntee, S. C., Collier, H., Bhardwaj, A., Martindale, A., Wolk, S. J., Badman, S. V., and Kraft, R. P.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Physics - Space Physics
Abstract

Jupiter's magnetosphere is considered to be the most powerful particle accelerator in the Solar System, accelerating electrons from eV to 70 MeV and ions to GeV energies. How electromagnetic processes drive energy and particle flows, producing and removing energetic particles, is at the heart of Heliophysics. Particularly, the 2013 Decadal Strategy for Solar and Space Physics was to "Discover and characterize fundamental processes that occur both within the heliosphere and throughout the universe". The Jovian system offers an ideal natural laboratory to investigate all of the universal processes highlighted in the previous Decadal. The X-ray waveband has been widely used to remotely study plasma across astrophysical systems. The majority of astrophysical emissions can be grouped into 5 X-ray processes: fluorescence, thermal/coronal, scattering, charge exchange and particle acceleration. The Jovian system offers perhaps the only system that presents a rich catalog of all of these X-ray emission processes and can also be visited in-situ, affording the special possibility to directly link fundamental plasma processes with their resulting X-ray signatures. This offers invaluable ground-truths for astrophysical objects beyond the reach of in-situ exploration (e.g. brown dwarfs, magnetars or galaxy clusters that map the cosmos). Here, we show how coupling in-situ measurements with in-orbit X-ray observations of Jupiter's radiation belts, Galilean satellites, Io Torus, and atmosphere addresses fundamental heliophysics questions with wide-reaching impact across helio- and astrophysics. New developments like miniaturized X-ray optics and radiation-tolerant detectors, provide compact, lightweight, wide-field X-ray instruments perfectly suited to the Jupiter system, enabling this exciting new possibility., Comment: A White Paper for the 2024-2033 Solar and Space Physics (Heliophysics) Decadal Survey

Published
2023

2. In Search of Subsurface Oceans within the Uranian Moons

Author

Cochrane, C. J., Vance, S. D., Nordheim, T. A., Styczinski, M., Masters, A., and Regoli, L. H.

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

The Galileo mission to Jupiter discovered magnetic signatures associated with hidden sub-surface oceans at the moons Europa and Callisto using the phenomenon of magnetic induction. These induced magnetic fields originate from electrically conductive layers within the moons and are driven by Jupiter's strong time-varying magnetic field. The ice giants and their moons are also ideal laboratories for magnetic induction studies. Both Uranus and Neptune have a strongly tilted magnetic axis with respect to their spin axis, creating a dynamic and strongly variable magnetic field environment at the orbits of their major moons. Although Voyager 2 visited the ice giants in the 1980s, it did not pass close enough to any of the moons to detect magnetic induction signatures. However, Voyager 2 revealed that some of these moons exhibit surface features that hint at recent geologically activity, possibly associated with sub-surface oceans. Future missions to the ice giants may therefore be capable of discovering sub-surface oceans, thereby adding to the family of known ocean worlds in our solar system. Here, we assess magnetic induction as a technique for investigating sub-surface oceans within the major moons of Uranus. Furthermore, we establish the ability to distinguish induction responses created by different interior characteristics that tie into the induction response: ocean thickness, conductivity, and depth, and ionospheric conductance. The results reported here demonstrate the possibility of single-pass ocean detection and constrained characterization within the moons of Miranda, Ariel, and Umbriel, and provide guidance for magnetometer selection and trajectory design for future missions to Uranus.

Published
2021
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3. Surface composition and properties of Ganymede: Updates from ground-based observations with the near-infrared imaging spectrometer SINFONI/VLT/ESO

Author

Ligier, N., Paranicas, C., Carter, J., Poulet, F., Calvin, W. M., Nordheim, T. A., Snodgrass, C., and Ferellec, L.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Ganymede's surface exhibits great geological diversity, with old dark terrains, expressed through the surface composition, which is known to be dominated by two constituents: H2O-ice and an unidentified darkening agent. In this paper, new investigations of the composition of Ganymede's surface at global scale are presented. The analyses are derived from the linear spectral modeling of a high spectral resolution dataset, acquired with the near-infrared ground-based integral field spectrometer SINFONI of the VLT. We find that the Oren-Nayar (1994) model, generalizing the Lambert's law for rough surfaces, produces excellent photometric corrections. Modeling confirms that Ganymede's surface composition is dominated by H2O-ice, mostly crystalline, as well as a darkening agent, but it also highlights the necessity of secondary species to better fit the measurements: sulfuric acid hydrate and salts. A latitudinal gradient and a hemispherical dichotomy are the strongest spatial patterns observed for the darkening agent, the H2O-ice, and the sulfuric acid: the darkening agent is the major compound at the equator and mid-latitudes, especially on the trailing hemisphere, while the H2O-ice and the sulfuric acid are mostly located at high latitudes and on the leading hemisphere. This anti-correlation is likely a consequence of the bombardment of the constituents in the Jovian magnetosphere which are more intense at higher latitudes. Furthermore, the modeling confirms that polar caps are enriched in small, fresh, H2O-ice grains while equatorial regions are composed of larger grains. Finally, the spatial distribution of the salts is neither related to the Jovian magnetospheric bombardment nor the craters. These species are mostly detected on bright grooved terrains surrounding darker areas. Endogenous processes, such as freezing of upwelling fluids in the ice shell, may explain this distribution.

Published
2019
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4. Atmospheric Electricity at the Ice Giants

Author

Aplin, K. L., Fischer, G., Nordheim, T. A., Konovalenko, A., Zakharenko, V., and Zarka, P.

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

Lightning was detected by Voyager 2 at Uranus and Neptune, and weaker electrical processes also occur throughout planetary atmospheres from galactic cosmic ray (GCR) ionisation. Lightning is an indicator of convection, whereas electrical processes away from storms modulate cloud formation and chemistry, particularly if there is little insolation to drive other mechanisms. The ice giants appear to be unique in the Solar System in that they are distant enough from the Sun for GCR-related mechanisms to be significant for clouds and climate, yet also convective enough for lightning to occur. This paper reviews observations (both from Voyager 2 and Earth), data analysis and modelling, and considers options for future missions. Radio, energetic particle and magnetic instruments are recommended for future orbiters, and Huygens-like atmospheric electricity sensors for in situ observations. Uranian lightning is also expected to be detectable from terrestrial radio telescopes., Comment: Revised version for Space Science Reviews

Published
2019
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5. Cassini CAPS identification of pickup ion compositions at Rhea

Author

Desai, R. T., Taylor, S. A., Regoli, L. H., Coates, A. J., Nordheim, T. A., Cordiner, M. A., Teolis, B. D., Thomsen, M. F., Johnson, R. E., Jones, G. H., Cowee, M. M., and Waite, J. H.

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

Saturn's largest icy moon, Rhea, hosts a tenuous surface-sputtered exosphere composed primarily of molecular oxygen and carbon dioxide. In this Letter, we examine Cassini Plasma Spectrometer velocity space distributions near Rhea and confirm that Cassini detected nongyrotropic fluxes of outflowing CO$_2^+$ during both the R1 and R1.5 encounters. Accounting for this nongyrotropy, we show that these possess comparable alongtrack densities of $\sim$2$\times$10$^{-3}$ cm$^{-3}$. Negatively charged pickup ions, also detected during R1, are surprisingly shown as consistent with mass 26$\pm$3 u which we suggest are carbon-based compounds, such as CN$^-$, C$_2$H$^-$, C$_2^-$, or HCO$^-$, sputtered from carbonaceous material on the moons surface. These negative ions are calculated to possess alongtrack densities of $\sim$5$\times$10$^{-4}$ cm$^{-3}$ and are suggested to derive from exogenic compounds, a finding consistent with the existence of Rhea's dynamic CO$_2$ exosphere and surprisingly low O$_2$ sputtering yields. These pickup ions provide important context for understanding the exospheric and surface-ice composition of Rhea and of other icy moons which exhibit similar characteristics., Comment: 6 pages, 4 figures, submitted to Geophysical Research Letters on 29th November 2017 and accepted on 24th January 2018

Published
2017
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6. Charged particle interactions at unmagnetized bodies

Author

Nordheim, T. A.

Subjects
523.01
Abstract

The overall theme for the work presented in this thesis is charged particle interactions at solar system bodies which do not possess a strong intrinsic magnetic field. This is the case for the planet Venus and minor bodies, such as comets, exposed to the solar wind as well as moons which orbit inside giant planet magnetospheres. In Chapter 2 I investigate surface charging at Saturn's moon Hyperion, which spends most of its orbit inside Saturn's strong magnetic field, and is thus exposed to the corotating hot plasma of the Saturnian magnetosphere. This discussion is supported by interpretation of charged particle and magnetic field observations by instruments onboard the Cassini spacecraft as well as by theoretical modelling. In Chapter 3 I extend the work on surface charging to conduct a theoretical study of surface charging effects on the nucleus of comet 67P/Churyumov-Gerasimenko, which is the target of the currently ongoing Rosetta mission operated by the European Space Agency. In Chapter 4 I present an analysis of electron observations made by the Venus Express spacecraft as it carried out a series of maneuvers which took the spacecraft deep within the Venusian ionosphere, to altitudes not previously sampled by a modern plasma instrument. In Chapters 5 and 6 I present the results of modelling of high energy cosmic ray interactions with the Venusian atmosphere, both due to the constant background of Galactic Cosmic Rays (GCR) as well as sporadic Solar Energetic Particle (SEP) events. This includes a study of the possible effects that extreme SEP events, as exemplified by the Carrington event of 1859, may have on atmospheric ionization rates.

Published
2016

10. Jupiter’s radiation belts as a target for NASA’s Heliophysics Division

Author

Kollmann, P., primary, Allanson, O., additional, Arruda, L., additional, Berland, G., additional, Blum, L. W., additional, Bortnik, J., additional, Cao, X., additional, Chen, T. Y., additional, Clark, G., additional, Cohen, I., additional, Cooper, J. F., additional, Crary, F., additional, Desai, R. T., additional, Dialynas, K., additional, Drozdov, A., additional, Dudnik, O. V., additional, Dunn, W. R., additional, Hospodarsky, G. B., additional, Huybrighs, H., additional, Jackman, C. M., additional, Jaynes, A. N., additional, Jun, I., additional, Khurana, K. K., additional, Kraft, R., additional, Kronberg, E. A., additional, Lejosne, S., additional, Li, W., additional, Li, X., additional, Liuzzo, L., additional, Ma, Q., additional, Marshall, R., additional, Mauk, B., additional, Nénon, Q., additional, Nordheim, T. A., additional, Paranicas, C., additional, Plainaki, C. C., additional, Regoli, L. H., additional, Roussos, E., additional, Shprits, Y., additional, Siecard, A., additional, Simon, S., additional, Smith, H. T., additional, Sorathia, K., additional, Spence, H. E., additional, Sulaiman, A., additional, Sun, Y., additional, Tu, W., additional, Turner, D. L., additional, Usanova, M. E., additional, Williams, P., additional, Woodfield, E. E., additional, Wu, X., additional, and Yuan, C.-J., additional

Published
2023
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14. An Exploration Strategy for Europa

Author

Cable, M, Hofgartner, J, Tan-Wang, G, Hofmann, A, Nordheim, T, Cameron, M, Craft, K, Pitesky, J, Scully, J, Hand, K, and Phillips, Cynthia

Published
2020

15. An Exploration Strategy for Europa

Author

Phillips, Cynthia, Hand, K, Scully, J, Pitesky, J, Craft, K, Cameron, M, Nordheim, T, Hofmann, A, Tan-Wang, G, Hofgartner, J, and Cable, M

Published
2020

21. Energetic Electrons Near Europa From Juno JEDI Data.

Author

Paranicas, C., Mauk, B. H., Clark, G., Kollmann, P., Westlake, J., Hibbitts, K., Nordheim, T., Hand, K., Brennan, M., Connerney, J. E. P., and Bolton, S.

Subjects
PARTICLE detectors, OPTICAL remote sensing, JUNO (Space probe), ELECTRONS, EUROPA (Satellite), CHEMICAL weathering
Abstract

Optical remote sensing observations have suggested that the top layer of Europa's icy surface is heavily affected by external weathering agents. To model and understand these effects, it is necessary to characterize the environment as fully as possible. In this paper, we focus on one agent in the environment (energetic electrons). We show Juno electron data from its 2022 Europa flyby and other time periods. While the Juno sensor used here (Jupiter Energetic Particle Detector Instrument) was not designed to obtain high quality electron data in an intense radiation environment, it is possible to extract information such as how Europa blocks energetic particles from accessing some of the surrounding space. The decrease in charged particle flux in Europa's wake provides an upper limit on the precipitation fluxes of the same particles. We also report that electron pitch angle distributions near Europa for the single energy channel considered here are time variable and not isotropic. Plain Language Summary: We present energetic electron data obtained when the Juno spacecraft crossed the plasma wake of the moon Europa in 2022. A major goal of this work is to estimate the amount of blockage of MeV electrons near the moon to inform radiation estimates for future Europa orbiters and landers. While the Jupiter Energetic Particle Detector Instrument does not directly detect particles between 1 and 20 MeV, using knowledge gained since the instrument began obtaining data we were able to estimate that about 80% of the particles in question are blocked by Europa in its wake at low altitude. Research on the weathering of Europa's surface by electrons is also discussed. Key Points: Jupiter Energetic Particle Detector Instrument electron data relevant to Europa are presentedWe estimate Europa's blockage causes an ∼80% reduction of ∼1–20 MeV electrons in the immediate plasma wakePitch angle distributions are computed from 70 keV electron data and show time variability [ABSTRACT FROM AUTHOR]

Published
2023
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22. Exploring Fundamental Particle Acceleration and Loss Processes in Heliophysics through an Orbiting X-ray Instrument in the Jovian System (A White Paper for the 2024-2033 Solar and Space Physics (Heliophysics) Decadal Survey)

Author

Dunn, W, Berland, G, Roussos, E, Clark, G, Kollmann, P, Turner, D, Feldman, C, Stallard, T, Branduardi-Raymont, G, Woodfield, E, Rae, I, Ray, L, Carter, J, Lindsay, S, Yao, Z, Marshall, R, Jaynes, A, Ezoe, Y, Numazawa, M, Hospodarsky, G, Wu, X, Weigt, D, Jackman, C, Mori, K, Nénon, Quentin, Desai, R, Blum, L, Nordheim, T, Ness, J, Bodewits, D, Kimura, T, Li, W, Smith, H, Millas, D, Wibisono, A, Achilleos, N, Koutroumpa, Dimitra, Mcentee, S, Collier, H, Bhardwaj, A, Martindale, A, Wolk, S, Badman, S, Kraft, R, University College of London [London] (UCL), Centre for Planetary Sciences [UCL/Birkbeck] (CPS), University of Colorado [Boulder], 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), University of Leicester, Mullard Space Science Laboratory (MSSL), British Antarctic Survey (BAS), Natural Environment Research Council (NERC), University of Northumbria at Newcastle [United Kingdom], Lancaster University, Chinese Academy of Sciences [Beijing] (CAS), University of Iowa [Iowa City], Tokyo Metropolitan University [Tokyo] (TMU), Université de Genève = University of Geneva (UNIGE), Dublin Institute for Advanced Studies (DIAS), Columbia University [New York], Institut de recherche en astrophysique et planétologie (IRAP), 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), Imperial College London, University of Warwick [Coventry], Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Auburn University (AU), Tokyo University of Science [Tokyo], Boston University [Boston] (BU), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Applied Sciences and Arts Northwestern Switzerland (FHNW), Physical Research Laboratory [Ahmedabad] (PRL), Indian Space Research Organisation (ISRO), Smithsonian Astrophysical Observatory, and Smithsonian Institution

Subjects
[SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR]
Published
2023

23. Driver of Energetic Electron Precipitation in the Vicinity of Ganymede

Author

Li, W., primary, Ma, Q., additional, Shen, X.‐C., additional, Zhang, X.‐J., additional, Mauk, B. H., additional, Clark, G., additional, Allegrini, F., additional, Kurth, W. S., additional, Hospodarsky, G. B., additional, Sulaiman, A., additional, Nordheim, T. A., additional, and Bolton, S. J., additional

Published
2022
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24. The science case for an orbital mission to Uranus: Exploring the origins and evolution of ice giant planets

Author

Arridge, C.S., Achilleos, N., Agarwal, J., Agnor, C.B., Ambrosi, R., André, N., Badman, S.V., Baines, K., Banfield, D., Barthélémy, M., Bisi, M.M., Blum, J., Bocanegra-Bahamon, T., Bonfond, B., Bracken, C., Brandt, P., Briand, C., Briois, C., Brooks, S., Castillo-Rogez, J., Cavalié, T., Christophe, B., Coates, A.J., Collinson, G., Cooper, J.F., Costa-Sitja, M., Courtin, R., Daglis, I.A., de Pater, I., Desai, M., Dirkx, D., Dougherty, M.K., Ebert, R.W., Filacchione, G., Fletcher, L.N., Fortney, J., Gerth, I., Grassi, D., Grodent, D., Grün, E., Gustin, J., Hedman, M., Helled, R., Henri, P., Hess, S., Hillier, J.K., Hofstadter, M.H., Holme, R., Horanyi, M., Hospodarsky, G., Hsu, S., Irwin, P., Jackman, C.M., Karatekin, O., Kempf, S., Khalisi, E., Konstantinidis, K., Krüger, H., Kurth, W.S., Labrianidis, C., Lainey, V., Lamy, L.L., Laneuville, M., Lucchesi, D., Luntzer, A., MacArthur, J., Maier, A., Masters, A., McKenna-Lawlor, S., Melin, H., Milillo, A., Moragas-Klostermeyer, G., Morschhauser, A., Moses, J.I., Mousis, O., Nettelmann, N., Neubauer, F.M., Nordheim, T., Noyelles, B., Orton, G.S., Owens, M., Peron, R., Plainaki, C., Postberg, F., Rambaux, N., Retherford, K., Reynaud, S., Roussos, E., Russell, C.T., Rymer, A.M., Sallantin, R., Sánchez-Lavega, A., Santolik, O., Saur, J., Sayanagi, K.M., Schenk, P., Schubert, J., Sergis, N., Sittler, E.C., Smith, A., Spahn, F., Srama, R., Stallard, T., Sterken, V., Sternovsky, Z., Tiscareno, M., Tobie, G., Tosi, F., Trieloff, M., Turrini, D., Turtle, E.P., Vinatier, S., Wilson, R., and Zarka, P.

Published
2014
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25. Observations of a Solar Energetic Particle Event From Inside and Outside the Coma of Comet 67P

Author

Wellbrock, A., primary, Jones, G. H., additional, Dresing, N., additional, Coates, A. J., additional, Simon Wedlund, C., additional, Nilsson, H., additional, Sanchez‐Cano, B., additional, Palmerio, E., additional, Turc, L., additional, Myllys, M., additional, Henri, P., additional, Goetz, C., additional, Witasse, O., additional, Nordheim, T. A., additional, and Mandt, K., additional

Published
2022
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26. The in-situ exploration of Jupiter's radiation belts

Author

Roussos, E., Allanson, O., Andre, N., Bertucci, B., Branduardi-Raymont, G., Clark, G., Dialynas, K., Dandouras, I., Desai, R.T., Futaana, Y., Gkioulidou, M., Jones, G.H., Kollmann, P., Kotova, A., Kronberg, E.A., Krupp, N., Murakami, G., Nenon, Q., Nordheim, T., Palmaerts, B., Plainaki, C., Rae, J., Santos-Costa, D., Sarris, T., Shprits, Y., Sulaiman, A., Woodfield, E., Wu, X., Yao, Z.H., Roussos, E., Allanson, O., Andre, N., Bertucci, B., Branduardi-Raymont, G., Clark, G., Dialynas, K., Dandouras, I., Desai, R.T., Futaana, Y., Gkioulidou, M., Jones, G.H., Kollmann, P., Kotova, A., Kronberg, E.A., Krupp, N., Murakami, G., Nenon, Q., Nordheim, T., Palmaerts, B., Plainaki, C., Rae, J., Santos-Costa, D., Sarris, T., Shprits, Y., Sulaiman, A., Woodfield, E., Wu, X., and Yao, Z.H.

Abstract

Jupiter has the most complex and energetic radiation belts in our Solar System and one of the most challenging space environments to measure and characterize in-depth. Their hazardous environment is also a reason why so many spacecraft avoid flying directly through their most intense regions, thus explaining how Jupiter's radiation belts have kept many of their secrets so well hidden, despite having been studied for decades. In this paper we argue why these secrets are worth unveiling. Jupiter's radiation belts and the vast magnetosphere that encloses them constitute an unprecedented physical laboratory, suitable for interdisciplinary and novel scientific investigations: from studying fundamental high energy plasma physics processes which operate throughout the Universe, such as adiabatic charged particle acceleration and nonlinear wave-particle interactions, to exploiting the astrobiological consequences of energetic particle radiation. The in-situ exploration of the uninviting environment of Jupiter's radiation belts presents us with many challenges in mission design, science planning, instrumentation, and technology. We address these challenges by reviewing the different options that exist for direct and indirect observations of this unique system. We stress the need for new instruments, the value of synergistic Earth and Jupiter-based remote sensing and in-situ investigations, and the vital importance of multi-spacecraft in-situ measurements. While simultaneous, multi-point in-situ observations have long become the standard for exploring electromagnetic interactions in the inner Solar System, they have never taken place at Jupiter or any strongly magnetized planet besides Earth. We conclude that a dedicated multi-spacecraft mission to Jupiter is an essential and obvious way forward for exploring the planet's radiation belts. Besides guaranteeing numerous discoveries and huge leaps in our understanding of radiation belt systems, such a mission would also enable u

Published
2022

27. Science Goals and Mission Architecture of the Europa Lander Mission Concept

Author

Hand, K. P., primary, Phillips, C. B., additional, Murray, A., additional, Garvin, J. B., additional, Maize, E. H., additional, Gibbs, R. G., additional, Reeves, G., additional, Martin, A. M. San, additional, Tan-Wang, G. H., additional, Krajewski, J., additional, Hurst, K., additional, Crum, R., additional, Kennedy, B. A., additional, McElrath, T. P., additional, Gallon, J. C., additional, Sabahi, D., additional, Thurman, S. W., additional, Goldstein, B., additional, Estabrook, P., additional, Lee, S. W., additional, Dooley, J. A., additional, Brinckerhoff, W. B., additional, Edgett, K. S., additional, German, C. R., additional, Hoehler, T. M., additional, Hörst, S. M., additional, Lunine, J. I., additional, Paranicas, C., additional, Nealson, K., additional, Smith, D. E., additional, Templeton, A. S., additional, Russell, M. J., additional, Schmidt, B., additional, Christner, B., additional, Ehlmann, B., additional, Hayes, A., additional, Rhoden, A., additional, Willis, P., additional, Yingst, R. A., additional, Craft, K., additional, Cameron, M. E., additional, Nordheim, T., additional, Pitesky, J., additional, Scully, J., additional, Hofgartner, J., additional, Sell, S. W., additional, Barltrop, K. J., additional, Izraelevitz, J., additional, Brandon, E. J., additional, Seong, J., additional, Jones, J.-P., additional, Pasalic, J., additional, Billings, K. J., additional, Ruiz, J. P., additional, Bugga, R. V., additional, Graham, D., additional, Arenas, L. A., additional, Takeyama, D., additional, Drummond, M., additional, Aghazarian, H., additional, Andersen, A. J., additional, Andersen, K. B., additional, Anderson, E. W., additional, Babuscia, A., additional, Backes, P. G., additional, Bailey, E. S., additional, Balentine, D., additional, Ballard, C. G., additional, Berisford, D. F., additional, Bhandari, P., additional, Blackwood, K., additional, Bolotin, G. S., additional, Bovre, E. A., additional, Bowkett, J., additional, Boykins, K. T., additional, Bramble, M. S., additional, Brice, T. M., additional, Briggs, P., additional, Brinkman, A. P., additional, Brooks, S. M., additional, Buffington, B. B., additional, Burns, B., additional, Cable, M. L., additional, Campagnola, S., additional, Cangahuala, L. A., additional, Carr, G. A, additional, Casani, J. R., additional, Chahat, N. E., additional, Chamberlain-Simon, B. K., additional, Cheng, Y., additional, Chien, S. A., additional, Cook, B. T., additional, Cooper, M., additional, DiNicola, M., additional, Clement, B., additional, Dean, Z., additional, Cullimore, E. A., additional, Curtis, A. G., additional, Croix, J-P. de la, additional, Pasquale, P. Di, additional, Dodd, E. M., additional, Dubord, L. A., additional, Edlund, J. A., additional, Ellyin, R., additional, Emanuel, B., additional, Foster, J. T., additional, Ganino, A. J., additional, Garner, G. J., additional, Gibson, M. T., additional, Gildner, M., additional, Glazebrook, K. J., additional, Greco, M. E., additional, Green, W. M., additional, Hatch, S. J., additional, Hetzel, M. M., additional, Hoey, W. A., additional, Hofmann, A. E., additional, Ionasescu, R., additional, Jain, A., additional, Jasper, J. D., additional, Johannesen, J. R., additional, Johnson, G. K., additional, Jun, I., additional, Katake, A. B., additional, Kim-Castet, S. Y., additional, Kim, D. I., additional, Kim, W., additional, Klonicki, E. F., additional, Kobeissi, B., additional, Kobie, B. D., additional, Kochocki, J., additional, Kokorowski, M., additional, Kosberg, J. A., additional, Kriechbaum, K., additional, Kulkarni, T. P., additional, Lam, R. L., additional, Landau, D. F., additional, Lattimore, M. A., additional, Laubach, S. L., additional, Lawler, C. R., additional, Lim, G., additional, Lin, J. Y, additional, Litwin, T. E., additional, Lo, M. W., additional, Logan, C. A., additional, Maghasoudi, E., additional, Mandrake, L., additional, Marchetti, Y., additional, Marteau, E., additional, Maxwell, K. A., additional, Namee, J. B. Mc, additional, Mcintyre, O., additional, Meacham, M., additional, Melko, J. P., additional, Mueller, J., additional, Muliere, D. A., additional, Mysore, A., additional, Nash, J., additional, Ono, H., additional, Parker, J. M., additional, Perkins, R. C., additional, Petropoulos, A. E, additional, Gaut, A., additional, Gomez, M. Y. Piette, additional, Casillas, R. P., additional, Preudhomme, M., additional, Pyrzak, G., additional, Rapinchuk, J., additional, Ratliff, J. M., additional, Ray, T. L., additional, Roberts, E. T., additional, Roffo, K., additional, Roth, D. C., additional, Russino, J. A., additional, Schmidt, T. M., additional, Schoppers, M. J., additional, Senent, J. S., additional, Serricchio, F., additional, Sheldon, D. J., additional, Shiraishi, L. R., additional, Shirvanian, J., additional, Siegel, K. J., additional, Singh, G., additional, Sirota, A. R., additional, Skulsky, E. D., additional, Stehly, J. S., additional, Strange, N. J., additional, Stevens, S. U., additional, Sunada, E. T., additional, Tepsuporn, S. P., additional, Tosi, L. P. C., additional, Trawny, N., additional, Uchenik, I., additional, Verma, V., additional, Volpe, R. A., additional, Wagner, C. T., additional, Wang, D., additional, Willson, R. G., additional, Wolff, J. L., additional, Wong, A. T., additional, Zimmer, A. K., additional, Sukhatme, K. G., additional, Bago, K. A., additional, Chen, Y., additional, Deardorff, A. M., additional, Kuch, R. S., additional, Lim, C., additional, Syvertson, M. L., additional, Arakaki, G. A., additional, Avila, A., additional, DeBruin, K. J., additional, Frick, A., additional, Harris, J. R., additional, Heverly, M. C., additional, Kawata, J. M., additional, Kim, S.-K., additional, Kipp, D. M., additional, Murphy, J., additional, Smith, M. W., additional, Spaulding, M. D., additional, Thakker, R., additional, Warner, N. Z., additional, Yahnker, C. R., additional, Young, M. E., additional, Magner, T., additional, Adams, D., additional, Bedini, P., additional, Mehr, L., additional, Sheldon, C., additional, Vernon, S., additional, Bailey, V., additional, Briere, M., additional, Butler, M., additional, Davis, A., additional, Ensor, S., additional, Gannon, M., additional, Haapala-Chalk, A., additional, Hartka, T., additional, Holdridge, M., additional, Hong, A., additional, Hunt, J., additional, Iskow, J., additional, Kahler, F., additional, Murray, K., additional, Napolillo, D., additional, Norkus, M., additional, Pfisterer, R., additional, Porter, J., additional, Roth, D., additional, Schwartz, P., additional, Wolfarth, L., additional, Cardiff, E. H., additional, Grob, E. W., additional, Adam, J. R., additional, Betts, E., additional, Norwood, J., additional, Heller, M. M., additional, Voskuilen, T., additional, Sakievich, P., additional, Gray, L., additional, Hansen, D. J., additional, Irick, K. W., additional, Hewson, J. C., additional, Lamb, J., additional, Stacy, S. C., additional, Brotherton, C. M., additional, Tappan, A. S, additional, Benally, D., additional, Thigpen, H., additional, Ortiz, E., additional, Sandoval, D., additional, Ison, A. M., additional, Warren, M., additional, Stromberg, P. G., additional, Thelen, P. M., additional, Blasy, B., additional, Nandy, P., additional, Haddad, A. W., additional, Trujillo, L. B., additional, Wiseley, T. H., additional, Bell, S. A., additional, Teske, N. P., additional, Post, C., additional, Torres-Castro, L., additional, Grosso, C., additional, and Wasiolek, M., additional

Published
2022
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29. Driver of Energetic Electron Precipitation in the Vicinity of Ganymede.

Author

Li, W., Ma, Q., Shen, X.‐C., Zhang, X.‐J., Mauk, B. H., Clark, G., Allegrini, F., Kurth, W. S., Hospodarsky, G. B., Sulaiman, A., Nordheim, T. A., and Bolton, S. J.

Subjects
JUNO (Space probe), ELECTRONS, ELECTROMAGNETIC waves, P-waves (Seismology), LATITUDE, MAGNETIC fields
Abstract

The driver of energetic electron precipitation into Ganymede's atmosphere has been an outstanding open problem. During the Juno flyby of Ganymede on 7 June 2021, Juno observed significant downward‐going electron fluxes inside the bounce loss cone of Ganymede's polar magnetosphere. Concurrently, Juno detected intense whistler‐mode waves, both in the quasi‐parallel and highly oblique directions with respect to the magnetic field line. We use quasi‐linear model to quantify energetic electron precipitation driven by quasi‐parallel and very oblique whistler‐mode waves, respectively, in the vicinity of Ganymede. The data‐model comparison indicates that in Ganymede's lower‐latitude (higher‐latitude) polar region, quasi‐parallel whistler‐mode waves play a dominant role in precipitating higher‐energy electrons above ∼100s eV (∼1 keV), whereas highly oblique waves are important for precipitating lower‐energy electrons below 100s eV (∼1 keV). Our result provides new evidence of whistler‐mode waves as a potential primary driver of precipitating energetic electrons into Ganymede's atmosphere. Plain Language Summary: During the Juno flyby of Ganymede on 7 June 2021, the Juno spacecraft detected energetic electrons precipitating into Ganymede's atmosphere. Simultaneously, Juno detected intense electromagnetic whistler‐mode waves in the vicinity of Ganymede. We use a physics‐based model to quantify the role of the observed whistler‐mode waves in energetic electron precipitation. The comparison between the Juno observation and modeling results reveals that whistler‐mode waves potentially play a dominant role in precipitating energetic electrons into Ganymede's atmosphere over a broad energy range from tens of eV to several hundred keV. Our findings are potentially important for understanding the loss process of energetic electrons in Ganymede's magnetosphere, as well as the generation of Ganymede's diffuse aurora. Key Points: We provide new evidence of whistler‐mode waves as a potential primary driver of precipitating energetic electrons into Ganymede's atmosphereThis finding is potentially important for the generation of aurora and the loss of energetic electrons in the vicinity of GanymedeJuno observations and quasi‐linear modeling are used to quantify energetic electron precipitation driven by whistler‐mode waves [ABSTRACT FROM AUTHOR]

Published
2023
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31. Triton: Fascinating Moon, Likely Ocean World, Compelling Destination!

Author

Hansen, Candice J., primary, Castillo-Rogez, J., additional, Grundy, W., additional, Hofgartner, J. D., additional, Martin, E. S., additional, Mitchell, K., additional, Nimmo, F., additional, Nordheim, T. A., additional, Paty, C., additional, Quick, L. C., additional, Roberts, J. H., additional, Runyon, K., additional, Schenk, P., additional, Stern, A., additional, and Umurhan, O., additional

Published
2021
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32. Magnetospheric Studies: A requirement for addressing interdisciplinary mysteries in the Ice Giant systems [White Paper]

Author

Kollmann, P., Allegini, F., Allen, R., André, N., Azari, A., Bagenal, F., Beddingfield, C., Brain, D., Brandt, P., Cao, X., Cartwright, R., Clark, G., Cohen, I., Cooper, J., Crary, F., Leonard, E., Paty, C., Pater, I., Desai, R., DiBraccio, G., Dietrich, W., Dong, C., Ebert, R., Felici, M., Filwett, R., Fischer, G., Gershman, D., Gkioulidou, M., Greathouse, T., Griton, L., Gritsevich, M., Hibbitts, K., Hospodarsky, G., Hue, V., Hunt, G., Huybrighs, H., Imai, M., Jackman, C., Jasinski, J., Jia, X., Jun, I., Kotova, A., Kurth, W., Lamy, L., Lazio, J., Lejosne, S., Louis, C., Masters, A., Mauk, B., Madanian, H., Mandt, K., McNutt, R., Melin, H., Miller, S., Moore, L., Nenon, Q., Neubauer, F., Nordheim, T., Palmaerts, B., Paranicas, C., Phipps, P., Regoli, L., Retherford, K., Roth, L., Roussos, E., Runyon, K., Rymer, A., Saur, J., Santos-Costa, D., SHPRITS, Y., Spilker, L., Stallard, T., Smirnov, A., Soderlund, K., Stanley, S., Sulaiman, A., Szalay, J., Turner, D., Vines, S., Wang, L., Weiss, B., Wicht, J., Wilson, R., and Woodfield, E.

Published
2021

33. The in-situ exploration of Jupiter's radiation belts

Author

Roussos, E., Allanson, O., Andre, N., Bertucci, B., Branduardi-Raymont, G., Clark, G., Dialynas, K., Dandouras, I., Desai, R.T., Futaana, Y., Gkioulidou, M., Jones, G.H., Kollmann, P., Kotova, A., Kronberg, E.A., Krupp, N., Murakami, G., Nenon, Q., Nordheim, T., Palmaerts, B., Plainaki, C., Rae, J., Santos-Costa, D., Sarris, T., Shprits, Y., Sulaiman, A., Woodfield, E., Wu, X., Yao, Z.H., Roussos, E., Allanson, O., Andre, N., Bertucci, B., Branduardi-Raymont, G., Clark, G., Dialynas, K., Dandouras, I., Desai, R.T., Futaana, Y., Gkioulidou, M., Jones, G.H., Kollmann, P., Kotova, A., Kronberg, E.A., Krupp, N., Murakami, G., Nenon, Q., Nordheim, T., Palmaerts, B., Plainaki, C., Rae, J., Santos-Costa, D., Sarris, T., Shprits, Y., Sulaiman, A., Woodfield, E., Wu, X., and Yao, Z.H.

Abstract

Jupiter has the most complex and energetic radiation belts in our Solar System and one of the most challenging space environments to measure and characterize in-depth. Their hazardous environment is also a reason why so many spacecraft avoid flying directly through their most intense regions, thus explaining how Jupiter's radiation belts have kept many of their secrets so well hidden, despite having been studied for decades. In this paper we argue why these secrets are worth unveiling. Jupiter's radiation belts and the vast magnetosphere that encloses them constitute an unprecedented physical laboratory, suitable for interdisciplinary and novel scientific investigations: from studying fundamental high energy plasma physics processes which operate throughout the Universe, such as adiabatic charged particle acceleration and nonlinear wave-particle interactions, to exploiting the astrobiological consequences of energetic particle radiation. The in-situ exploration of the uninviting environment of Jupiter's radiation belts presents us with many challenges in mission design, science planning, instrumentation, and technology. We address these challenges by reviewing the different options that exist for direct and indirect observations of this unique system. We stress the need for new instruments, the value of synergistic Earth and Jupiter-based remote sensing and in-situ investigations, and the vital importance of multi-spacecraft in-situ measurements. While simultaneous, multi-point in-situ observations have long become the standard for exploring electromagnetic interactions in the inner Solar System, they have never taken place at Jupiter or any strongly magnetized planet besides Earth. We conclude that a dedicated multi-spacecraft mission to Jupiter is an essential and obvious way forward for exploring the planet's radiation belts. Besides guaranteeing numerous discoveries and huge leaps in our understanding of radiation belt systems, such a mission would also enable u

Published
2021

34. The Science Case for Spacecraft Exploration of the Uranian SatellitesA Science White Paper for the Planetary Science and Astrobiology Decadal Survey 2023-2032

Author

Cartwright, Richard, Beddingfield, Chloe, Nordheim, T, Elder, C., Grundy, W., Buratti, B., Bramson, A., Sori, M., Pappalardo, R., Neveu, M., Burr, D., Ermakov, A., Roser, J., Castillo-Rogez, J., Showalter, M., Cohen, I., Turtle, E., Hofstadter, M., Leonard, E., Pater, I. de, Patthoff, D.A., Masters, A., Fletcher, L., Ahrens, C., Andres, C., Aplin, K., Arney, G., Baillie, Kevin, Barth, E., Bennett, C., Beyer, R., Bierson, C., Bland, M., Bray, V., Byrne, P., Cabrol, N., Cameron, M., Chanover, N., Cochrane, C., Collins, G., Cook, J., Coustenis, A., Cruikshank, D., Ćuk, M., Daubar, I., Denton, A., DeColibus, D., Dhingra, R., Dong, C., Ferguson, S., Filacchione, G., French, R., Golder, K., Grava, C., Griton, L., Hammond, N., Hayes, A., Hawkins, E., Helfenstein, P., Hendrix, A., Hofmann, A., Holler, B., Holt, T., Howell, S., Howett, C., Hussmann, H., Hsu, H., Izenberg, N., Jacobsen, R., Jha, D., Juanola-Parramon, R., Jun, I., Keane, J., Karkoschka, E., Kattenhorn, S., Kinczyk, M., Kirchoff, M., Klimczak, C., Kollmann, P., Lopes, R., Lucas, M., Lucchetti, A., Martin, E., MacKenzie, S., Moses, J., Mlinar, A. Barr, Moore, J., Nimmo, F., O’Hara, S., Pajola, M., Peel, S., Peterson, G., Pinilla-Alonso, N., Porter, S., Postberg, F., Poston, M., Probst, A., Protopapa, S., Quick, L., Ricca, A., Roberge, A., Roberts, J., Robbins, S., Rodriguez, S., Runyon, K., Schenk, P., Schneegurt, M., Scipioni, F., Shusterman, M., Singer, K., Soderlund, K., Spencer, J., Spilker, L., Stephan, K., Stryk, T., Tiscareno, M., Tomlinson, T., Tosi, F., Tortora, P., Umurhan, O., Vance, S., Verbiscer, A., Walker, C., Weiss, B., White, O., Search for Extraterrestrial Intelligence Institute (SETI), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

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

A Science White Paper for the Planetary Science and Astrobiology Decadal Survey 2023-2032; Uranian satellites imaged by Voyager 2, not shown to scale (NASA/JPL-Caltech/USGS, [55]). Puck (top left), Miranda (top middle), Ariel (top right), Umbriel (bottom left), Titania (bottom middle), and Oberon (bottom right).

Published
2020

35. Science of the Europa Lander Mission Concept

Author

Hand, Kevin, primary, Murray, A. E., additional, Garvin, J. B., additional, Brinckerhoff, W. B., additional, Christner, B., additional, Edgett, K. E., additional, Ehlmann, B., additional, German, C., additional, Hayes, A., additional, Hoehler, T., additional, Hörst, S., additional, Lunine, J., additional, Nealson, K., additional, Paranicas, C., additional, Schmidt, B. E., additional, Smith, D. E., additional, Rhoden, A., additional, Russell, M., additional, Templeton, A., additional, Willis, P., additional, Yingst, A., additional, Phillips, C. B., additional, Cable, M. L., additional, Craft, K. L., additional, Nordheim, T. A., additional, Pitesky, J., additional, Cameron, M., additional, Hofgartner, J. D., additional, Hofmann, A. E., additional, Scully, J., additional, Kosberg, J., additional, Foster, J., additional, and Klonicki, E., additional

Published
2021
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36. Magnetospheric Studies: A requirement for addressing interdisciplinary mysteries in the Ice Giant systems

Author

Kollmann, Peter, primary, Allegini, F., additional, Allen, R. C., additional, André, N., additional, Azari, A. R., additional, Bagenal, F., additional, Beddingfield, C. B., additional, Brain, D., additional, Brandt, P., additional, Cao, X., additional, Cartwright, R. J., additional, Clark, G., additional, Cohen, I., additional, Cooper, J. F., additional, Crary, F., additional, Leonard, E. J., additional, Paty, C., additional, Pater, I. de, additional, Desai, R. T., additional, DiBraccio, G. A., additional, Dietrich, W., additional, Dong, C., additional, Ebert, R. W., additional, Felici, M., additional, Filwett, R. J., additional, Fischer, G., additional, Gershman, D. J., additional, Gkioulidou, M., additional, Greathouse, T. K., additional, Griton, L., additional, Gritsevich, M., additional, Hibbitts, K., additional, Hospodarsky, G., additional, Hue, V., additional, Hunt, G., additional, Huybrighs, H. L. F., additional, Imai, M., additional, Jackman, C. M., additional, Jasinski, J. M., additional, Jia, X., additional, Jun, I., additional, Kotova, A., additional, Kurth, W. S., additional, Lamy, L., additional, Lazio, J., additional, Lejosne, S., additional, Louis, C., additional, Masters, A., additional, Mauk, B., additional, Madanian, H., additional, Mandt, K. E., additional, Jr., R. McNutt,, additional, Melin, H., additional, Miller, S., additional, Moore, L., additional, Nenon, Q., additional, Neubauer, F. M., additional, Nordheim, T., additional, Palmaerts, B., additional, Paranicas, C., additional, Phipps, P., additional, Regoli, L., additional, Retherford, K., additional, Roth, L., additional, Roussos, E., additional, Runyon, K. D., additional, Rymer, A., additional, Saur, J., additional, Santos-Costa, D., additional, Shprits, Y. Y., additional, Spilker, L. J., additional, Stallard, T., additional, Smirnov, A. G., additional, Soderlund, K., additional, Stanley, S., additional, Sulaiman, A. H., additional, Szalay, J. R., additional, Turner, D. L., additional, Vines, S., additional, Wang, L., additional, Weiss, B., additional, Wicht, J., additional, Wilson, R. J., additional, and Woodfield, E., additional

Published
2021
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38. Solar System Ice Giants: Exoplanets in our Backyard

Author

Rymer, A, Mandt, K, Hurley, D, Lisse, C, Izenberg, N, Smith, HT, Westlake, J, Bunce, E, Arridge, C, Masters, A, Hofstadter, M, Simon, A, Brandt, P, Clark, G, Cohen, I, Allen, R, Vine, S, Hansen, K, Hospodarsky, G, Kurth, W, Romani, P, Lamy, L, Zarka, P, Cao, H, Paty, C, Hedman, M, Roussos, E, Cruikshank, D, Farrell, W, Fieseler, P, Coates, A, Yelle, R, Parkinson, C, Militzer, B, Grodent, D, Kollmann, P, McNutt, R, André, N, Strange, N, Barnes, J, Dones, L, Denk, T, Rathbun, J, Lunine, J, Desai, R, Cochrane, C, Sayanagi, KM, Postberg, F, Ebert, R, Hill, T, Mueller-Wodarg, I, Regoli, L, Pontius, D, Stanley, S, Greathouse, T, Saur, J, Marouf, E, Bergman, J, Higgins, C, Johnson, R, Thomsen, M, Soderlund, K, Jia, X, Wilson, R, Englander, J, Burch, J, Nordheim, T, Grava, C, Baines, K, Quick, L, Russell, C, Cravens, T, Cecconi, B, Aslam, S, Bray, V, Garcia-Sage, K, Richardson, J, Clark, J, Hsu, S, Achterberg, R, Sergis, N, Paganelli, F, Kempf, S, Orton, G, Portyankina, G, Jones, G, Economou, T, Livengood, T, Krimigi, S, Szalay, J, Jackman, C, Valek, P, Lecacheux, A, Colwell, J, Jasinski, J, Tosi, F, Sulaiman, A, Galand, M, Kotova, A, Khurana, K, Kivelson, M, Strobel, D, Radiota, A, Estrada, P, Livi, S, Azari, A, Yates, J, Allegrini, F, Vogt, M, Felici, M, Luhmann, J, Filacchione, G, and Moore, L

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Physics::Space Physics, astro-ph.EP, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Physics::Atmospheric and Oceanic Physics
Abstract

Future remote sensing of exoplanets will be enhanced by a thorough investigation of our solar system Ice Giants (Neptune-size planets). What can the configuration of the magnetic field tell us (remotely) about the interior, and what implications does that field have for the structure of the magnetosphere; energy input into the atmosphere, and surface geophysics (for example surface weathering of satellites that might harbour sub-surface oceans). How can monitoring of auroral emission help inform future remote observations of emission from exoplanets? Our Solar System provides the only laboratory in which we can perform in-situ experiments to understand exoplanet formation, dynamos, systems and magnetospheres.

Published
2019

39. Saturn's open‐closed field line boundary:a Cassini electron survey at Saturn's magnetosphere

Author

Jasinski, Jamie M., Arridge, Chris, Bader, Alexander, Smith, Andrew, Felici, Marianna, Kinrade, Joe, Coates, A.J., Jones, Geraint, Nordheim, T., Gilbert, Lin, Azari, Abigail, Badman, Sarah, Provan, G., Sergis, N., Murphy, Neil, Jasinski, Jamie M., Arridge, Chris, Bader, Alexander, Smith, Andrew, Felici, Marianna, Kinrade, Joe, Coates, A.J., Jones, Geraint, Nordheim, T., Gilbert, Lin, Azari, Abigail, Badman, Sarah, Provan, G., Sergis, N., and Murphy, Neil

Abstract

We investigate the average configuration and structure of Saturn's magnetosphere in the nightside equatorial and high‐latitude regions. Electron data from the Cassini Plasma Spectrometer's Electron Spectrometer (CAPS‐ELS) is processed to produce a signal‐to‐noise ratio for the entire CAPS‐ELS time of operation at Saturn's magnetosphere. We investigate where the signal‐to‐noise ratio falls below 1, to identify regions in the magnetosphere where there is a significant depletion in the electron content. In the nightside equatorial region we use this to find that the most planetward reconnection x‐line location is at 20 – 25 RS downtail from the planet in the midnight to dawn sector. We also find an equatorial dawn‐dusk asymmetry at a radial distance of >20 RS which may indicate the presence of plasma depleted flux tubes returning to the dayside after reconnection in the tail. Furthermore, we find that the high‐latitude magnetosphere is predominantly in a state of constant plasma depletion and located on open field lines. We map the region of high‐latitude magnetosphere that is depleted of electrons to the polar cap to estimate the size and open flux content within the polar caps. The mean open flux content for the northern and southern polar caps are found to be 25±5 and 32±5 GWb, respectively. The average location of the open‐closed field boundary is found at invariant colatitudes of 12.7±0.6° and 14.5±0.6°. The northern boundary is modulated by planetary period oscillations more than the southern boundary.

Published
2019

40. Saturn's open‐closed field line boundary : a Cassini electron survey at Saturn's magnetosphere

Author

Jasinski, Jamie M., Arridge, Chris, Bader, Alexander, Smith, Andrew, Felici, Marianna, Kinrade, Joe, Coates, A.J., Jones, Geraint, Nordheim, T., Gilbert, Lin, Azari, Abigail, Badman, Sarah, Provan, G., Sergis, N., Murphy, Neil, Jasinski, Jamie M., Arridge, Chris, Bader, Alexander, Smith, Andrew, Felici, Marianna, Kinrade, Joe, Coates, A.J., Jones, Geraint, Nordheim, T., Gilbert, Lin, Azari, Abigail, Badman, Sarah, Provan, G., Sergis, N., and Murphy, Neil

Abstract

We investigate the average configuration and structure of Saturn's magnetosphere in the nightside equatorial and high‐latitude regions. Electron data from the Cassini Plasma Spectrometer's Electron Spectrometer (CAPS‐ELS) is processed to produce a signal‐to‐noise ratio for the entire CAPS‐ELS time of operation at Saturn's magnetosphere. We investigate where the signal‐to‐noise ratio falls below 1, to identify regions in the magnetosphere where there is a significant depletion in the electron content. In the nightside equatorial region we use this to find that the most planetward reconnection x‐line location is at 20 – 25 RS downtail from the planet in the midnight to dawn sector. We also find an equatorial dawn‐dusk asymmetry at a radial distance of >20 RS which may indicate the presence of plasma depleted flux tubes returning to the dayside after reconnection in the tail. Furthermore, we find that the high‐latitude magnetosphere is predominantly in a state of constant plasma depletion and located on open field lines. We map the region of high‐latitude magnetosphere that is depleted of electrons to the polar cap to estimate the size and open flux content within the polar caps. The mean open flux content for the northern and southern polar caps are found to be 25±5 and 32±5 GWb, respectively. The average location of the open‐closed field boundary is found at invariant colatitudes of 12.7±0.6° and 14.5±0.6°. The northern boundary is modulated by planetary period oscillations more than the southern boundary.

Published
2019

42. A Qualitative Study of the Experiences of Norwegian Parents of Very Low Birthweight Infants Enrolled in a Randomized Nutritional Trial

Author

Nordheim, T., Anderzen-Carlsson, Agneta, Nakstad, B., Nordheim, T., Anderzen-Carlsson, Agneta, and Nakstad, B.

Abstract

Purpose: The aim of this study was to examine how parents of very low birth weight (VLBW) infants experienced having their newborn infant enrolled in a randomized controlled intervention trial (RCT). Design and Methods: A qualitative descriptive design was used. Data were collected through individual semi-structured interviews with 15 parents of 9 participating VLBW infants. The data were then made the object of an inductive qualitative content analysis. Results: The parents expressed trust in the competence and motivation of the researchers and were confident that participating in the project would do no harm, but instead would potentially benefit their infant. The parents felt privileged for being given the chance to participate, to commit to the project; they were willing to invest their time and effort in the project. Participation could be stressful for the parents, ranging from minor irritation to situations in which they felt overwhelmed and not entirely in control. Many families lived stressful lives, and participation, particularly the follow-up after being discharged, may have added to this. Conclusions: Infant participation in an RCT can be a positive experience, making the parents feel that they are given a chance to both contribute and receive something special. Participation can also be stressful because of conditions both related and unrelated to the RCT. Practice Implications: We identified several issues that researchers in future trials with VLBW infants need to address to minimize parental stress. Recruitment to intervention studies within the immediate period around birth should be avoided, if possible.

Published
2018
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44. Cassini CAPS Identification of Pickup Ion Compositions at Rhea

Author

Desai, R. T., primary, Taylor, S. A., additional, Regoli, L. H., additional, Coates, A. J., additional, Nordheim, T. A., additional, Cordiner, M. A., additional, Teolis, B. D., additional, Thomsen, M. F., additional, Johnson, R. E., additional, Jones, G. H., additional, Cowee, M. M., additional, and Waite, J. H., additional

Published
2018
Full Text
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45. The science case for an orbital mission to Uranus: Exploring the origins and evolution of ice giant planets

Author

Arridge, C.S. Achilleos, N. Agarwal, J. Agnor, C.B. Ambrosi, R. André, N. Badman, S.V. Baines, K. Banfield, D. Barthélémy, M. Bisi, M.M. Blum, J. Bocanegra-Bahamon, T. Bonfond, B. Bracken, C. Brandt, P. Briand, C. Briois, C. Brooks, S. Castillo-Rogez, J. Cavalié, T. Christophe, B. Coates, A.J. Collinson, G. Cooper, J.F. Costa-Sitja, M. Courtin, R. Daglis, I.A. De Pater, I. Desai, M. Dirkx, D. Dougherty, M.K. Ebert, R.W. Filacchione, G. Fletcher, L.N. Fortney, J. Gerth, I. Grassi, D. Grodent, D. Grün, E. Gustin, J. Hedman, M. Helled, R. Henri, P. Hess, S. Hillier, J.K. Hofstadter, M.H. Holme, R. Horanyi, M. Hospodarsky, G. Hsu, S. Irwin, P. Jackman, C.M. Karatekin, O. Kempf, S. Khalisi, E. Konstantinidis, K. Krüger, H. Kurth, W.S. Labrianidis, C. Lainey, V. Lamy, L.L. Laneuville, M. Lucchesi, D. Luntzer, A. MacArthur, J. Maier, A. Masters, A. McKenna-Lawlor, S. Melin, H. Milillo, A. Moragas-Klostermeyer, G. Morschhauser, A. Moses, J.I. Mousis, O. Nettelmann, N. Neubauer, F.M. Nordheim, T. Noyelles, B. Orton, G.S. Owens, M. Peron, R. Plainaki, C. Postberg, F. Rambaux, N. Retherford, K. Reynaud, S. Roussos, E. Russell, C.T. Rymer, A.M. Sallantin, R. Sánchez-Lavega, A. Santolik, O. Saur, J. Sayanagi, K.M. Schenk, P. Schubert, J. Sergis, N. Sittler, E.C. Smith, A. Spahn, F. Srama, R. Stallard, T. Sterken, V. Sternovsky, Z. Tiscareno, M. Tobie, G. Tosi, F. Trieloff, M. Turrini, D. Turtle, E.P. Vinatier, S. Wilson, R. Zarka, P.

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

Giant planets helped to shape the conditions we see in the Solar System today and they account for more than 99% of the mass of the Sun's planetary system. They can be subdivided into the Ice Giants (Uranus and Neptune) and the Gas Giants (Jupiter and Saturn), which differ from each other in a number of fundamental ways. Uranus, in particular is the most challenging to our understanding of planetary formation and evolution, with its large obliquity, low self-luminosity, highly asymmetrical internal field, and puzzling internal structure. Uranus also has a rich planetary system consisting of a system of inner natural satellites and complex ring system, five major natural icy satellites, a system of irregular moons with varied dynamical histories, and a highly asymmetrical magnetosphere. Voyager 2 is the only spacecraft to have explored Uranus, with a flyby in 1986, and no mission is currently planned to this enigmatic system. However, a mission to the uranian system would open a new window on the origin and evolution of the Solar System and would provide crucial information on a wide variety of physicochemical processes in our Solar System. These have clear implications for understanding exoplanetary systems. In this paper we describe the science case for an orbital mission to Uranus with an atmospheric entry probe to sample the composition and atmospheric physics in Uranus' atmosphere. The characteristics of such an orbiter and a strawman scientific payload are described and we discuss the technical challenges for such a mission. This paper is based on a white paper submitted to the European Space Agency's call for science themes for its large-class mission programme in 2013. © 2014 Elsevier Ltd.

Published
2014

46. Unveiling the evolution and formation of icy giants

Author

Dominic, D., Bocanegra, T., Bracken, C., Costa, M., Gerth, I., Konstantinidis, K., Labrianidis, C., Laneuville, M., Luntzer, A., MacArthur , J., Maier, A., Morschhauser, A., Nordheim, T., Sallantin , R., and Tlustos, R.

Subjects
evolution, formation, icy giants
Published
2013

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

Author

Arridge, C. S., Achilleos, N., Agarwal, J., Agnor, C. B., Ambrosi, R., Andre, N., Badman, S. V., Baines, K., Banfield, D., Barthelemy, M., Bisi, M. M., Blum, J., Bocanegra-Bahamon, T., Bonfond, B. ., Bracken, C., Brandt, P., Briand, C., Briois, C., Brooks, S., Castillo-Rogez, J., Cavalie, T., Christophe, B., Coates, A. J., Collinson, G., Cooper, J. F., Costa-Sitja, M., Courtin, R., Daglis, I. A., De Pater, I., Desai, M., Dirkx, D., Dougherty, M. K., Ebert, R. W., Filacchione, G., Fletcher, L. N., Fortney, J., Gerth, I., Grassi, D., Grodent, D., Grun, E., Gustin, J., Hedman, M., Helled, R., Henri, P., Hess, S., Hillier, J. K., Hofstadter, M. H., Holme, R., Horanyi, M., Hospodarsky, G., Hsu, S., Irwin, P., Jackman, C. M., Karatekin, O., Kempf, S., Khalisi, E., Konstantinidis, K., Kruger, H., Kurth, W. S., Labrianidis, C., Lainey, V., Lamy, L. L., Laneuville, M., Lucchesi, D., Luntzer, A., MacArthur, J., Maier, A., Masters, A., McKenna-Lawlor, S., Melin, H., Milillo, A., Moragas-Klostermeyer, G., Morschhauser, A., Moses, J. I., Mousis, O., Nettelmann, N., Neubauer, F. M., Nordheim, T., Noyelles, B., Orton, G. S., Owens, M., Peron, R., Plainaki, C., Postberg, F., Rambaux, N., Retherford, K., Reynaud, S., Roussos, E., Russell, C. T., Rymer, Am., Sallantin, R., Sanchez-Lavega, A., Santolik, O., Saur, J., Sayanagi, Km., Schenk, P., Schubert, J., Sergis, N., Sittler, E. C., Smith, A., Spahn, F., Srama, R., Stallard, T., Sterken, V., Sternovsky, Z., Tiscareno, M., Tobie, G., Tosi, F., Trieloff, M., Turrini, D., Turtle, E. P., Vinatier, S., Wilson, R., Zarkat, P., Arridge, C. S., Achilleos, N., Agarwal, J., Agnor, C. B., Ambrosi, R., Andre, N., Badman, S. V., Baines, K., Banfield, D., Barthelemy, M., Bisi, M. M., Blum, J., Bocanegra-Bahamon, T., Bonfond, B. ., Bracken, C., Brandt, P., Briand, C., Briois, C., Brooks, S., Castillo-Rogez, J., Cavalie, T., Christophe, B., Coates, A. J., Collinson, G., Cooper, J. F., Costa-Sitja, M., Courtin, R., Daglis, I. A., De Pater, I., Desai, M., Dirkx, D., Dougherty, M. K., Ebert, R. W., Filacchione, G., Fletcher, L. N., Fortney, J., Gerth, I., Grassi, D., Grodent, D., Grun, E., Gustin, J., Hedman, M., Helled, R., Henri, P., Hess, S., Hillier, J. K., Hofstadter, M. H., Holme, R., Horanyi, M., Hospodarsky, G., Hsu, S., Irwin, P., Jackman, C. M., Karatekin, O., Kempf, S., Khalisi, E., Konstantinidis, K., Kruger, H., Kurth, W. S., Labrianidis, C., Lainey, V., Lamy, L. L., Laneuville, M., Lucchesi, D., Luntzer, A., MacArthur, J., Maier, A., Masters, A., McKenna-Lawlor, S., Melin, H., Milillo, A., Moragas-Klostermeyer, G., Morschhauser, A., Moses, J. I., Mousis, O., Nettelmann, N., Neubauer, F. M., Nordheim, T., Noyelles, B., Orton, G. S., Owens, M., Peron, R., Plainaki, C., Postberg, F., Rambaux, N., Retherford, K., Reynaud, S., Roussos, E., Russell, C. T., Rymer, Am., Sallantin, R., Sanchez-Lavega, A., Santolik, O., Saur, J., Sayanagi, Km., Schenk, P., Schubert, J., Sergis, N., Sittler, E. C., Smith, A., Spahn, F., Srama, R., Stallard, T., Sterken, V., Sternovsky, Z., Tiscareno, M., Tobie, G., Tosi, F., Trieloff, M., Turrini, D., Turtle, E. P., Vinatier, S., Wilson, R., and Zarkat, P.

Abstract

Giant planets helped to shape the conditions we see in the Solar System today and they account for more than 99% of the mass of the Sun's planetary system. They can be subdivided into the Ice Giants (Uranus and Neptune) and the Gas Giants (Jupiter and Saturn), which differ from each other in a number of fundamental ways. Uranus, in particular is the most challenging to our understanding of planetary formation and evolution, with its large obliquity, low self-luminosity, highly asymmetrical internal field, and puzzling internal structure. Uranus also has a rich planetary system consisting of a system of inner natural satellites and complex ring system, five major natural icy satellites, a system of irregular moons with varied dynamical histories, and a highly asymmetrical magnetosphere. Voyager 2 is the only spacecraft to have explored Uranus, with a flyby in 1986, and no mission is currently planned to this enigmatic system. However, a mission to the uranian system would open a new window on the origin and evolution of the Solar System and would provide crucial information on a wide variety of physicochemical processes in our Solar System. These have clear implications for understanding exoplanetary systems. In this paper we describe the science case for an orbital mission to Uranus with an atmospheric entry probe to sample the composition and atmospheric physics in Uranus' atmosphere. The characteristics of such an orbiter and a strawman scientific payload are described and we discuss the technical challenges for such a mission. This paper is based on a white paper submitted to the European Space Agency's call for science themes for its large-class mission programme in 2013. (C) 2014 Published by Elsevier Ltd.

Published
2014

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

Author

Arridge, C. S., Achilleos, N., Agarwal, J., Agnor, C. B., Ambrosi, R., Andre, N., Badman, S. V., Baines, K., Banfield, D., Barthelemy, M., Bisi, M. M., Blum, J., Bocanegra-Bahamon, T., Bonfond, B. ., Bracken, C., Brandt, P., Briand, C., Briois, C., Brooks, S., Castillo-Rogez, J., Cavalie, T., Christophe, B., Coates, A. J., Collinson, G., Cooper, J. F., Costa-Sitja, M., Courtin, R., Daglis, I. A., De Pater, I., Desai, M., Dirkx, D., Dougherty, M. K., Ebert, R. W., Filacchione, G., Fletcher, L. N., Fortney, J., Gerth, I., Grassi, D., Grodent, D., Grun, E., Gustin, J., Hedman, M., Helled, R., Henri, P., Hess, S., Hillier, J. K., Hofstadter, M. H., Holme, R., Horanyi, M., Hospodarsky, G., Hsu, S., Irwin, P., Jackman, C. M., Karatekin, O., Kempf, S., Khalisi, E., Konstantinidis, K., Kruger, H., Kurth, W. S., Labrianidis, C., Lainey, V., Lamy, L. L., Laneuville, M., Lucchesi, D., Luntzer, A., MacArthur, J., Maier, A., Masters, A., McKenna-Lawlor, S., Melin, H., Milillo, A., Moragas-Klostermeyer, G., Morschhauser, A., Moses, J. I., Mousis, O., Nettelmann, N., Neubauer, F. M., Nordheim, T., Noyelles, B., Orton, G. S., Owens, M., Peron, R., Plainaki, C., Postberg, F., Rambaux, N., Retherford, K., Reynaud, S., Roussos, E., Russell, C. T., Rymer, Am., Sallantin, R., Sanchez-Lavega, A., Santolik, O., Saur, J., Sayanagi, Km., Schenk, P., Schubert, J., Sergis, N., Sittler, E. C., Smith, A., Spahn, F., Srama, R., Stallard, T., Sterken, V., Sternovsky, Z., Tiscareno, M., Tobie, G., Tosi, F., Trieloff, M., Turrini, D., Turtle, E. P., Vinatier, S., Wilson, R., Zarkat, P., Arridge, C. S., Achilleos, N., Agarwal, J., Agnor, C. B., Ambrosi, R., Andre, N., Badman, S. V., Baines, K., Banfield, D., Barthelemy, M., Bisi, M. M., Blum, J., Bocanegra-Bahamon, T., Bonfond, B. ., Bracken, C., Brandt, P., Briand, C., Briois, C., Brooks, S., Castillo-Rogez, J., Cavalie, T., Christophe, B., Coates, A. J., Collinson, G., Cooper, J. F., Costa-Sitja, M., Courtin, R., Daglis, I. A., De Pater, I., Desai, M., Dirkx, D., Dougherty, M. K., Ebert, R. W., Filacchione, G., Fletcher, L. N., Fortney, J., Gerth, I., Grassi, D., Grodent, D., Grun, E., Gustin, J., Hedman, M., Helled, R., Henri, P., Hess, S., Hillier, J. K., Hofstadter, M. H., Holme, R., Horanyi, M., Hospodarsky, G., Hsu, S., Irwin, P., Jackman, C. M., Karatekin, O., Kempf, S., Khalisi, E., Konstantinidis, K., Kruger, H., Kurth, W. S., Labrianidis, C., Lainey, V., Lamy, L. L., Laneuville, M., Lucchesi, D., Luntzer, A., MacArthur, J., Maier, A., Masters, A., McKenna-Lawlor, S., Melin, H., Milillo, A., Moragas-Klostermeyer, G., Morschhauser, A., Moses, J. I., Mousis, O., Nettelmann, N., Neubauer, F. M., Nordheim, T., Noyelles, B., Orton, G. S., Owens, M., Peron, R., Plainaki, C., Postberg, F., Rambaux, N., Retherford, K., Reynaud, S., Roussos, E., Russell, C. T., Rymer, Am., Sallantin, R., Sanchez-Lavega, A., Santolik, O., Saur, J., Sayanagi, Km., Schenk, P., Schubert, J., Sergis, N., Sittler, E. C., Smith, A., Spahn, F., Srama, R., Stallard, T., Sterken, V., Sternovsky, Z., Tiscareno, M., Tobie, G., Tosi, F., Trieloff, M., Turrini, D., Turtle, E. P., Vinatier, S., Wilson, R., and Zarkat, P.

Abstract

Giant planets helped to shape the conditions we see in the Solar System today and they account for more than 99% of the mass of the Sun's planetary system. They can be subdivided into the Ice Giants (Uranus and Neptune) and the Gas Giants (Jupiter and Saturn), which differ from each other in a number of fundamental ways. Uranus, in particular is the most challenging to our understanding of planetary formation and evolution, with its large obliquity, low self-luminosity, highly asymmetrical internal field, and puzzling internal structure. Uranus also has a rich planetary system consisting of a system of inner natural satellites and complex ring system, five major natural icy satellites, a system of irregular moons with varied dynamical histories, and a highly asymmetrical magnetosphere. Voyager 2 is the only spacecraft to have explored Uranus, with a flyby in 1986, and no mission is currently planned to this enigmatic system. However, a mission to the uranian system would open a new window on the origin and evolution of the Solar System and would provide crucial information on a wide variety of physicochemical processes in our Solar System. These have clear implications for understanding exoplanetary systems. In this paper we describe the science case for an orbital mission to Uranus with an atmospheric entry probe to sample the composition and atmospheric physics in Uranus' atmosphere. The characteristics of such an orbiter and a strawman scientific payload are described and we discuss the technical challenges for such a mission. This paper is based on a white paper submitted to the European Space Agency's call for science themes for its large-class mission programme in 2013. (C) 2014 Published by Elsevier Ltd.

Published
2014

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