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  • Journal article
    Southwood DJ, 2016,

    Space in 150 years: From fantasy through fiction to fact and function

    , Aeronautical Journal, Vol: 120, Pages: 201-208, ISSN: 0001-9240

    In the last century and half, space has moved from the realm of fantasy to everyday reality.In parallel the way space has been regarded by the person in the street and the ideas of whataccess to space might be used for have evolved extraordinarily.
  • Journal article
    Goswami BN, Rao S, Sengupta D, Chowdary Set al., 2016,

    Monsoons to Mixing in the Bay of Bengal: Multiscale Air-Sea Interactions and Monsoon Predictability

    , Oceanography, Vol: 29, Pages: 18-27, ISSN: 1042-8275
  • Book chapter
    Badman SV, Branduardi-Raymont G, Galand M, Hess SLG, Krupp N, Lamy L, Melin H, Tao Cet al., 2016,

    Auroral Processes at the Giant Planets: Energy Deposition, Emission Mechanisms, Morphology and Spectra

    , MAGNETODISCS AND AURORAE OF GIANT PLANETS, Editors: Szego, Achilleos, Arridge, Badman, Delamere, Grodent, Kivelson, Louarn, Publisher: SPRINGER, Pages: 99-179, ISBN: 978-1-4939-3394-5
  • Journal article
    group ISOSISOS, Holt P, Rhodes A, Wilson M, Ferguson M, Macmahon M, Gillespie D, Phillips K, Reynolds J, Kerridge R, Bennett M, Stewart M, Hartmann A, Jacobs T, Ortega D, Dias F, Machado M, Garcia J, Lopes M, Carr A, Yu HC, Rowe B, Sampson S, George R, Jones P, Tran D, Dobson G, Hall R, Lee E, Tsui A, Choi S, Dwyer H, McCartney C, Carroll J, Huang Y, Cao Y, Gao H, Hu T, Yang J, Yang Y, Zhong Y, Zhou J, He M, Li X, Wang H, Chen L, Wang L, Cai Y, Li Y, Sun H, Wang S, Wang Z, Wang K, Zhu Y, Du X, Fu Y, Huang L, Huang Y, Wang Z, Wang G, Wang S, Zhang Y, Zhang X, Chen C, Wang W, Liu Z, Fan L, Tang J, Chen Y, Chen Y, Huang C, Shen J, Wang J, Yang Q, Zhou H, Chen J, Chen Z, Li X, Zhang X, Bi Y, Cao J, Lin H, Liu Y, Sun C, Sun Y, Wang Y, Wang S, Zhang M, Shen Z, Zhang Y, Zhao B, Zhou X-J, Chen Q, Guo H, Guo Y, Qi Y, Zhang W, Zheng L, Chen Y, Chen Y, Hu X, Li X, Shen C, Sun Y, Wang Y, Wang D, Wu C, Xu L, Yuan J, Zhang L, Zhang H, Zhang Y, Zhao J, Zhao C, Zhou H, Zhou C, Chen H, Chen S, He J, Li C, Li H, Pan Y, Shi Y, Wu S, Zhang K, Zhao B, Chen F, Lin X, Liu G, Tao J, Yang L, Zhou J, Chen F, Cheng Z, Feng Y, Hou B, Hu CH, Huang H, Huang J, Jiang Z, Li M, Lin J, Liu M, Liu W, Liu Z, Ma L, Min J, Song Z, Xiong Y, Xu L, Yang S, Zhang Q, Zhang H, Zhang H, Zhang X, Zhao W, Zhao W, Zhu X, Chen L, Chen S, Dai Q, Han K, He X, Huang L, Jia D, Jin S, Li Q, Luo S, Pan Y, Qian M, Qin J, Shi Y, Wang J, Wang J, Wang L, Yan Y, Yao Y, Zhang M, Zhao J, He L, Huang L, Li Z, Li H, Li Y, Li L, Yuan Y, Zhang E, Zhang J, Zhao S, Chen C, Li J, Wen Z, Yu Y, Yuan F, Hu X, Zhang Y, Xiao W, Zhu Z, Dai Q, Fu K, Hu R, Hu X, Huang S, Li Y, Liang Y, Yu S, Guo Z, Wu J, Zhang R, Zhao X, Li Y, Liu C-X, Liu F-F, Ren W, Wang X-L, Xu G-J, Li B, Ou Y, Tang Y, Yao S, Zhang S, Kong C-C, Liu B, Wang T, Xiao W, Lu B, Xia Y, Zhou J, Hu S, Wang H, Hu L, Li B, Liu Q, Liu Y, Qiu X, Ren Q, Tong Y, Wang J, Xia J, Xiong X, Xu S, Yang T, Yuan J, Zhang B, Chen S, Fan Y, Fu S, Ge X, Guo B, Huang W, Jiang L, Jiang X, Liu Y, Paet al., 2016,

    Global patient outcomes after elective surgery: Prospective cohort study in 27 low-, middle- and high-income countries

    , British Journal of Anaesthesia, ISSN: 0007-0912
  • Book chapter
    Turnbull JC, Graven H, Krakauer NY, 2016,

    Radiocarbon in the Atmosphere

    , RADIOCARBON AND CLIMATE CHANGE: MECHANISMS, APPLICATIONS AND LABORATORY TECHNIQUES, Editors: Schuur, Druffel, Trumbore, Publisher: SPRINGER INTERNATIONAL PUBLISHING AG, Pages: 83-137, ISBN: 978-3-319-25641-2
  • Conference paper
    Tao J, Wang L, Zong Q, Li G, Salem CS, Wimmer-Schweingruber RF, He J, Tu C, Bale SDet al., 2016,

    Solar Wind ∼0.1-1.5 keV Electrons at Quiet Times

    , 14th International Solar Wind Conference (Solar Wind), Publisher: AMER INST PHYSICS, ISSN: 0094-243X
  • Conference paper
    Franci L, Hellinger P, Matteini L, Verdini A, Landi Set al., 2016,

    Two-dimensional Hybrid Simulations of Kinetic Plasma Turbulence: Current and Vorticity vs Proton Temperature

    , 14th International Solar Wind Conference (Solar Wind), Publisher: AMER INST PHYSICS, ISSN: 0094-243X
  • Conference paper
    Yang L, Wang L, Li G, He J, Salem CS, Tu C, Wimmer-Schweingruber RF, Bale SDet al., 2016,

    The Angular Distribution of Solar Wind ∼20-200 keV Superhalo Electrons at Quiet Times

    , 14th International Solar Wind Conference (Solar Wind), Publisher: AMER INST PHYSICS, ISSN: 0094-243X
  • Journal article
    Mistry R, Eastwood JP, Hietala H, 2015,

    Development of bifurcated current sheets in solar wind reconnection exhausts

    , Geophysical Research Letters, Vol: 42, Pages: 10513-10520, ISSN: 1944-8007

    Petschek-type reconnection is expected to result in bifurcations of reconnection current sheets. In contrast, Hall reconnection simulations show smooth changes in the reconnecting magnetic field. Here we study three solar wind reconnection events where different spacecraft sample oppositely directed reconnection exhausts from a common reconnection site. The spacecraft's relative separations and measurements of the exhaust width are used to geometrically calculate each spacecraft's distance from the X line. We find that in all cases spacecraft farthest from the X line observe clearly bifurcated reconnection current sheets, while spacecraft nearer to the X line do not. These observations suggest that clear bifurcations of reconnection current sheets occur at large distances from the X line (~1000 ion skin depths) and that Petschek-type signatures are less developed close to the reconnection site. This may imply that fully developed bifurcations of reconnection current sheets are unlikely to be observed in the near-Earth magnetotail.
  • Journal article
    Archer MO, Hartinger MD, Walsh BM, Plaschke F, Angelopoulos Vet al., 2015,

    Frequency variability of standing Alfven waves excited by fast mode resonances in the outer magnetosphere

    , Geophysical Research Letters, Vol: 42, Pages: 10150-10159, ISSN: 0094-8276

    Coupled fast mode resonances (cFMRs) in the outer magnetosphere, between the magnetopause and a turning point, are often invoked to explain observed discrete frequency field line resonances. We quantify their frequency variability, applying cFMR theory to a realistic magnetic field model and magnetospheric density profiles observed over almost half a solar cycle. Our calculations show that cFMRs are most likely around dawn, since the plasmaspheric plumes and extended plasmaspheres often found at noon and dusk can preclude their occurrence. The relative spread (median absolute deviation divided by the median) in eigenfrequencies is estimated to be 28%, 72%, and 55% at dawn, noon, and dusk, respectively, with the latter two chiefly due to density. Finally, at dawn we show that the observed bimodal density distribution results in bimodal cFMR frequencies, whereby the secondary peaks are consistent with the so-called “CMS” frequencies that have previously been attributed to cFMRs.
  • Journal article
    Odelstad E, Eriksson AI, Edberg NJT, Johansson F, Vigren E, Andre M, Tzou CY, Carr CM, Cupido Eet al., 2015,

    Evolution of the plasma environment of comet 67P from spacecraft potential measurements by the Rosetta Langmuir probe instrument

    , Geophysical Research Letters, Vol: 42, Pages: 10126-10134, ISSN: 1944-8007

    We study the evolution of the plasma environment of comet 67P using measurements of the spacecraft potential from early September 2014 (heliocentric distance 3.5 AU) to late March 2015 (2.1 AU) obtained by the Langmuir probe (RPC-LAP) instrument. The low collision rate keeps the electron temperature high (~ 5 eV), resulting in a negative spacecraft potential whose magnitude depends on the electron density. This potential is more negative in the northern (summer) hemisphere, particularly over sunlit parts of the neck region on the nucleus, consistent with neutral gas measurements by ROSINA-COPS. Assuming constant electron temperature, the spacecraft potential traces the electron density. This increases as the comet approaches the Sun, most clearly in the southern hemisphere by a factor possibly as high as 20 - 44 between September 2014 and January 2015. The northern hemisphere plasma density increase stays around a factor of around or below 8 - 12, consistent with seasonal insolation change.
  • Journal article
    Stawarz JE, Pouquet A, 2015,

    Small-scale behavior of Hall magnetohydrodynamic turbulence

    , PHYSICAL REVIEW E, Vol: 92, ISSN: 2470-0045
  • Journal article
    Regoli LH, Roussos E, Feyerabend M, Jones GH, Krupp N, Coates AJ, Simon S, Motschmann U, Dougherty MKet al., 2015,

    Access of energetic particles to Titan's exobase: A study of Cassini's T9 flyby

    , Planetary and Space Science, Vol: 130, Pages: 40-53, ISSN: 1873-5088

    We study how the local electromagnetic disturbances introduced by Titan affect the ionization rates of the atmosphere. For this, we model the precipitation of energetic particles, specifically hydrogen and oxygen ions with energies between 1 keV and 1 MeV, into Titan׳s exobase for the specific magnetospheric configuration of the T9 flyby. For the study, a particle tracing software package is used which consists of an integration of the single particle Lorentz force equation using a 4th order Runge–Kutta numerical method. For the electromagnetic disturbances, the output of the A.I.K.E.F. hybrid code (kinetic ions, fluid electrons) is used, allowing the possibility of analyzing the disturbances and asymmetries in the access of energetic particles originated by their large gyroradii. By combining these methods, 2D maps showing the access of each set of particles were produced. We show that the access of different particles is largely dominated by their gyroradii, with the complexity of the maps increasing with decreasing gyroradius, due to the larger effect that local disturbances introduced by the presence of the moon have in the trajectory of the particles with lower energies. We also show that for particles with gyroradii much larger than the moon׳s radius, simpler descriptions of the electromagnetic environment can reproduce similar results to those obtained when using the full hybrid simulation description, with simple north–south fields being sufficient to reproduce the hybrid code results for O+ ions with energies larger than 10 keV but not enough to reproduce those for H+ ions at any of the energies covered in the present study. Finally, by combining the maps created with upstream plasma flow measurements by the MIMI/CHEMS instrument, we are able to estimate normalized fluxes arriving at different selected positions of the moon׳s exobase. We then use these fluxes to calculate energy deposition and non-dissociative N2 ionization rates for precipitati
  • Journal article
    Tinetti G, Drossart P, Eccleston P, Hartogh P, Isaak K, Linder M, Lovis C, Micela G, Ollivier M, Puig L, Ribas I, Snellen I, Swinyard B, Allard F, Barstow J, Cho J, Coustenis A, Cockell C, Correia A, Decin L, de Kok R, Deroo P, Encrenaz T, Forget F, Glasse A, Griffith C, Guillot T, Koskinen T, Lammer H, Leconte J, Maxted P, Mueller-Wodarg I, Nelson R, North C, Palle E, Pagano I, Piccioni G, Pinfield D, Selsis F, Sozzetti A, Stixrude L, Tennyson J, Turrini D, Zapatero-Osorio M, Beaulieu J-P, Grodent D, Guedel M, Luz D, Norgaard-Nielsen HU, Ray T, Rickman H, Selig A, Swain M, Banaszkiewicz M, Barlow M, Bowles N, Branduardi-Raymont G, du Foresto VC, Gerard J-C, Gizon L, Hornstrup A, Jarchow C, Kerschbaum F, Kovacs G, Lagage P-O, Lim T, Lopez-Morales M, Malaguti G, Pace E, Pascale E, Vandenbussche B, Wright G, Ramos Zapata G, Adriani A, Azzollini R, Balado A, Bryson I, Burston R, Colome J, Crook M, Di Giorgio A, Griffin M, Hoogeveen R, Ottensamer R, Irshad R, Middleton K, Morgante G, Pinsard F, Rataj M, Reess J-M, Savini G, Schrader J-R, Stamper R, Winter B, Abe L, Abreu M, Achilleos N, Ade P, Adybekian V, Affer L, Agnor C, Agundez M, Alard C, Alcala J, Allende Prieto C, Alonso Floriano FJ, Altieri F, Alvarez Iglesias CA, Amado P, Andersen A, Aylward A, Baffa C, Bakos G, Ballerini P, Banaszkiewicz M, Barber RJ, Barrado D, Barton EJ, Batista V, Bellucci G, Belmonte Aviles JA, Berry D, Bezard B, Biondi D, Blecka M, Boisse I, Bonfond B, Borde P, Boerner P, Bouy H, Brown L, Buchhave L, Budaj J, Bulgarelli A, Burleigh M, Cabral A, Capria MT, Cassan A, Cavarroc C, Cecchi-Pestellini C, Cerulli R, Chadney J, Chamberlain S, Charnoz S, Jessen NC, Ciaravella A, Claret A, Claudi R, Coates A, Cole R, Collura A, Cordier D, Covino E, Danielski C, Damasso M, Deeg HJ, Delgado-Mena E, Del Vecchio C, Demangeon O, De Sio A, De Wit J, Dobrijevic M, Doel P, Dominic C, Dorfi E, Eales S, Eiroa C, Espinoza Contreras M, Esposito M, Eymet V, Fabrizio N, Fernandez M, Femena Castella B, Figueira Pet al., 2015,

    The EChO science case

    , Experimental Astronomy, Vol: 40, Pages: 329-391, ISSN: 1572-9508

    The discovery of almost two thousand exoplanets has revealed an unexpectedlydiverse planet population. We see gas giants in few-day orbits, whole multi-planet systemswithin the orbit of Mercury, and new populations of planets with masses between that of theEarth and Neptune—all unknown in the Solar System. Observations to date have shown thatour Solar System is certainly not representative of the general population of planets in ourMilky Way. The key science questions that urgently need addressing are therefore: What areexoplanets made of? Why are planets as they are? How do planetary systems work and whatcauses the exceptional diversity observed as compared to the Solar System? The EChO(Exoplanet Characterisation Observatory) space mission was conceived to take up thechallenge to explain this diversity in terms of formation, evolution, internal structure andplanet and atmospheric composition. This requires in-depth spectroscopic knowledge of theatmospheres of a large and well-defined planet sample for which precise physical, chemicaland dynamical information can be obtained. In order to fulfil this ambitious scientificprogram, EChO was designed as a dedicated survey mission for transit and eclipsespectroscopy capable of observing a large, diverse and well-defined planet sample withinits 4-year mission lifetime. The transit and eclipse spectroscopy method, whereby the signalfrom the star and planet are differentiated using knowledge of the planetary ephemerides,allows us to measure atmospheric signals from the planet at levels of at least 10−4 relative tothe star. This can only be achieved in conjunction with a carefully designed stable payloadand satellite platform. It is also necessary to provide broad instantaneous wavelengthcoverage to detect as many molecular species as possible, to probe the thermal structureof the planetary atmospheres and to correct for the contaminating effects of the stellarphotosphere. This requires wavelength coverage of at l
  • Journal article
    Russell AJB, Yeates AR, Eastwood JP, 2015,

    Magnetic reconnection now and in the future

    , Astronomy and Geophysics, Vol: 56, ISSN: 1366-8781
  • Journal article
    Russell AJB, Yeates AR, Eastwood JP, 2015,

    Magnetic reconnection now and in the future

    , ASTRONOMY & GEOPHYSICS, Vol: 56, Pages: 18-23, ISSN: 1366-8781
  • Journal article
    Arridge CS, Eastwood J, Jackman CM, Poh GK, Slavin JA, Thomsen MF, Andre N, Jia X, Kidder A, Lamy L, Radioti A, Reisenfeld DB, Sergis N, Volwerk M, Walsh AP, Zarka P, Coates AJ, Dougherty MKet al., 2015,

    Cassini in situ observations of long duration magnetic reconnection in Saturn’s magnetotail

    , Nature Physics, Vol: 12, Pages: 268-271, ISSN: 1745-2481

    Magnetic reconnection is a fundamental process in solar system and astrophysical plasmas, through which stored magnetic energy associated with current sheets is converted into thermal, kinetic and wave energy1, 2, 3, 4. Magnetic reconnection is also thought to be a key process involved in shedding internally produced plasma from the giant magnetospheres at Jupiter and Saturn through topological reconfiguration of the magnetic field5, 6. The region where magnetic fields reconnect is known as the diffusion region and in this letter we report on the first encounter of the Cassini spacecraft with a diffusion region in Saturn’s magnetotail. The data also show evidence of magnetic reconnection over a period of 19 h revealing that reconnection can, in fact, act for prolonged intervals in a rapidly rotating magnetosphere. We show that reconnection can be a significant pathway for internal plasma loss at Saturn6. This counters the view of reconnection as a transient method of internal plasma loss at Saturn5, 7. These results, although directly relating to the magnetosphere of Saturn, have applications in the understanding of other rapidly rotating magnetospheres, including that of Jupiter and other astrophysical bodies.
  • Journal article
    Walker SN, Balikhin MA, Shklyar DR, Yearby KH, Canu P, Carr CM, Dandouras Iet al., 2015,

    Experimental determination of the dispersion relation of magnetosonic waves

    , Journal of Geophysical Research: Space Physics, Vol: 120, Pages: 9632-9650, ISSN: 2169-9402

    Magnetosonic waves are commonly observed in the vicinity of the terrestrial magnetic equator. It has been proposed that within this region they may interact with radiation belt electrons, accelerating some to high energies. These wave-particle interactions depend upon the characteristic properties of the wave mode. Hence determination of the wave properties is a fundamental part of understanding these interaction processes. Using data collected during the Cluster Inner Magnetosphere Campaign, this paper identifies an occurrence of magnetosonic waves, discusses their generation and propagation properties from a theoretical perspective, and utilises multispacecraft measurements to experimentally determine their dispersion relation. Their experimental dispersion is found to be in accordance with that based on cold plasma theory.
  • Journal article
    Field RD, Luo M, Kim D, Del Genio AD, Voulgarakis A, Worden Jet al., 2015,

    Sensitivity of simulated tropospheric CO to subgrid physics parameterization: a case study of Indonesian biomass burning emissions in 2006

    , Journal of Geophysical Research: Atmospheres, Vol: 120, Pages: 11743-11759, ISSN: 2169-8996

    Recent cumulus and turbulence parameterization changes to the NASA GISS ModelE2 have improved representation of the Madden-Julian Oscillation and low cloud distribution, but their effect on composition-related quantities is not known. In this study, we simulate the vertical transport of carbon monoxide (CO) from uncontrolled biomass burning in Indonesia in late 2006, during which uniquely high CO was detected in the upper troposphere. Two configurations of ModelE2, one without the changes (AR5) and one with the changes (AR5′), are used for an ensemble simulation of the transport of CO from the biomass burning. The simulation results are evaluated against new CO profiles retrieved jointly from the Aura Tropospheric Emission Spectrometer and the Microwave Limb Sounder. Modeled upper tropospheric CO using the AR5 physics was unrealistically high. The AR5′ physics suppress deep convection that reaches near the tropopause, reducing vertical transport of CO to the upper troposphere and bringing the model into better agreement with satellite CO. In this regard, the most important changes were related to the strength of entrainment of environmental air into the convective column, the strength of re-evaporation above cloud base, and a negative plume buoyancy threshold based on density temperature. This study illustrates how individual, noncomposition model changes can lead to significantly different modeled composition, which in this case improved agreement with satellite retrievals. This study also illuminates the potential usefulness of CO satellite observations in constraining unobservable processes in general circulation models.
  • Journal article
    Provan G, Tao C, Cowley SWH, Dougherty MK, Coates AJet al., 2015,

    Planetary period oscillations in Saturn's magnetosphere: Examining the relationship between abrupt changes in behavior and solar wind-induced magnetospheric compressions and expansions

    , Journal of Geophysical Research: Space Physics, Vol: 120, Pages: 9524-9544, ISSN: 2169-9402

    We examine planetary period oscillations (PPOs) observed in Saturn's magnetospheric magnetic field data from the time of Saturn's equinox in 2009. In particular, we focus on the time period commencing February 2011, when the oscillations started to display sudden and unexpected changes in behavior at ~100–200 day intervals. These were characterized by large simultaneous changes in the amplitude of the northern and southern PPO systems, together with small changes in period and jumps in phase. Nine significant abrupt changes have been observed in the postequinox interval to date, commencing as the Sun started to emerge from a long extended solar minimum. We perform a statistical study to determine whether these modulations in PPO behavior were associated with changes in the solar and/or upstream solar wind conditions. We report that the upstream solar wind conditions show elevated values of solar wind dynamic pressure and density around the time of PPO behavioral transitions, as opposed to before and after these times. We suggest that abrupt changes in PPO behavior may be related to significant changes in the size of the Saturnian magnetosphere in response to varying solar wind conditions.
  • Journal article
    Turner DL, O'Brien TP, Fennell JF, Claudepierre SG, Blake JB, Kilpua EKJ, Hietala Het al., 2015,

    The effects of geomagnetic storms on electrons in Earth's radiation belts

    , GEOPHYSICAL RESEARCH LETTERS, Vol: 42, Pages: 9176-9184, ISSN: 0094-8276
  • Journal article
    He J, Tu C, Marsch E, Chen CHK, Wang L, Pei Z, Zhang L, Salem CS, Bale SDet al., 2015,

    PROTON HEATING IN SOLAR WIND COMPRESSIBLE TURBULENCE WITH COLLISIONS BETWEEN COUNTER-PROPAGATING WAVES

    , ASTROPHYSICAL JOURNAL LETTERS, Vol: 813, ISSN: 2041-8205
  • Journal article
    Steckiewicz M, Mazelle C, Garnier P, André N, Penou E, Beth A, Sauvaud J-A, Toublanc D, Mitchell DL, McFadden JP, Luhmann JG, Lillis RJ, Connerney JEP, Espley JR, Andersson L, Halekas JS, Larson DE, Jakosky BMet al., 2015,

    Altitude dependence of nightside Martian suprathermal electron depletions as revealed by MAVEN observations

    , Geophysical Research Letters, Vol: 42, Pages: 8877-8884, ISSN: 0094-8276

    The MAVEN (Mars Atmosphere and Volatile EvolutioN) spacecraft is providing new detailed observations of the Martian ionosphere thanks to its unique orbital coverage and instrument suite. During most periapsis passages on the nightside ionosphere suprathermal electron depletions were detected. A simple criterion was implemented to identify the 1742 depletions observed from 16 November 2014 to 28 February 2015. A statistical analysis reveals that the main ion and electron populations within the depletions are surprisingly constant in time and altitude. Absorption by CO2 is the main loss process for suprathermal electrons, and electrons that strongly peaked around 6 eV are resulting from this interaction. The observation of depletions appears however highly dependent on altitude. Depletions are mainly located above strong crustal magnetic sources above 170 km, whereas the depletions observed for the first time below 170 km are globally scattered onto the Martian surface with no particular dependence on crustal fields.
  • Journal article
    Hadid LZ, Sahraoui F, Kiyani KH, Retino A, Modolo R, Canu P, Masters A, Dougherty MKet al., 2015,

    Nature of the MHD and kinetic scale turbulence in the magnetosheath of Saturn: Cassini observations

    , Astrophysical Journal Letters, Vol: 813, ISSN: 2041-8213

    Low-frequency turbulence in Saturn's magnetosheath is investigated using in situ measurements of the Cassini spacecraft. Focus is put on the magnetic energy spectra computed in the frequency range of ~[10−4, 1]Hz. A set of 42 time intervals in the magnetosheath were analyzed, and three main results that contrast with known features of solar wind turbulence are reported. (1) The magnetic energy spectra showed a ~f−1 scaling at MHD scales followed by an $\sim {f}^{-2.6}$ scaling at sub-ion scales without forming the so-called inertial range. (2) The magnetic compressibility and the cross-correlation between the parallel component of the magnetic field and density fluctuations $C(\delta n,\delta {B}_{| | })$ indicate the dominance of the compressible magnetosonic slow-like modes at MHD scales rather than the Alfvén mode. (3) Higher-order statistics revealed a monofractal (multifractal) behavior of the turbulent flow downstream of a quasi-perpendicular (quasi-parallel) shock at sub-ion scales. Implications of these results on theoretical modeling of space plasma turbulence are discussed.
  • Journal article
    Engelhardt IAD, Wahlund J-E, Andrews DJ, Eriksson AI, Ye S, Kurth WS, Gurnett DA, Morooka MW, Farrell WM, Dougherty MKet al., 2015,

    Plasma regions, charged dust and field-aligned currents near Enceladus

    , PLANETARY AND SPACE SCIENCE, Vol: 117, Pages: 453-469, ISSN: 0032-0633
  • Journal article
    Koskinen TT, Sandel BR, Yelle RV, Strobel DF, Mueller-Wodarg ICF, Erwin JTet al., 2015,

    Saturn's variable thermosphere from Cassini/UVIS occultations

    , Icarus, Vol: 260, Pages: 174-189, ISSN: 0019-1035

    We retrieved the density and temperature profiles in Saturn’s thermosphere from 26 stellar occultations observed by the Cassini/UVIS instrument. These results expand upon and complement the previous analysis of 15 Cassini/UVIS solar occultations by Saturn’s upper thermosphere. We find that the exospheric temperatures based on the stellar occultations agree with the solar occultations and range from 380 K to 590 K. These temperatures are also consistent with the recent re-analysis of the Voyager/UVS occultations. The retrieved density profiles support our earlier inference that the shape of the atmosphere at low pressures is consistent with a meridional trend of increasing temperatures with absolute latitude. This implies a high-latitude heat source, such as auroral heating, although the existing circulation models that include auroral heating still underestimate the equatorial temperatures by overestimating the meridional temperature gradient. This suggests either that the circulation models are somehow incomplete or there is some other heat source at low to mid latitudes that is relatively less efficient than high-latitude heating. We also find evidence for the expansion of the exobase by about 500 km between 2006 and 2011 near the equator, followed by possible contraction after 2011. The expansion appears to be caused by significant warming of the lower thermosphere that anti-correlates with solar activity and may be connected to changes in global circulation. Lastly, we note that our density profiles are in good general agreement with the Voyager/UVS data. In particular, the Voyager density profiles are most consistent with the Cassini/UVIS stellar occultations from late 2008 and early 2009 that roughly coincide in season with the Voyager flybys.
  • Journal article
    Fuselier SA, Altwegg K, Balsiger H, Berthelier JJ, Bieler A, Briois C, Broiles TW, Burch JL, Calmonte U, Cessateur G, Combi M, De Keyser J, Fiethe B, Galand M, Gasc S, Gombosi TI, Gune H, Hansen KC, Haessig M, Jaeckel A, Korth A, Le Roy L, Mall U, Mandt KE, Petrinec SM, Raghuram S, Reme H, Rinaldi M, Rubin M, Semon T, Trattner KJ, Tzou C-Y, Vigren E, Waite JH, Wurz Pet al., 2015,

    ROSINA/DFMS and IES observations of 67P: Ion-neutral chemistry in the coma of a weakly outgassing comet

    , Astronomy & Astrophysics, Vol: 583, ISSN: 1432-0746

    Context. The Rosetta encounter with comet 67P/Churyumov-Gerasimenko provides a unique opportunity for an in situ, up-closeinvestigation of ion-neutral chemistry in the coma of a weakly outgassing comet far from the Sun.Aims. Observations of primary and secondary ions and modeling are used to investigate the role of ion-neutral chemistry within thethin coma.Methods. Observations from late October through mid-December 2014 show the continuous presence of the solar wind 30 km fromthe comet nucleus. These and other observations indicate that there is no contact surface and the solar wind has direct access tothe nucleus. On several occasions during this time period, the Rosetta/ROSINA/Double Focusing Mass Spectrometer measured thelow-energy ion composition in the coma. Organic volatiles and water group ions and their breakup products (masses 14 through 19),CO+, and CO+2(masses 28 and 44) and other mass peaks (at masses 26, 27, and possibly 30) were observed. Secondary ions includeH3O+and HCO+(masses 19 and 29). These secondary ions indicate ion-neutral chemistry in the thin coma of the comet. A relativelysimple model is constructed to account for the low H3O+/H2O+and HCO+/CO+ratios observed in a water dominated coma. Resultsfrom this simple model are compared with results from models that include a more detailed chemical reaction network.Results. At low outgassing rates, predictions from the simple model agree with observations and with results from more complex modelsthat include much more chemistry. At higher outgassing rates, the ion-neutral chemistry is still limited and high HCO+/CO+ratiosare predicted and observed. However, at higher outgassing rates, the model predicts high H3O+/H2O+ratios and the observed ratiosare often low. These low ratios may be the result of the highly heterogeneous nature of the coma, where CO and CO2 number densitiescan exceed that of water.
  • Journal article
    Beth A, Garnier P, Toublanc D, Dandouras I, Mazelle Cet al., 2015,

    Theory for planetary exospheres: I. Radiation pressure effect on dynamical trajectories

    , Icarus, Vol: 266, Pages: 410-422, ISSN: 0019-1035

    The planetary exospheres are poorly known in their outer parts, since the neutral densities are low comparedwith the instruments detection capabilities. The exospheric models are thus often the main sourceof information at such high altitudes. We present a new way to take into account analytically the additionaleffect of the radiation pressure on planetary exospheres. In a series of papers, we present with anHamiltonian approach the effect of the radiation pressure on dynamical trajectories, density profiles andescaping thermal flux. Our work is a generalisation of the study by Bishop and Chamberlain (Bishop, J.,Chamberlian, J.W. [1989]. Icarus 81, 145–163). In this first paper, we present the complete solutions ofparticles trajectories, which are not conics, under the influence of the solar radiation pressure with someassumptions. This problem is similar to the classical Stark problem (Stark, J. [1914]. Ann. Phys. 348,965–982). This problem was largely tackled in the literature and more specifically, recently by Lantoineand Russell (Lantoine, G., Russell, R.P. [2011]. Celest. Mech. Dynam. Astron. 109, 333–366) and byBiscani and Izzo (Biscani, F., Izzo, D. [2014]. Mon. Not. R. Astron. Soc. 439, 810–822) as we will discussin this paper. We give here the full set of solutions for the motion of a particle (in our case for an atomor a molecule), i.e. the space coordinates and the time solution for bounded and unbounded trajectoriesin terms of Jacobi elliptic functions. We thus provide here the complete set of solutions for this so-callStark effect (Stark, J. [1914]. Ann. Phys. 348, 965–982) in terms of Jacobi elliptic functions (Jacobi, C.G.J. [1829]. Fundamenta nova theoriae functionum ellipticarum. Sumtibus fratrum), which may be usedto model the trajectories of particles in planetary exospheres.
  • Journal article
    Hausmann U, Czaja A, Marshall J, 2015,

    Estimates of air–sea feedbacks on sea surface temperature anomalies in the southern ocean

    , Journal of Climate, Vol: 29, Pages: 439-454, ISSN: 1520-0442

    Sea surface temperature (SST) air–sea feedback strengths and associated decay time scales in the Southern Ocean (SO) are estimated from observations and reanalysis datasets of SST, air–sea heat fluxes, and ocean mixed layer depths. The spatial, seasonal, and scale dependence of the air–sea heat flux feedbacks is mapped in circumpolar bands and implications for SST persistence times are explored. It is found that the damping effect of turbulent heat fluxes dominates over that due to radiative heat fluxes. The turbulent heat flux feedback acts to damp SSTs in all bands and spatial scales and in all seasons, at rates varying between 5 and 25 W m−2 K−1, while the radiative heat flux feedback has a more uniform spatial distribution with a magnitude rarely exceeding 5 W m−2 K−1. In particular, the implied net air–sea feedback (turbulent + radiative) on SST south of the polar front, and in the region of seasonal sea ice, is as weak as 5–10 W m−2 K−1 in the summertime on large spatial scales. Air–sea interaction alone thus allows SST signals induced around Antarctica in the summertime to persist for several seasons. The damping effect of mixed layer entrainment on SST anomalies averages to approximately 20 W m−2 K−1 across the ACC bands in the summer-to-winter entraining season and thereby reduces summertime SST persistence to less than half of that predicted by air–sea interaction alone (i.e., 3–6 months).
  • Journal article
    Brindley H, Osipov S, Bantges R, Smirnov A, Banks J, Levy R, Prakash PJ, Stenchikov Get al., 2015,

    An assessment of the quality of aerosol retrievals over the Red Sea and evaluation of the climatological cloud-free dust direct radiative effect in the region

    , Journal of Geophysical Research: Atmospheres, Vol: 120, ISSN: 2169-897X

    Ground-based and satellite observations are used in conjunction with the Rapid RadiativeTransfer Model (RRTM) to assess climatological aerosol loading and the associated cloud-free aerosol directradiative effect (DRE) over the Red Sea. Aerosol optical depth (AOD) retrievals from the Moderate ResolutionImaging Spectroradiometer and Spinning Enhanced Visible and InfraRed Imager (SEVIRI) instruments are firstevaluated via comparison with ship-based observations. Correlations are typically better than 0.9 with verysmall root-mean-square and bias differences. Calculations of the DRE along the ship cruises using RRTM alsoshow good agreement with colocated estimates from the Geostationary Earth Radiation Budget instrumentif the aerosol asymmetry parameter is adjusted to account for the presence of large particles. A monthlyclimatology of AOD over the Red Sea is then created from 5 years of SEVIRI retrievals. This shows enhancedaerosol loading and a distinct north to south gradient across the basin in the summer relative to the wintermonths. The climatology is used with RRTM to estimate the DRE at the top and bottom of the atmosphereand the atmospheric absorption due to dust aerosol. These climatological estimates indicate that althoughlongwave effects can reach tens of W m 2, shortwave cooling typically dominates the net radiativeeffect over the Sea, being particularly pronounced in the summer, reaching 120 W m 2 at the surface.The spatial gradient in summertime AOD is reflected in the radiative effect at the surface and in associateddifferential heating by aerosol within the atmosphere above the Sea. This asymmetric effect is expected toexert a significant influence on the regional atmospheric and oceanic circulation.

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