Publications

2013

• From 1AU solar wind turbulence backward to coronal turbulence: an inverse problem
  
  • Dong Yue
  • Verdini Andrea
  • Grappin Roland
  , 2013, 15, pp.3285. This work deals with the formation of the low-frequency spectrum of solar wind turbulence, including the so-called inertial range and the lower frequency 1/f range. Much is known on the turbulent state of the solar wind plasma at distances larger than 0.3 AU, but few is known on the turbulent state of the plasma at the sources of the wind, like the coronal plasma. Characterizing the turbulence state of plasma in the solar corona is thus an inverse problem. To solve this inverse problem, we use the MHD expanding box model, which consists in incorporating in the MHD equations the effects of expansion on a turbulent plasma volume advected by a wind with constant (radial) velocity, by using comobile coordinates. In spite of its limitations (assumption of constant expansion), the model includes the basic effects of expansion (i) anisotropic damping of velocity and magnetic field (ii) weakening of nonlinear coupling in the perpendicular directions. The code allows in particular to follow the 3D turbulent evolution of the kinetic and magnetic energy spectra. We present here for the first time numerical solutions of the expanding 3D MHD equations by starting with different initial conditions: we follow the turbulent evolution of the plasma box imbedded in a radial wind up to 1 AU and compare the final turbulent state with observations, thus allowing us to determine which initial conditions are acceptable. We vary three kinds of initial parameters: (1) spectral/components anisotropy (2) Alfvén species imbalance (3) kinetic/magnetic imbalance. The connection of the results with available models of the formation of coronal turbulence is discussed at the end.
• Evidence of coherent drift-resonant acceleration of radiation belt particles by ULF waves
  
  • Sauvaud J.-A.
  • Walt M.
  • Delcourt Dominique C.
  • Benoist C.
  • Penou E.
  • Chen Y.
  • Russell Christopher T.
  , 2013, 15, pp.EGU2013-1830. Evidence is presented for frequent, coherent and powerful accelerations of radiation belt electrons and protons during magnetic storms. Geomagnetic storms are indeed frequently associated with the formation of well developed, multiple bands of energetic electrons inside the inner radiation belt at L=1.1-1.9 and with prominent similar energy structures of protons inside the slot region at L=2.2-3.5. These structures typically from 100 keV up to the MeV range result from coherent interactions of energetic particles with quasi- monochromatic Ultra Low Frequency waves (ULF). These waves are induced by magnetospheric changes due to the arrival of dense solar material and related nightside injections of particles from the outer magnetosphere that destabilize field lines in the inner magnetosphere down to L=1.1. We show that, at the low altitudes of the Demeter spacecraft, these structures are best seen near the South Atlantic Anomaly because of lowering of the belt particle mirror point. As evidenced from ground measurements, energy bands are associated with quasi-sinusoidal ULF Pc5 and Pc4 waves with periods in the 1000 second range for L = 1.1-1.9 and in the 60 second range for L=2.2-3.5. Numerical simulations of the coherent drift resonance of energetic particles with Ultra Low Frequency waves show how the particles are accelerated and how the observed structures build up. The structures are formed for interaction times of the order of 20-40 minutes. For longer resonance times, particles are accelerated at energies higher than 1.5 MeV while lower energy particles are decelerated.
• Europlanet/IDIS: Combining Diverse Planetary Observations and Models
  
  • Schmidt Walter
  • Capria Maria Teresa
  • Chanteur Gérard
  , 2013, 15, pp.6726. Planetary research involves a diversity of research fields from astrophysics and plasma physics to atmospheric physics, climatology, spectroscopy and surface imaging. Data from all these disciplines are collected from various space-borne platforms or telescopes, supported by modelling teams and laboratory work. In order to interpret one set of data often supporting data from different disciplines and other missions are needed while the scientist does not always have the detailed expertise to access and utilize these observations. The Integrated and Distributed Information System (IDIS) [1], developed in the framework of the Europlanet-RI project, implements a Virtual Observatory approach ([2] and [3]), where different data sets, stored in archives around the world and in different formats, are accessed, re-formatted and combined to meet the user's requirements without the need of familiarizing oneself with the different technical details. While observational astrophysical data from different observatories could already earlier be accessed via Virtual Observatories, this concept is now extended to diverse planetary data and related model data sets, spectral data bases etc. A dedicated XML-based Europlanet Data Model (EPN-DM) [4] was developed based on data models from the planetary science community and the Virtual Observatory approach. A dedicated editor simplifies the registration of new resources. As the EPN-DM is a super-set of existing data models existing archives as well as new spectroscopic or chemical data bases for the interpretation of atmospheric or surface observations, or even modeling facilities at research institutes in Europe or Russia can be easily integrated and accessed via a Table Access Protocol (EPN-TAP) [5] adapted from the corresponding protocol of the International Virtual Observatory Alliance [6] (IVOA-TAP). EPN-TAP allows to search catalogues, retrieve data and make them available through standard IVOA tools if the access to the archive is compatible with IVOA standards. For some major data archives with different standards adaptation tools are available to make the access transparent to the user. EuroPlaNet-IDIS has contributed to the definition of PDAP, the Planetary Data Access Protocol of the International Planetary Data Alliance (IPDA) [7] to access the major planetary data archives of NASA in the USA [8], ESA in Europe [9] and JAXA in Japan [10]. Acknowledgement: Europlanet-RI was funded by the European Commission under the 7th Framework Program, grant 228319 "Capacities Specific Programme" - Research Infrastructures Action. Reference: [1] Details to IDIS and the Europlanet-RI via Web-site: http://www.idis.europlanet-ri.eu/ [2] Demonstrator implementation for Plasma-VO AMDA: http://cdpp-amda.cesr.fr/DDHTML/index.html [3] Demonstrator implementation for the IDIS-VO: http://www.idis-dyn.europlanet-ri.eu/vodev.shtml [4] Europlanet Data Model EPN-DM: http://www.europlanet-idis.fi/documents/public_documents/EPN-DM-v2.0.pdf [5] Europlanet Table Access Protocol EPN-TAP: http://www.europlanet-idis.fi/documents/public_documents/EPN-TAPV₀.26.pdf [6] International Virtual Observatory Alliance IVOA: http://www.ivoa.net [7] International Planetary Data Alliance IPDA: http://planetarydata.org/ [8] NASA's Planetary Data System: http://pds.jpl.nasa.gov/ [9] ESA's Planetary Science Archive PSA: http://www.sciops.esa.int/index.php?project=PSA [10] JAXAs Data Archive and Transmission System DARTS: http://darts.isas.jaxa.jp
• Impact of the Earth bow shock crossing on magnetic clouds structure
  
  • Turc Lucile
  • Fontaine Dominique
  • Savoini Philippe
  • Kilpua E. K. J.
  , 2013, 15, pp.4848. In the solar wind, magnetic clouds (MC) display a well-defined magnetic structure. When they reach the vicinity of the Earth, their structure is modified by their interaction with the Earth environment. In this study, we focus on the bow shock crossing of MCs, and more specifically on how it alters their magnetic structure. We compare observations from the Cluster spacecraft in the magnetosheath to ACE magnetic field measurements in the solar wind, in order to highlight the differences before and after the bow shock crossing. We find that the magnetic field amplitude is higher inside the magnetosheath, as expected from the compression behind the shock, but that the magnetic field direction can exhibit different features. It can be similar to the solar wind magnetic field direction, display a phase shift or the smooth rotation can even disappear in the magnetosheath. The correlation between the variation of the magnetic field direction from the solar wind to the magnetosheath and the shock obliquity angle is investigated. Finally, a simple 3D MHD model is developed to describe the interaction of a MC with the bow shock and calculate the magnetic field amplitude and direction inside the magnetosheath. We show several outputs of the model, corresponding to different orientations of the MC axis. We compare these modeled cases to observations. In some cases, the results show that the trends are in qualitative agreement, and other cases are further discussed.
• Magnetic field and plasma fluctuations in CME-driven sheath regions
  
  • Kilpua E. K. J.
  • Hietala H.
  • Koskinen H.
  • Fontaine Dominique
  • Turc Lucile
  , 2013, 15, pp.2855. Coronal mass ejection (CME)-driven sheath regions exhibit large-amplitude interplanetary magnetic field and dynamic pressure fluctuations, which may enhance the solar wind-magnetosphere coupling and lead to larger geomagnetic activity. The internal structure of CME sheath region is extremely complex as it gradually forms when the CME propagates from the Sun to the orbit of the Earth. In this study we perform a statistical superposed epoch analysis of the magnetic field and dynamic pressure fluctuations in sheath regions observed by the ACE spacecraft near Lagrangian point L1 using the wavelet analysis. In particular, we investigate where in the sheath the fluctuation power is strongest and how its level and distribution within the sheath depends on the CME properties (speed, strength and the closest approach distance from the CME center). We found that there is a sharp decrease in the magnetic field Ultra Low Frequency (2-15 minutes) power between the sheath and the CME leading edge. We suggest that this decrease can be used as a proxy for the CME front boundary.
• Analysis of amplitudes of equatorial noise emissions and their variation with L, MLT and magnetic activity
  
  • Hrbackova Z.
  • Santolík O.
  • Cornilleau-Wehrlin Nicole
  , 2013, 15, pp.EGU2013-10281. Wave-particle interactions are an important mechanism of energy exchange in the outer Van Allen radiation belt. These interactions can cause an increase or decrease of relativistic electron flux. The equatorial noise (EN) emissions (also called fast magnetosonic waves) are electromagnetic waves which could be effective in producing MeV electrons. EN emissions propagate predominantly within 10° of the geomagnetic equator at L shells from 1 to 10. Their frequency range is between the local proton cyclotron frequency and the lower hybrid resonance. We use a data set measured by the STAFF-SA instruments onboard four Cluster spacecraft from January 2001 to December 2010. We have compiled the list of the time intervals of the observed EN emissions during the investigated time period. For each interval we have computed an intensity profile of the wave magnetic field as a function of frequency. The frequency band is then determined by an automatic procedure and the measured power spectral densities are reliably transformed into wave amplitudes. The results are shown as a function of the McIlwain's parameter, magnetic local time and magnetic activity - Kp and Dst indexes. This work has received EU support through the FP7-Space grant agreement n 284520 for the MAARBLE collaborative research project.
• Case study of an atypical magnetopause crossing
  
  • Dorville Nicolas
  • Belmont Gérard
  • Rezeau Laurence
  • Grappin Roland
  • Retinò Alessandro
  , 2013, 15, pp.EGU2013-2279.
• Eleven years of Cluster observations of whistler-mode chorus
  
  • Santolík O.
  • Macusova E.
  • Kolmasova Ivana
  • Cornilleau-Wehrlin Nicole
  • Pickett J. S.
  , 2013, 15, pp.EGU2013-10234. Electromagnetic emissions of whistler-mode chorus carry enough power to increase electron fluxes in the outer Van Allen radiation belt at time scales on the order of one day. However, the ability of these waves to efficiently interact with relativistic electrons is controlled by the wave propagation directions and time-frequency structure. Eleven years of measurements of the STAFF-SA and WBD instruments onboard the Cluster spacecraft are systematically analyzed in order to determine the probability density functions of propagation directions of chorus as a function of geomagnetic latitude, magnetic local time, L* parameter, and frequency. A large database of banded whistler-mode emissions and time-frequency structured chorus has been used for this analysis. This work has received EU support through the FP7-Space grant agreement no 284520 for the MAARBLE collaborative research project.
• BV technique for investigating 1D interfaces
  
  • Dorville Nicolas
  • Belmont Gérard
  • Rezeau Laurence
  • Aunai N.
  • Retinò Alessandro
  , 2013.
• Radial evolution of thin current sheets in the Earth's magnetotail
  
  • Malova H. V.
  • Zelenyi L. M.
  • Popov V. Y.
  • Delcourt Dominique
  • Petrukovich A. A.
  , 2013, 15, pp.EGU2013-3116. The model of thin current sheet in the Earth's magnetotail taking into account the radial inhomogeneity of magnetic field is constructed and investigated. It is shown that charge particle dynamics which is different in earthward and tailward regions of current sheet is determined by large-scale changes of the normal component of the magnetic field. At the same time as transient ions support practically 1D structure of current sheet, contributions of electrons and quasi-trapped ions differ dependently on the radial distance from the Earth. Thus quasi-trapped ions should dominate in earthward region of current sheet, in contrast to electrons supporting a narrow strong peak of current density in tailward edge of current sheet. Generally, it is shown that thin current sheets in the Earth's magnetotail might be described as 2D multiscale embedded structure.
• Directions of equatorial noise propagation determined using Cluster and DEMETER spacecraft
  
  • Nemec F.
  • Hrbackova Z.
  • Santolík O.
  • Pickett J. S.
  • Parrot M.
  • Cornilleau-Wehrlin Nicole
  , 2013, 15, pp.EGU2013-2203. Equatorial noise emissions are electromagnetic waves at frequencies between the proton cyclotron frequency and the lower hybrid frequency routinely observed within a few degrees of the geomagnetic equator at radial distances from about 2 to 6 Re. High resolution data reveal that the emissions are formed by a system of spectral lines, being generated by instabilities of proton distribution functions at harmonics of the proton cyclotron frequency in the source region. The waves propagate in the fast magnetosonic mode nearly perpendicularly to the ambient magnetic field, i.e. the corresponding magnetic field fluctuations are almost linearly polarized along the ambient magnetic field and the corresponding electric field fluctuations are elliptically polarized in the equatorial plane, with the major polarization axis having the same direction as wave and Poynting vectors. We conduct a systematic analysis of azimuthal propagation of equatorial noise. Combined WBD and STAFF-SA measurements performed on the Cluster spacecraft are used to determine not only the azimuthal angle of the wave vector direction, but also to estimate the corresponding beaming angle. It is found that the beaming angle is generally rather large, i.e. the detected waves come from a significant range of directions, and a traditionally used approximation of a single plane wave fails. The obtained results are complemented by a raytracing analysis in order to get a comprehensive picture of equatorial noise propagation in the inner magnetosphere. Finally, high resolution multi-component measurements performed by the low-altitude DEMETER spacecraft are used to demonstrate that equatorial noise emissions can reach altitudes as low as 660 km, and that the observed propagation properties are in agreement with the overall propagation picture.
• Electron acceleration to relativistic energies at a strong quasi-parallel shock wave
  
  • Masters A.
  • Stawarz L.
  • Fujimoto M.
  • Schwartz S. J.
  • Sergis N.
  • Thomsen M. F.
  • Retinò Alessandro
  • Hasegawa H.
  • Zieger B.
  • Lewis G. R.
  • Coates A. J.
  • Canu Patrick
  • Dougherty M.
  , 2013, 15, pp.EGU2013-6522. Electrons can be accelerated to ultrarelativistic energies at strong (high-Mach number) collisionless shock waves that form when stellar debris rapidly expands after a supernova. Collisionless shock waves also form in the flow of particles from the Sun (the solar wind), and extensive spacecraft observations have established that electron acceleration at these shocks is effectively absent whenever the upstream magnetic field is roughly parallel to the shock surface normal (quasi-parallel conditions). However, it is unclear whether this magnetic dependence of electron acceleration also applies to the far stronger shocks around young supernova remnants, where local magnetic conditions are poorly understood. Here we present Cassini spacecraft observations of an unusually strong solar system shock wave (Saturn's bow shock) where significant local electron acceleration has been confirmed under quasi-parallel magnetic conditions for the first time, contradicting the established magnetic dependence of electron acceleration at solar system shocks. Furthermore, the acceleration led to electrons at relativistic energies (~MeV), comparable to the highest energies ever attributed to shock-acceleration in the solar wind. These observations suggest that at high-Mach numbers, like those of young supernova remnant shocks, quasi-parallel shocks become considerably more effective electron accelerators.
• Characteristics of banded chorus-like emission measured by the TC-1 Double Star spacecraft
  
  • Macusova E.
  • Santolík O.
  • Cornilleau-Wehrlin Nicole
  • Yearby K. H.
  , 2013, 15, pp.10341. We present a study of the spatio-temporal characteristics of banded whistler-mode emissions. It covers the full operational period of the TC-1 spacecraft, between January 2004 and the end of September 2007. The analyzed data set has been visually selected from the onboard-analyzed time-frequency spectrograms of magnetic field fluctuations below 4 kHz measured by the STAFF/DWP wave instrument situated onboard the TC-1 spacecraft with a low inclination elliptical equatorial orbit. This orbit covers magnetic latitudes between -39o and 39o. The entire data set has been collected between L=2 and L=12. Our results show that almost all intense emissions (above a threshold of 10-5nT2Hz-1) occur at L-shells from 6 to 12 and in the MLT sector from 2 to 11 hours. This is in a good agreement with previous observations. We determine the bandwidth of the observed emission by an automatic procedure based on the measured spectra. This allows us to reliably calculate the integral amplitudes of the measured signals. The majority of the largest amplitudes of chorus-like emissions were found closer to the Earth. The other result is that the upper band chorus-like emissions (above one half of the electron cyclotron frequency) are much less intense than the lower band chorus-like emissions (below one half of the electron cyclotron frequency) and are usually observed closer to the Earth than the lower band. This work has received EU support through the FP7-Space grant agreement n 284520 for the MAARBLE collaborative research project.
• Solar wind plasma turbulence: one or several turbulent regimes?
  
  • Dong Yue
  • Grappin Roland
  , 2013, 15, pp.3269. The average turbulent spectrum in the solar wind shows non trivial properties. At 1 AU, the average spectral index of the magnetic and kinetic spectra in the inertial range are respectively 5/3 and 3/2, which is not predicted by any turbulence theory. The spectral indices, as well as the amplitude of the fluctuations, actually vary around their average values in a non-random way: they appear to be controled by the average wind parameters, the best control parameter being the ion temperature, as first noted by Grappin Velli Mangeney 1991. We come back on this analysis here using a more refined method that isolates the inertial range from the 1/f range, allowing us to reveal a more reduced variation of the inertial range slope, which is however still controled by the ion temperature. We discuss the possible origin of the variation, and attempt to understand what it reveals on the birth of turbulence close to the Sun.
• A single spacecraft method to study the spatial profiles inside the magnetopause
  
  • Dorville Nicolas
  • Belmont Gérard
  • Rezeau Laurence
  • Aunai N.
  • Retinò Alessandro
  , 2013, 15, pp.EGU2013-2282. Previous magnetopause observations have revealed that the tangential magnetic field often rotates over C-shaped hodograms during the boundary crossing. Using observations of magnetopause crossings by the ESA Cluster mission and a simulation developed at LPP by Nicolas Aunai, we developed a single spacecraft method using the temporal information on the magnetic field in such crossings, complemented by the ion data. We can so obtain a 1D spatial parameter to characterize the depth in the layer and study the structure of the magnetopause as a function of this parameter. This allows using one single spacecraft magnetic data, completed by ion data at large temporal scales, to study the spatial structure of the boundary, and access scales that the particle temporal measurements of the four spacecraft do not permit. To obtain the normal direction and position, we first initialize our computations thanks to the standard MVABC method. Then we use the magnetic field data in the current layer, and suppose it is 1D, rotating in the tangential plane along an ellipse, with an angle variation essentially linear in space, with small sinusoidal perturbations. Making the assumption that the normal velocity of ions is dominated by the motion of the boundary and that the internal structure of the magnetopause is stationary over the duration of a crossing, we can compute the best normal direction and parameters of the model with CIS velocity and FGM magnetic field data, and so derive the spatial position of the spacecraft in the boundary. This method, which has been tested on the simulation data, could be applied successfully on several magnetopause crossings observed by Cluster. It directly gives a thickness and a normal direction, and permits to establish spatial profiles of all the physical quantities inside the boundary. It can be used to better understand the internal structure of the boundary, its physical properties and behavior regarding the flux conservation equations. The obtained results are compared with the results of other methods.
• Mercury intrinsic magnetic field : Limits of the offset-dipole representation
  
  • Chanteur Gérard
  • Modolo Ronan
  • Richer Emilie
  • Hess Sebastien
  • Leblanc François
  , 2013, 15, pp.EGU2013-6483. The interaction of the solar wind (SW) with the magnetic field of The analysis of MESSENGER orbital observations led Anderson et al (2011) to propose a dipole centered on the spin axis of the planet with a northward offset equal to 484±11 km to represent the intrinsic magnetic field of Mercury at northern latitudes higher than 30°. The magnetic moment has a magnitude of 195±10nT, points southward and is tilted by less than 3° with respect to the spin axis. The restriction to northern latitude comes from the lack of low altitude measurements of the magnetic field at southern latitudes due to MESSENGER orbit. Hence for the moment being there is no observation to constrain the representation of the southern planetary field. The suggested offset is equal to about 20% of the planetary radius which is quite a large value by comparison to 8.5% in the terrestrial case although with a lateral offset. This representation of the intrinsic field by an offset dipole suggests that the southern polar cap should be much wider than the northern one, leading to important consequences for magnetospheric dynamics. Nevertheless the offset dipole is just a convenient representation that can be fitted by the first terms of the multipolar development. The surface field of the planet produced by the offset dipole (OD) proposed by Anderson et al (2011) is thus fitted by the sum of a dipolar and a quadrupolar field (DQ) for northern latitudes higher than 50°. The resulting field differs slightly from the offset dipole field at northern latitudes but a separatrix exists at southern latitudes between dipolar-like and quadrupolar like field lines. This separatrix begins on the polar axis at an altitude RS equal to three times the ratio of the quadrupolar to the dipolar moment. When the relative axial offset of the dipole becomes larger than 16% then RS becomes larger than the planetary radius leading to important topological changes of the southern field. Global hybrid simulations of the Hermean magnetosphere for the two models OD and DQ demonstrate that the southern magnetosphere produced by the DQ model differs greatly from what is expected using the OD model (Richer et al 2012). Reference: Anderson et al., Science, 333 , 1859, (2011) Richer, E., R. Modolo, G. M. Chanteur, S. Hess, and F. Leblanc (2012), A global hybrid model for Mercury's interaction with the solar wind: Case study of the dipole representation, J. Geophys. Res., 117, A10228, doi:10.1029/2012JA017898.
• Review of Recent Mid-Z Precursor Wire Array Experiments on the Zebra Generator at UNR
  
  • Stafford A.
  • Safronova Alla S.
  • Kantsyrev Viktor L.
  • Esaulov A. A.
  • Weller Michael E.
  • Osborne Glenn C.
  • Shrestha Ishor
  • Keim S. F.
  • Shlyaptseva V. V.
  • Coverdale C.
  • Chuvatin Alexandre S.
  , 2013.
• Radiation Sources with Planar Wire Arrays for ICF and High Energy Density Physics Research
  
  • Kantsyrev Viktor L.
  • Chuvatin Alexandre S.
  • Safronova Alla S.
  • Rudakov Leonid I.
  • Esaulov A. A.
  • Velikovich A. L.
  • Shrestha Ishor
  • Astanovitsky A.
  • Obsorne G. C.
  • Shlyaptseva V. V.
  • Weller S. F.
  • Keim S.
  • Stafford A.
  , 2013.
• RADIATION FROM MULTI-PLANAR WIRE ARRAYS AND APPLICATIONS
  
  • Safronova Alla S.
  • Kantsyrev Viktor L.
  • Esaulov A. A.
  • Weller Michael E.
  • Shlyaptseva V. V.
  • Shrestha Ishor
  • Osborne Glenn C.
  • Keim S. F.
  • Stafford A.
  • Chuvatin Alexandre S.
  • Apruzese J. P.
  • Giuliani J. L.
  • Coverdale C. A.
  • Jones Brent M.
  , 2013. as a Sandia report, number SAND2013-2638C
• Etudes de l'Ionosphère Equatoriale dans le cadre du réseau GIRGEA (Groupe International de Recherche en Géophysique Europe Afrique)
  
  • Amory-Mazaudier Christine
  • Fleury Rolland
  • Ouattara Frédéric Martial
  • Zerbo J.-L.
  • Pham Thi Thu Hong
  • Shimeis Amira
  • Zoundi C.
  • Fathy Ibrahim
  • Le Huy Minh
  • Mahrous A. M.
  , 2013, http://ursi-france.institut-telecom.fr/index.php?id=67. Résumé: Durant la dernière décennie dans le cadre des projets CAWSES (Climate and Weather in the Sun Earth System), AHI (Année Héliophysique Internationale) 2006-2009 et ISWI (International Space Weather Initiative) 2010-2012, la connaissance du soleil et de son impact sur les couches ionisées a considérablement avancé suivant différents canaux : - synthèse connectant la physique du soleil à celle de lionosphère - analyse de longues séries de données ionosphériques sur plusieurs cycles solaires - déploiement dinstruments (GPS et magnétomètres) sur le continent africain dans des régions où les mesures étaient inexistantes, ce fait entrainant la révision de certains modèles. Le réseau de recherche GIRGEA a profité de ces projets et développé des études des zones équatoriales en Afrique et en Asie. Cet article présente les résultats obtenus concernant principalement les variations long terme de lIonosphère équatoriale, limpact des éjections de masse coronale et des jets de vents rapides issus des trous coronaux sur les couches ionisés, et linadéquation de certains modèles à représenter les récentes observations en Afrique.
• Spectral dynamics and Predator-Prey oscillations in turbulence in fusion plasmas
  
  • Gürcan Özgür D.
  • Morel Pierre
  • Berionni Vincent
  , 2013.
• Cluster-STAFF sensitivity
  
  • Piberne Rodrigue
  • Robert Patrick
  , 2013. This software was developped in order to produce figure 8 and 9 of the article: Patrick Robert, Nicole Cornilleau-Wehrlin, Rodrigue Piberne, Y. de Conchy, C. Lacombe, et al.. CLUSTER-STAFF search coil magnetometer calibration - comparisons with FGM. Geoscientific Instrumentation, Methods and Data Systems, 2014, 3, pp.153-177. ⟨10.5194/gi-3-153-2014⟩.
• Wave emissions at ion scales close to Ganymede
  
  • Grison B.
  • Santolík O.
  • Pickett J. S.
  • Chust Thomas
  • Zouganelis I.
  , 2013.
• Goniopolarimetry with Coupled Electric and Magnetic Measurements
  
  • Cecconi Baptiste
  • Gautier Anne-Lise
  • Bergman J. E. S.
  • Chust Thomas
  • Marchaudon Aurélie
  • Cavoit C.
  • Santolýk Ondrej
  , 2013.
• Basic Plasma Physics: the collisionless limit and the fluid-kinetic dilemma
  
  • Belmont Gérard
  , 2013.