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14 results on '"Y. de Conchy"'

1. CLUSTER–STAFF search coil magnetometer calibration – comparisons with FGM

Author

P. Robert, N. Cornilleau-Wehrlin, R. Piberne, Y. de Conchy, C. Lacombe, V. Bouzid, B. Grison, D. Alison, and P. Canu

Subjects
Geophysics. Cosmic physics, QC801-809
Abstract

The main part of the Cluster Spatio-Temporal Analysis of Field Fluctuations (STAFF) experiment consists of triaxial search coils allowing the measurements of the three magnetic components of the waves from 0.1 Hz up to 4 kHz. Two sets of data are produced, one by a module to filter and transmit the corresponding waveform up to either 10 or 180 Hz (STAFF-SC), and the second by the onboard Spectrum Analyser (STAFF-SA) to compute the elements of the spectral matrix for five components of the waves, 3 × B and 2 × E (from the EFW experiment), in the frequency range 8 Hz to 4 kHz. In order to understand the way the output signals of the search coils are calibrated, the transfer functions of the different parts of the instrument are described as well as the way to transform telemetry data into physical units across various coordinate systems from the spinning sensors to a fixed and known frame. The instrument sensitivity is discussed. Cross-calibration inside STAFF (SC and SA) is presented. Results of cross-calibration between the STAFF search coils and the Cluster Fluxgate Magnetometer (FGM) data are discussed. It is shown that these cross-calibrations lead to an agreement between both data sets at low frequency within a 2% error. By means of statistics done over 10 yr, it is shown that the functionalities and characteristics of both instruments have not changed during this period.

Published
2014
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2. Systematic analysis of equatorial noise below the lower hybrid frequency

Author

O. Santolík, F. Němec, K. Gereová, E. Macúšová, Y. de Conchy, and N. Cornilleau-Wehrlin

Subjects
Science, Physics, QC1-999, Geophysics. Cosmic physics, QC801-809
Abstract

We report results of a systematic analysis of a large number of observations of equatorial noise between the local proton cyclotron frequency and the local lower hybrid frequency. The analysis is based on the data collected by the STAFF-SA instruments on board the four Cluster spacecraft. The data set covers their first two years of measurement in the equatorial magnetosphere at radial distances between 3.9 and 5 Earth radii. Inspection of 781 perigee passages shows that the occurrence rate of equatorial noise is approximately 60%. We identify equatorial noise by selecting data with nearly linearly polarized magnetic field fluctuations. These waves are found within 10° of the geomagnetic equator, consistent with the published past observations. Our results show that equatorial noise has the most intense magnetic field fluctuations among all the natural emissions in the given interval of frequencies and latitudes. Electric field fluctuations of equatorial noise are also more intense compared to the average of all detected waves. Equatorial noise thus can play a non-negligible role in the dynamics of the internal magnetosphere.

Published
2004
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3. First results obtained by the Cluster STAFF experiment

Author

N. Cornilleau-Wehrlin, G. Chanteur, S. Perraut, L. Rezeau, P. Robert, A. Roux, C. de Villedary, P. Canu, M. Maksimovic, Y. de Conchy, D. Hubert, C. Lacombe, F. Lefeuvre, M. Parrot, J. L. Pinçon, P. M. E. Décréau, C. C. Harvey, Ph. Louarn, O. Santolik, H. St. C. Alleyne, M. Roth, T. Chust, O. Le Contel, and STAFF team

Subjects
Science, Physics, QC1-999, Geophysics. Cosmic physics, QC801-809
Abstract

The Spatio Temporal Analysis of Field Fluctuations (STAFF) experiment is one of the five experiments, which constitute the Cluster Wave Experiment Consortium (WEC). STAFF consists of a three-axis search coil magnetometer to measure magnetic fluctuations at frequencies up to 4 kHz, a waveform unit (up to either 10 Hz or 180 Hz) and a Spectrum Analyser (up to 4 kHz). The Spectrum Analyser combines the 3 magnetic components of the waves with the two electric components measured by the Electric Fields and Waves experiment (EFW) to calculate in real time the 5 × 5 Hermitian cross-spectral matrix at 27 frequencies distributed logarithmically in the frequency range 8 Hz to 4 kHz. The time resolution varies between 0.125 s and 4 s. The first results show the capabilities of the experiment, with examples in different regions of the magnetosphere-solar wind system that were encountered by Cluster at the beginning of its operational phase. First results obtained by the use of some of the tools that have been prepared specifically for the Cluster mission are described. The characterisation of the motion of the bow shock between successive crossings, using the reciprocal vector method, is given. The full characterisation of the waves analysed by the Spectrum Analyser, thanks to a dedicated program called PRASSADCO, is applied to some events; in particular a case of very confined electromagnetic waves in the vicinity of the equatorial region is presented and discussed.Key words. Magnetospheric physics (magnetopause, cusp and boundary layer) – Space plasma physics (waves and instabilities; shock waves)

Published
2003
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4. Polarisation and propagation of lion roars in the dusk side magnetosheath

Author

M. Maksimovic, C. C. Harvey, O. Santolík, C. Lacombe, Y. de Conchy, D. Hubert, F. Pantellini, N. Cornilleau-Werhlin, I. Dandouras, E. A. Lucek, and A. Balogh

Subjects
Science, Physics, QC1-999, Geophysics. Cosmic physics, QC801-809
Abstract

We present observations of "lion roars" obtained in the magnetosheath by the Spectrum Analyser (SA) of the Spatio-Temporal Analysis of Field Fluctuations (STAFF) experiment aboard Cluster. STAFF-SA calculates, in near real time, the complete auto- and cross-spectral matrix derived from three magnetic and two electric components of the electromagnetic field at 27 frequencies in the range of 8 Hz to 4 kHz. This allows the study of the properties of whistler mode waves and more particularly, the properties of "lion roars", which are intense, short-duration, narrow-banded packets of whistler waves. Their presence is favoured by the magnetic field troughs associated with mirror mode structures. During two short periods of well-defined mirror modes, we study the depth δB/B of the magnetic troughs, and the direction of propagation of the lion roars. During the first period, close to the magnetopause, deep magnetic troughs pass the satellites. Lion roars are then observed to propagate simultaneously in two directions, roughly parallel and anti-parallel to the magnetic field: this probably indicates that during this period, the satellites were within the successive source regions of lion roars. For the second period, far from the magnetopause, the magnetic troughs are less deep. Lion roars are propagating in only one direction, roughly anti-parallel to the magnetic field, suggesting that the source regions are more distant and predominantly on one side of the satellites.Key words. Magnetospheric physics (magnetosheath; plasma waves and instabilities) Radio science (radiowave propagation)

Published
2001
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5. The Solar Orbiter Radio and Plasma Waves (RPW) instrument (Corrigendum)

Author

Andris Vaivads, V. Krupař, M. Chariet, Lars Bylander, L. R. Malac-Allain, J. Parisot, Mats André, W. Recart, W. Puccio, C. Agrapart, D. Bérard, V. Leray, Robert F. Wimmer-Schweingruber, K. Boughedada, Baptiste Cecconi, E. Lorfèvre, M. Steller, B. Katra, F. Chapron, Helmut O. Rucker, Stuart D. Bale, Matthieu Kretzschmar, J.-C. Pellion, Ivana Kolmasova, J. Sanisidro, N. Quéruel, Filippo Pantellini, V. Bouzid, Laurent Lamy, Milan Maksimovic, L. Guéguen, C. Fiachetti, S. Chaintreuil, Mykhaylo Panchenko, Karine Issautier, M. Dekkali, O. Krupařová, Keith Goetz, Tomas Karlsson, I. Fratter, H. Ottacher, Philippe Louarn, P. Fergeau, O. Le Contel, Christopher J. Owen, Jan Soucek, A. Retino, Mihailo M. Martinović, Y. de Conchy, Olga Alexandrova, E. Bellouard, G. T. Delory, David Pisa, S. Thijs, E. Guilhem, Anders Eriksson, L. Åhlén, Antonio Vecchio, Timothy S. Horbury, Ondrej Santolik, Eduard P. Kontar, T. Vincent, V. Cripps, Daniel Dias, I. Zouganelis, A. Jeandet, T. Dudok de Wit, Sonny Lion, L. Uhlíř, Quynh Nhu Nguyen, M. Timofeeva, Dirk Plettemeier, J. Baše, Christopher Cully, Petr Hellinger, Lorenzo Matteini, Fouad Sahraoui, C. Collin, Paul Turin, Javier Rodriguez-Pacheco, Säm Krucker, P. Plasson, J.-Y. Brochot, Vladimir Krasnoselskikh, P. Leroy, Petr Travnicek, R. Lán, Yu. V. Khotyaintsev, S.-E. Jansson, Štěpán Štverák, G. Barbary, Pierre Astier, G. Jannet, R. Piberne, E. P. G. Johansson, F. Gonzalez, P. Danto, Arnaud Zaslavsky, J. Břínek, Thomas Chust, Xavier Bonnin, C. Laffaye, G. Cassam-Chenai, S. Julien, B. Pontet, Matthieu Berthomier, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Swedish Institute of Space Physics [Uppsala] (IRF), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Technische Universität Dresden = Dresden University of Technology (TU Dresden), Commission for Astronomy of the Austrian Academy of Sciences, Austrian Academy of Sciences (OeAW), Institute of Atmospheric Physics [Prague] (IAP), Czech Academy of Sciences [Prague] (CAS), Space Research Institute of Austrian Academy of Sciences (IWF), Royal Institute of Technology [Stockholm] (KTH ), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Nexeya Conseil & Formation, Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud university [Nijmegen], Centre National d'Études Spatiales [Toulouse] (CNES), Centre d’Ecologie Fonctionnelle et Evolutive (CEFE), Université Paul-Valéry - Montpellier 3 (UPVM)-Centre international d'études supérieures en sciences agronomiques (Montpellier SupAgro)-École pratique des hautes études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Institut national d’études supérieures agronomiques de Montpellier (Montpellier SupAgro), Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), ALTRAN (FRANCE), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES), Univerzita Karlova v Praze, Universities Space Research Association (USRA), NASA Goddard Space Flight Center (GSFC), Department of Physics and Astronomy [Calgary], University of Calgary, School of Physics and Astronomy [Minneapolis], University of Minnesota [Twin Cities] (UMN), University of Minnesota System-University of Minnesota System, Department of Physics [Imperial College London], Imperial College London, University of Glasgow, Fachhochschule Nordwestschweiz [Windisch] (FHNW), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, University of Belgrade [Belgrade], Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Universidad de Alcalá - University of Alcalá (UAH), Institute of Experimental and Applied Physics [Kiel] (IEAP), Christian-Albrechts-Universität zu Kiel (CAU), European Space Astronomy Centre (ESAC), European Space Agency (ESA), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Radboud University [Nijmegen], Université Paul-Valéry - Montpellier 3 (UPVM)-École Pratique des Hautes Études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut Agro - Montpellier SupAgro, Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro), Université de Rennes (UR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and Agence Spatiale Européenne = European Space Agency (ESA)

Subjects
Physics, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Astrophysics, Plasma, 01 natural sciences, law.invention, instrumentation: miscellaneous, Solar wind, Orbiter, solar wind, Space and Planetary Science, law, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, addenda, ComputingMilieux_MISCELLANEOUS, errata
Abstract

Contains fulltext : 239392.pdf (Publisher’s version ) (Open Access)

Published
2021
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6. The Solar Orbiter Radio and Plasma Waves (RPW) instrument

Author

L. R. Malac-Allain, T. Dudok de Wit, E. Lorfèvre, C. Collin, J. Sanisidro, Mihailo M. Martinović, X. Bonnin, E. Guilhem, Milan Maksimovic, P. Leroy, A. Vecchio, Eduard P. Kontar, L. Uhlíř, N. Quéruel, H. Ottacher, K. Boughedada, Christopher Cully, G. Barbary, Pierre Astier, Anders Eriksson, L. Åhlén, O. Krupařová, B. Pontet, T. Chust, G. Jannet, J. Parisot, Mats André, Paul Turin, P. Plasson, F. Chapron, M. Steller, W. Recart, W. Puccio, Vladimir Krasnoselskikh, Robert F. Wimmer-Schweingruber, V. Bouzid, Laurent Lamy, V. Cripps, R. Lán, Keith Goetz, B. Katra, S. Chaintreuil, Gregory T. Delory, I. Fratter, Dirk Plettemeier, C. Fiachetti, V. Krupař, M. Chariet, Sonny Lion, M. Dekkali, Lars Bylander, F. Gonzalez, Jan Soucek, Christopher J. Owen, Mykhaylo Panchenko, P. Danto, David Pisa, T. Vincent, Y. de Conchy, Säm Krucker, G. Cassam-Chenai, S. Julien, Baptiste Cecconi, Olga Alexandrova, A. Retino, V. Leray, Karine Issautier, S. Thijs, E. P. G. Johansson, Filippo Pantellini, D. Bérard, J. Baše, L. Guéguen, R. Piberne, P. Fergeau, Matthieu Berthomier, Tomas Karlsson, Arnaud Zaslavsky, Quynh Nhu Nguyen, J.-Y. Brochot, E. Bellouard, Yu. V. Khotyaintsev, Lorenzo Matteini, Štěpán Štverák, Javier Rodriguez-Pacheco, Fouad Sahraoui, S.-E. Jansson, O. Le Contel, Timothy S. Horbury, J.-C. Pellion, Pavel M. Trávníček, A. Jeandet, C. Agrapart, Petr Hellinger, Ondrej Santolik, I. Zouganelis, C. Laffaye, M. Timofeeva, D. Dias, Philippe Louarn, Helmut O. Rucker, Stuart D. Bale, Ivana Kolmasova, J. Břínek, Matthieu Kretzschmar, Andris Vaivads, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Swedish Institute of Space Physics [Uppsala] (IRF), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Technische Universität Dresden = Dresden University of Technology (TU Dresden), Institute of Computing [Campinas] (IC), Universidade Estadual de Campinas = University of Campinas (UNICAMP), Laboratoire de Biométrie et Biologie Evolutive - UMR 5558 (LBBE), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Recherche en Informatique et en Automatique (Inria)-VetAgro Sup - Institut national d'enseignement supérieur et de recherche en alimentation, santé animale, sciences agronomiques et de l'environnement (VAS)-Centre National de la Recherche Scientifique (CNRS), Centre d'Investigation Clinique [CHU Clermont-Ferrand] (CIC 1405), Institut National de la Santé et de la Recherche Médicale (INSERM)-Direction de la recherche clinique et de l’innovation [CHU Clermont-Ferrand] (DRCI), CHU Clermont-Ferrand-CHU Clermont-Ferrand, Department of Physics [Imperial College London], Imperial College London, Laboratoire Structures, Propriétés et Modélisation des solides (SPMS), Institut de Chimie du CNRS (INC)-CentraleSupélec-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Hasselt University (UHasselt), Centre National d'Études Spatiales [Toulouse] (CNES), Centre National d’Etudes Spatiales, Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de physique et chimie de l'environnement (LPCE), Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), DIREN RHONE ALPES LYON FRA, Partenaires IRSTEA, Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), International Agency for Research on Cancer (IARC), Institute of Genetics and Molecular Medicine, University of Edinburgh, Centre Hospitalier Régional Universitaire [Montpellier] (CHRU Montpellier), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Institute of Atmospheric Physics [Prague] (IAP), Czech Academy of Sciences [Prague] (CAS), NASA Goddard Space Flight Center (GSFC), Universities Space Research Association (USRA), Jiangsu University of Science and Technology (JUST), Universidade Estadual Paulista Júlio de Mesquita Filho = São Paulo State University (UNESP), Alfven Laboratory, Royal Institute of Technology [Stockholm] (KTH ), Department of Plant Physiology, Umeå University, Umea Plant Science Centre, Umeå University-Umeå University, Swedish University of Agricultural Sciences (SLU), Department of Space and Plasma Physics [Stockholm], KTH School of Electrical Engineering, Royal Institute of Technology [Stockholm] (KTH )-Royal Institute of Technology [Stockholm] (KTH ), Swedish Institute of Space Physics [Kiruna] (IRF), 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), Agence Spatiale Européenne = European Space Agency (ESA), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institute of Computing [Campinas] (UNICAMP), Universidade Estadual de Campinas (UNICAMP), Université d'Orléans (UO)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of California [Berkeley], University of California-University of California, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and European Space Agency (European Space Agency) (ESA)

Subjects
010504 meteorology & atmospheric sciences, Astronomy, Astrophysics, Plasma oscillation, 01 natural sciences, law.invention, Orbiter, Astronomi, astrofysik och kosmologi, law, 0103 physical sciences, Astronomy, Astrophysics and Cosmology, Aerospace engineering, 010303 astronomy & astrophysics, miscellaneous [instrumentation], 0105 earth and related environmental sciences, Physics, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Plasma, Solar radio, instrumentation: miscellaneous, Solar wind, solar wind, Space and Planetary Science, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Interplanetary spaceflight, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The Radio and Plasma Waves (RPW) instrument on the ESA Solar Orbiter mission is described in this paper. This instrument is designed to measure in-situ magnetic and electric fields and waves from the continuous to a few hundreds of kHz. RPW will also observe solar radio emissions up to 16 MHz. The RPW instrument is of primary importance to the Solar Orbiter mission and science requirements since it is essential to answer three of the four mission overarching science objectives. In addition RPW will exchange on-board data with the other in-situ instruments in order to process algorithms for interplanetary shocks and type III langmuir waves detections. Correction in: Astronomy & Astrophysics, Volume 654, Article Number C2, DOI 10.1051/0004-6361/201936214e

Published
2020
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7. Polarisation and propagation of lion roars in the dusk side magnetosheath

Author

Milan Maksimovic, D. Hubert, Filippo Pantellini, Nicole Cornilleau-Werhlin, C. Lacombe, Ondrej Santolik, Elizabeth Lucek, Y. de Conchy, Iannis Dandouras, C. C. Harvey, A. Balogh, Departement de recherche SPAtiale (DESPA), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Department of Physics and Astronomy [Ames, Iowa], Iowa State University (ISU), Centre d'étude des environnements terrestre et planétaires (CETP), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Imperial College London, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
Electromagnetic field, Atmospheric Science, 010504 meteorology & atmospheric sciences, Field (physics), Whistler, Magnetosphere, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Astrophysics, 01 natural sciences, Magnetosheath, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), lcsh:Science, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Radio Science, Physics, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, lcsh:QC801-809, Geology, Astronomy and Astrophysics, Geophysics, lcsh:QC1-999, Magnetic field, lcsh:Geophysics. Cosmic physics, Space and Planetary Science, Physics::Space Physics, Magnetopause, lcsh:Q, lcsh:Physics
Abstract

We present observations of "lion roars" obtained in the magnetosheath by the Spectrum Analyser (SA) of the Spatio-Temporal Analysis of Field Fluctuations (STAFF) experiment aboard Cluster. STAFF-SA calculates, in near real time, the complete auto- and cross-spectral matrix derived from three magnetic and two electric components of the electromagnetic field at 27 frequencies in the range of 8 Hz to 4 kHz. This allows the study of the properties of whistler mode waves and more particularly, the properties of "lion roars", which are intense, short-duration, narrow-banded packets of whistler waves. Their presence is favoured by the magnetic field troughs associated with mirror mode structures. During two short periods of well-defined mirror modes, we study the depth δB/B of the magnetic troughs, and the direction of propagation of the lion roars. During the first period, close to the magnetopause, deep magnetic troughs pass the satellites. Lion roars are then observed to propagate simultaneously in two directions, roughly parallel and anti-parallel to the magnetic field: this probably indicates that during this period, the satellites were within the successive source regions of lion roars. For the second period, far from the magnetopause, the magnetic troughs are less deep. Lion roars are propagating in only one direction, roughly anti-parallel to the magnetic field, suggesting that the source regions are more distant and predominantly on one side of the satellites.Key words. Magnetospheric physics (magnetosheath; plasma waves and instabilities) Radio science (radiowave propagation)

Published
2001

8. [Untitled]

Author

P. Louarn, J. M. Nappa, L. Friel, Wlodek Kofman, N. Cornilleau-Wehrlin, R. Manning, S. Perraut, P. Robert, C. de Villedary, D. Hubert, F. Wouters, Laurence Rezeau, Jean-Louis Pinçon, Y. de Conchy, C. Lacombe, A. Meyer, François Lefeuvre, S. Louis, Michel Parrot, A. Roux, B. Poirier, C. C. Harvey, and P. Chauveau

Subjects
Electromagnetic field, Physics, Spectrum analyzer, 010504 meteorology & atmospheric sciences, Field (physics), Dynamic range, Magnetometer, Acoustics, Astronomy and Astrophysics, 01 natural sciences, law.invention, Search coil, Solar wind, Nuclear magnetic resonance, Space and Planetary Science, law, 0103 physical sciences, Waveform, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

The Spatio-Temporal Analysis of Field Fluctuations (STAFF) experiment is one of five experiments which together comprise the Wave Experiment Consortium (WEC). STAFF consists of a three-axis search coil magnetometer to measure magnetic fluctuations at frequencies up to 4 kHz, and a spectrum analyser to calculate in near-real time aboard the spacecraft, the complete auto- and cross-spectral matrices using the three magnetic and two electric components of the electromagnetic field. The magnetic waveform at frequencies below either 10 Hz or 180 Hz is also transmitted. The sensitivity of the search coil is adapted to the phenomena theo be studied: the values 3 × 10-3 nT Hz-1/2 and 3 × 10-5 nT Hz-1/2 are achieved respectively at 1 Hz and 100 Hz. The dynamic range of the STAFF instruments is about 96 dB in both waveform and spectral power, so as to allow the study of waves near plasma boundaries. Scientific objectives of the STAFF investigations, particularly those requiring four point measurements, are discussed. Methods by which the wave data will be characterised are described with emphasis on those specific to four-point measurements, including the use of the Field Energy Distribution function.

Published
1997
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9. CLUSTER STAFF search coils magnetometer calibration - comparisons with FGM

Author

P. Robert, N. Cornilleau-Wehrlin, R. Piberne, Y. de Conchy, C. Lacombe, V. Bouzid, B. Grison, D. Alison, P. Canu, Laboratoire de Physique des Plasmas (LPP), Université Paris-Sud - Paris 11 (UP11)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Informatique, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Physique des plasmas, Institute of Atmospheric Physics [Prague] (IAP), and Czech Academy of Sciences [Prague] (CAS)

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; The main part of Cluster Spatio Temporal Analysis of Field Fluctuations (STAFF) experiment consists of triaxial search coils allowing the measurements of the three magnetic components of the waves from 0.1 Hz up to 4 kHz. Two sets of data are produced, one by a module to filter and transmit the corresponding waveform up to either 10 or 180 Hz (STAFF-SC) and the second by an onboard Spectrum Analyser (STAFF-SA) to compute the elements of the spectral matrix for five components of the waves, 3 × B and 2 × E (from EFW experiment) in the frequency range 8 Hz to 4 kHz. In order to understand the way the output signal of the search coils are calibrated, the transfer functions of the different parts of the instrument are described as well as the way to transform telemetry data into physical units, across various coordinate systems from the spinning sensors to a fixed and known frame. The instrument sensitivity is discussed. Cross-calibration inside STAFF (SC and SA) is presented. Results of cross-calibration between the STAFF search coils and the Cluster Flux Gate Magnetometer (FGM) data are discussed. It is shown that these cross-calibrations lead to an agreement between both data sets at low frequency within a 2% error. By means of statistics done over 10 yr, it is shown that the functionalities and characteristics of both instruments have not changed during this period.

Published
2013

10. The RETE experiment for the TSS-1 mission

Author

S. Ekholm, Y. de Conchy, E. Melchioni, C. C. Harvey, J. P. Lebereton, F. Wouters, R. Orfei, M. Maggi, Luciano Iess, R. M. Manning, A. Butler, U. Guidoni, and M. Dobrowolny

Subjects
On board, Space Shuttle, Satellite, Instrumentation (computer programming), Ionosphere, Electrodynamic tether, Remote sensing
Abstract

This paper describes the RETE (Research on Electrodynamic Tether Effects) experiment mounted on board the TSS (Tethered-Satellite System) satellite which was deployed on a cable from the space Shuttle Atlantis during the TSS mission flown in August 1992. The experiment layout and its modes of operation are described in detail. To give an idea of RETE capabilities and actual performance during the mission, samples of measurements are also presented.

Published
1994
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11. Equatorial noise : statistical study of its localization, and the derived number density

Author

Eva Macusova, Ondrej Santolik, K. Gereová, Harri Laakso, Nicole Cornilleau-Wehrlin, Y. de Conchy, Milan Maksimovic, František Němec, Faculty of Mathematics and Physics [Praha/Prague], Charles University [Prague], European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude des environnements terrestre et planétaires (CETP), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Faculty of Mathematics and Physics [Charles University of Praha], Charles University [Prague] (CU), Agence Spatiale Européenne = European Space Agency (ESA), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique des plasmas, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Atmospheric Science, 010504 meteorology & atmospheric sciences, Meteorology, Aerospace Engineering, Magnetic dip, Magnetosphere, Cluster, STAFF-SA, Equatorial noise, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Geomagnetic latitude, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, STAFF-SA, Number density, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Linear polarization, Astronomy and Astrophysics, Lower hybrid oscillation, Computational physics, Magnetic field, Geophysics, 13. Climate action, Space and Planetary Science, Cluster, Physics::Space Physics, General Earth and Planetary Sciences, Equatorial noise, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Noise (radio)
Abstract

International audience; Results of a statistical study of equatorial noise emissions are presented. These electromagnetic emissions are observed in the inner magnetosphere in the vicinity of the geomagnetic equator at frequencies below the lower hybrid frequency. We use the data recorded by four Cluster spacecraft during years 2001-2003. The data set was processed in three steps. In the first one, we have selected the data with a nearly linear polarization (ellipticity less than 0.2), corresponding to the known properties of the equatorial noise. Secondly, we have found parameters of a Gaussian model of the frequency-averaged power-spectral density of those selected waves as a function of the geomagnetic latitude. Finally, we have analyzed the data in the latitudinal interval defined by the width of the Gaussian model. Our results show that most intensity peaks of equatorial noise occur exactly at the magnetic equator. Incidental deviations are most probably caused by problems in determination of the true magnetic equator, which is shown by using different magnetic field models. We have estimated the plasma number density at the observation points using the cold plasma theory. These estimates are, within experimental errors, close to the values obtained from the spacecraft potential data measured by the EFW instrument.

Published
2006
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12. Initial Results of a Survey of Equatorial Noise Emissions Observed by the Cluster Spacecraft

Author

K. Gereová, Nicole Cornilleau-Wehrlin, Y. de Conchy, Ondrej Santolik, Eva Macusova, František Němec, Centre d'étude des environnements terrestre et planétaires (CETP), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Faculty of Mathematics and Physics [Praha/Prague], Charles University [Prague] (CU), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique des plasmas, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris

Subjects
Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Linear polarization, Waves in plasmas, Magnetosphere, Astronomy and Astrophysics, Geophysics, Lower hybrid oscillation, Earth radius, Computational physics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Amplitude, Space and Planetary Science, Physics::Space Physics, Geomagnetic latitude, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Noise (radio)
Abstract

International audience; Initial results of a survey of equatorial noise emissions are presented. These plasma wave emissions are observed in the inner magnetosphere close to the geomagnetic equator at frequencies below the local lower hybrid frequency. We use the data recorded by the four Cluster spacecraft during the first 24 months of measurements. The data set was processed in three steps. First, we have selected the data with a nearly linear polarization corresponding to the known properties of the equatorial noise. Second, we have found parameters of a Gaussian model of the frequency-averaged power-spectral density of the selected waves as a function of the geomagnetic latitude. Third, we have analyzed the data as a function of frequency in the latitudinal interval defined by the width of the Gaussian model. Our results show that most intensity peaks of equatorial noise occur within 2o of the magnetic equator and the full-width at half-maximum (FWHM) of these peaks is below 3o in the majority of cases. The most probable frequency of the emissions is between 4 and 5 local proton cyclotron frequencies. The probability density of occurrence of the emissions then slowly decreases toward higher frequencies. Multipoint measurements indicate that the variations of the ratios of amplitudes of the equatorial noise emissions measured on different spacecraft do not increase at spatial scales up to 0.7 Earth radii in the equatorial plane. On the other hand, the variations do increase with time delay between measurements in an interval from tenths to hundreds of minutes.

Published
2005
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13. Systematic analysis of equatorial noise below the lower hybrid frequency

Author

Nicole Cornilleau-Wehrlin, Eva Macusova, František Němec, Ondrej Santolik, Y. de Conchy, K. Gereová, Faculty of Mathematics and Physics [Praha/Prague], Charles University [Prague] (CU), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude des environnements terrestre et planétaires (CETP), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and EGU, Publication

Subjects
Atmospheric Science, 010504 meteorology & atmospheric sciences, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Magnetosphere, 01 natural sciences, Earth radius, Latitude, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Electric field, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), lcsh:Science, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.OCEAN] Sciences of the Universe [physics]/Ocean, Atmosphere, Linear polarization, lcsh:QC801-809, Geology, Astronomy and Astrophysics, Geophysics, Lower hybrid oscillation, lcsh:QC1-999, Computational physics, Magnetic field, lcsh:Geophysics. Cosmic physics, 13. Climate action, Space and Planetary Science, Physics::Space Physics, [SDU.STU] Sciences of the Universe [physics]/Earth Sciences, lcsh:Q, Astrophysics::Earth and Planetary Astrophysics, lcsh:Physics, Noise (radio)
Abstract

We report results of a systematic analysis of a large number of observations of equatorial noise between the local proton cyclotron frequency and the local lower hybrid frequency. The analysis is based on the data collected by the STAFF-SA instruments on board the four Cluster spacecraft. The data set covers their first two years of measurement in the equatorial magnetosphere at radial distances between 3.9 and 5 Earth radii. Inspection of 781 perigee passages shows that the occurrence rate of equatorial noise is approximately 60%. We identify equatorial noise by selecting data with nearly linearly polarized magnetic field fluctuations. These waves are found within 10° of the geomagnetic equator, consistent with the published past observations. Our results show that equatorial noise has the most intense magnetic field fluctuations among all the natural emissions in the given interval of frequencies and latitudes. Electric field fluctuations of equatorial noise are also more intense compared to the average of all detected waves. Equatorial noise thus can play a non-negligible role in the dynamics of the internal magnetosphere.

Published
2004
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14. First results obtained by the Cluster STAFF experiment

Author

A. Roux, J. L. Pinçon, Gérard Chanteur, Michel Parrot, Laurence Rezeau, C. de Villedary, François Lefeuvre, H. St. C. Alleyne, P. Décréau, Staff team, C. Lacombe, O. Le Contel, D. Hubert, C. C. Harvey, Ondrej Santolik, N. Cornilleau-Wehrlin, Milan Maksimovic, Patrick Canu, T. Chust, S. Perraut, Y. de Conchy, P. Robert, M. Roth, P. Louarn, Centre d'étude des environnements terrestre et planétaires (CETP), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire de physique et chimie de l'environnement (LPCE), Université d'Orléans (UO)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Faculty of Mathematics and Physics [Praha/Prague], Charles University [Prague] (CU), University of Sheffield [Sheffield], Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Shock wave, Physics, Atmospheric Science, Field (physics), lcsh:QC801-809, Phase (waves), [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Geology, Astronomy and Astrophysics, Geophysics, Bow shocks in astrophysics, Electromagnetic radiation, lcsh:QC1-999, Computational physics, Search coil, Solar wind, lcsh:Geophysics. Cosmic physics, Space and Planetary Science, Earth and Planetary Sciences (miscellaneous), Magnetopause, lcsh:Q, lcsh:Science, lcsh:Physics
Abstract

The Spatio Temporal Analysis of Field Fluctuations (STAFF) experiment is one of the five experiments, which constitute the Cluster Wave Experiment Consortium (WEC). STAFF consists of a three-axis search coil magnetometer to measure magnetic fluctuations at frequencies up to 4 kHz, a waveform unit (up to either 10 Hz or 180 Hz) and a Spectrum Analyser (up to 4 kHz). The Spectrum Analyser combines the 3 magnetic components of the waves with the two electric components measured by the Electric Fields and Waves experiment (EFW) to calculate in real time the 5 × 5 Hermitian cross-spectral matrix at 27 frequencies distributed logarithmically in the frequency range 8 Hz to 4 kHz. The time resolution varies between 0.125 s and 4 s. The first results show the capabilities of the experiment, with examples in different regions of the magnetosphere-solar wind system that were encountered by Cluster at the beginning of its operational phase. First results obtained by the use of some of the tools that have been prepared specifically for the Cluster mission are described. The characterisation of the motion of the bow shock between successive crossings, using the reciprocal vector method, is given. The full characterisation of the waves analysed by the Spectrum Analyser, thanks to a dedicated program called PRASSADCO, is applied to some events; in particular a case of very confined electromagnetic waves in the vicinity of the equatorial region is presented and discussed.Key words. Magnetospheric physics (magnetopause, cusp and boundary layer) – Space plasma physics (waves and instabilities; shock waves)

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