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12 results on '"L. Duvet"'

1. The Solar Electron and Proton Telescope for the STEREO Mission

Author

B. Johlander, Reinhold Müller-Mellin, Stephan Böttcher, J. Falenski, Hans Smit, B. Butler, E. Rode, L. Duvet, and T. R. Sanderson

Subjects
Physics, Range (particle radiation), Solar energetic particles, Solar flare, Proton, business.industry, Ecliptic, Astronomy and Astrophysics, Electron, law.invention, Telescope, Optics, Space and Planetary Science, law, Heliospheric current sheet, business
Abstract

The Solar Electron and Proton Telescope (SEPT), one of four instruments of the Solar Energetic Particle (SEP) suite for the IMPACT investigation, is designed to provide the three-dimensional distribution of energetic electrons and protons with good energy and time resolution. This knowledge is essential for characterizing the dynamic behaviour of CME associated and solar flare associated events. SEPT consists of two dual double-ended magnet/foil particle telescopes which cleanly separate and measure electrons in the energy range from 30–400 keV and protons from 60–7 000 keV. Anisotropy information on a non-spinning spacecraft is provided by the two separate telescopes: SEPT-E looking in the ecliptic plane along the Parker spiral magnetic field both towards and away from the Sun, and SEPT-NS looking vertical to the ecliptic plane towards North and South. The dual set-up refers to two adjacent sensor apertures for each of the four view directions: one for protons, one for electrons. The double-ended set-up refers to the detector stack with view cones in two opposite directions: one side (electron side) is covered by a thin foil, the other side (proton side) is surrounded by a magnet. The thin foil leaves the electron spectrum essentially unchanged but stops low energy protons. The magnet sweeps away electrons but lets ions pass. The total geometry factor for electrons and protons is 0.52 cm2 sr and 0.68 cm2 sr, respectively. This paper describes the design and calibration of SEPT as well as the scientific objectives that the instrument will address.

Published
2007

2. Rosina – Rosetta Orbiter Spectrometer for Ion and Neutral Analysis

Author

T Magoncelli, E. G. Shelley, Jenny Müller, E. Arijs, Christian Mazelle, Peter Bochsler, C. Aoustin, J. M. Illiano, Timm-Emanuel Riesen, H. Lauche, A. Loose, Stefano Livi, B. Fiethe, Tamas I. Gombosi, J. De Keyser, J. Fischer, Stephan Graf, Lennard A. Fisk, H. Rème, J. L. Medale, Jean-Jacques Berthelier, S. Scherer, Hermann Wollnik, Bruce P. Block, Peter Wurz, Annette Jäckel, Sandra Wüthrich, Kathrin Altwegg, Jean-André Sauvaud, S. Delanoye, U. Langer, Eernest Kopp, Eddy Neefs, D. T. Young, Fritz Gliem, Jean-Loup Bertaux, A. G. Ghielmetti, J. H. Waite, D. Nevejans, B. Wilken, A. Korth, M. Mildner, L. Duvet, Martin Rubin, Hans Balsiger, Peter Eberhardt, K Heerlein, G. R. Carignan, Stephen A. Fuselier, Ulrich Mall, Physikalisches Institut [Bern], Universität Bern [Bern], Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), 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, 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), Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Lockheed Martin Advanced Technology Center (ATC), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Space Physics Research Laboratory [Ann Arbor] (SPRL), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Southwest Research Institute [San Antonio] (SwRI), Physikalisches Institut [Gießen], Justus-Liebig-Universität Gießen (JLU), Universität Bern [Bern] (UNIBE), 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), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), and Justus-Liebig-Universität Gießen = Justus Liebig University (JLU)

Subjects
[PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], Physics, 010504 meteorology & atmospheric sciences, Spectrometer, Comet, Astronomy and Astrophysics, Mass spectrometry, 7. Clean energy, 01 natural sciences, Ion, law.invention, Astrobiology, Nuclear physics, Orbiter, Planetary science, Fragmentation (mass spectrometry), 13. Climate action, Space and Planetary Science, law, 0103 physical sciences, Formation and evolution of the Solar System, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

The Rosetta Orbiter Spectrometer for Ion and Neutral Analysis (ROSINA) will answer important questions posed by the mission's main objectives. After Giotto, this will be the first time the volatile part of a comet will be analyzed in situ. This is a very important investigation, as comets, in contrast to meteorites, have maintained most of the volatiles of the solar nebula. To accomplish the very demanding objectives through all the different phases of the comet's activity, ROSINA has unprecedented capabilities including very wide mass range (1 to >300 amu), very high mass resolution (m/Δ m > 3000, i.e. the ability to resolve CO from N2 and 13C from 12CH), very wide dynamic range and high sensitivity, as well as the ability to determine cometary gas velocities, and temperature. ROSINA consists of two mass spectrometers for neutrals and primary ions with complementary capabilities and a pressure sensor. To ensure that absolute gas densities can be determined, each mass spectrometer carries a reservoir of a calibrated gas mixture allowing in-flight calibration. Furthermore, identical flight-spares of all three sensors will serve for detailed analysis of all relevant parameters, in particular the sensitivities for complex organic molecules and their fragmentation patterns in our electron bombardment ion sources.

Published
2007

3. Visible and infrared detector developments supported by the European Space Agency

Author

K. Minoglou, Bruno Leone, Y. Levillain, C. Voland, R. Meynart, L. Duvet, N. Nelms, P.-E. Crouzet, J.-L. Bezy, M. Zahir, and A. Ciapponi

Subjects
Physics, business.industry, Remote sensing (archaeology), Detector, Agency (sociology), Infrared detector, Space (commercial competition), Telecommunications, business, Remote sensing
Abstract

Remote sensing is a priority activity for the European Space Agency and detector performance is a crucial factor in determining how well this role is performed. Consequently, the Agency has a strong interest in continuous improvement of both detector capabilities and availability within Europe. To this end, ESA maintains a number of strategic detector development plans combining both technology-push and technology-pull. The visible and infrared wavebands are of particular interest for remote sensing activities and this paper sets out the requirements for current and future missions and presents details of the Agency’s current and planned detector developments.

Published
2015

4. A low-energy spectrometer with a 2pi field of view for planetary missions

Author

M Godefroy, J Illiano, J J Berthelier, and L Duvet

Subjects
Physics, Range (particle radiation), Spectrometer, Spacecraft, business.industry, Applied Mathematics, Analyser, Energy analyser, Field of view, Ion, Optics, Magnet, business, Instrumentation, Engineering (miscellaneous)
Abstract

We present a novel ion mass spectrometer designed to measure thermal and low-energy suprathermal ion populations of planetary and cometary environments on board a three-axis-stabilized spacecraft. It consists of three main parts: an electrostatic analyser to perform the angular and energy scans, a magnetic analyser to provide the mass separation and a position-sensitive detector in the focal plane of the magnet. The instrument has a 2 field of view divided into 16 azimuthal sectors with continuous-elevation scanning between 0 and 90°. A high-resolution cylindrical energy analyser with adjustable energy resolution allows measurement of the temperature and velocity of thermal ions and the energy spectrum of suprathermal ions. The mass range extends from 1 to 45 amu/q . Comparisons between numerical simulation and laboratory tests of a prototype are presented.

Published
2000

5. Solar Prominence Diagnostics From the November 3, 1994 Eclipse

Author

E. Maurice, B. H. Foing, T. Beaufort, B. Altieri, L. Duvet, Sophie Cravatte, J. E. Wiik, L. Ligot, F. David, and N. Henrich

Subjects
Solar eclipse, Continuum (design consultancy), Coronal hole, Astronomy, Balmer series, General Medicine, Corona, Solar prominence, law.invention, Telescope, symbols.namesake, law, symbols, Geology, Eclipse
Abstract

We report results on solar prominences from our observations of the November 3, 1994 total solar eclipse from the North Chile alteplano. From the military base at Putre, we used our transportable CCD camera and telescope, as well as support photographic digitised observations from Putre and Parinacota volcano. The variation of density and equivalent temperature were derived in coronal holes (plumes and interplumes) and in equatorial streamers. We obtained images from the inner to the outer corona, as well as low-resolution spectra of prominences and of the inner corona. We present the analysis of images and spectra of prominences in the Balmer, He I and Ca II lines, and in the Thomson scattered continuum.

Published
1998

6. Assessment of space proton radiation-induced charge transfer inefficiency in the CCD204 for the Euclid space observatory

Author

Andrew D. Holland, G. Hopkinson, L Duvet, Neil J. Murray, David Hall, David W. Burt, Mark Cropper, and Jason Gow

Subjects
Physics, Basis (linear algebra), business.industry, media_common.quotation_subject, Space (mathematics), Galaxy, Universe, Optics, Operating temperature, Mask set, Baryon acoustic oscillations, business, Instrumentation, Mathematical Physics, Weak gravitational lensing, media_common
Abstract

Euclid is a medium class European Space Agency mission candidate for launch in 2019 with a primary goal to study the dark universe using the weak lensing and baryonic acoustic oscillations techniques. Weak lensing depends on accurate shape measurements of distant galaxies. Therefore it is beneficial that the effects of radiation-induced charge transfer inefficiency (CTI) in the Euclid CCDs over the course of the 5 year mission at L2 are understood. This will allow, through experimental analysis and modelling techniques, the effects of radiation induced CTI on shape to be decoupled from those of mass inhomogeneities along the line-of-sight. This paper discusses a selection of work from the study that has been undertaken using the e2v CCD204 as part of the initial proton radiation damage assessment for Euclid. The experimental arrangement and procedure are described followed by the results obtained, thereby allowing recommendations to be made on the CCD operating temperature, to provide an insight into CTI effects using an optical background, to assess the benefits of using charge injection on CTI recovery and the effect of the use of two different methods of serial clocking on serial CTI. This work will form the basis of a comparison with a p-channel CCD204 fabricated using the same mask set as the n-channel equivalent. A custom CCD has been designed, based on this work and discussions between e2v technologies plc. and the Euclid consortium, and designated the CCD273.

Published
2012

7. VIS: the visible imager for Euclid

Author

Mark Cropper, A. Refregier, P. Guttridge, O. Boulade, J. Amiaux, D. Walton, P. Thomas, K. Rees, P. Pool, J. Endicott, A. Holland, J. Gow, N. Murray, A. Amara, D. Lumb, L. Duvet, R. Cole, J.-L. Augueres, and G. Hopkinson

Published
2010

8. Control and acquisition system for SWIR focal plane arrays from SOFRADIR

Author

T. Beaufort and L. Duvet

Subjects
Engineering, business.industry, Adapter (computing), Interface (computing), Detector, Integrated circuit, Multiplexing, law.invention, Data acquisition, Control theory, law, Electronic engineering, business, Throughput (business)
Abstract

We report on the design, testing and characterization of a control and acquisition system developed for SWIR detectors from SOFRADIR. These detectors are MCT arrays developed for SWIR (Short Wavelength Infra Red) and hyperspectral applications;. The ROIC (Readout integrated circuitry) of each FPA (Focal Plane Array) delivers multiple analog outputs buffered and converted in the digital domain by dedicated board designed by SOFRADIR. These boards perform a time multiplexing of the digitized signals, leading to high data throughputs. Each FPA has its own dedicated Stirling micro-cooler. The control and acquisition system developed by our team is able to handle the high data throughput (up to 1.6 Gbit/s) thanks to a high speed acquisition board from National Instruments embedded in a PXI system. A standard DAQ card is used to acquire the house-keepings, control the different power supplies and clock generators while an SPI adapter enables the configuration of the FPA. The overall system is managed under the Labview environment with a flexible and comprehensive interface to the user with extensive logging of all operational parameters. The purpose of this paper is to describe the architecture of the overall system and to detail its performances.

Published
2009

9. Performance evaluation of MCT arrays developed for SWIR and hyperspectral applications: test bench and preliminary results

Author

N. Nelms, E. Martin, and L. Duvet

Subjects
On board, Engineering, Test bench, Optics, business.industry, Detector, Hyperspectral imaging, Quantum efficiency, business, Focus (optics), Sensitivity (electronics), Dark current
Abstract

We report here the first results of a performance evaluation program of two MCT arrays developed under ESA (European Space Agency) contracts by SOFRADIR. The program will first somehow repeat the electro-optical tests performed by the manufacturer and then focus on dark current and quantum efficiency. The first detector has a cut-off at 2.5 um and a format of 1000 x 256 (so called "SHOWMA") with 30 um pitch. A customized dewar has been manufactured in order to allow in particular a proper dark current measurements over a wide range of temperature. The second detector has a cut-off at 2.2 um with a format of 500 x256 (so called "BEPI") and a 30 um pitch. The particularity of the second detector is to have the CdZnTe substrate removed, leading to a sensitivity down to 0.4 um, as was requested for the targeted application (hyperspectral imager on board Bepi Colombo). It was delivered in a sealed dedicated miniaturized dewar with cooler. A complete electro-optical test bench has been developed and its commissioning will also be detailed. The test bench allows in particular quantum efficiency measurements over the full wavelength range 0.3 to 2.5 um.

Published
2009

10. Rosetta Orbiter Spectrometer for Ion and Neutral Analysis ROSINA

Author

H. Balsiger, K. Altwegg, P. Bochsler, P. Eberhardt, J. Fischer, S. Graf, A. Jäckel, E. Kopp, U. Langer, M. Mildner, J. Müller, T. Riesen, M. Rubin, S. Scherer, P. Wurz, S. Wüthrich, E. Arijs, S. Delanoye, J. De Keyser, E. Neefs, D. Nevejans, H. Rème, C. Aoustin, C. Mazelle, J.-L. Médale, J.A. Sauvaud, J.-J. Berthelier, J.-L. Bertaux, L. Duvet, J-M. Illiano, S.A. Fuselier, A.G. Ghielmetti, T. Magoncelli, E.G. Shelley, A. Korth, K. Heerlein, H. Lauche, S. Livi, A. Loose, U. Mall, B. Wilken, F. Gliem, B. Fiethe, T.I. Gombosi, B. Block, G.R. Carignan, L.A. Fisk, J.H. Waite, D.T. Young, and H. Wollnik

Published
2009

12. Scientific objectives of the DYNAMO mission

Author

R. Lin, M. Moncuquet, François Leblanc, David L. Mitchell, C. Mazelle, John Clarke, L. Duvet, E. Lellouch, Tilman Spohn, D. Toublanc, J. Dyment, Michael E. Purucker, S. Smrekar, Robert M. Haberle, P. Tarits, R. Hodges, G. Balmino, J. Luhmann, Bruce M. Jakosky, Michel Parrot, François Forget, Y. Cohen, Eric Chassefière, J. Connerney, O. Grasset, A M Buckley, Paul Gough, Olivier Witasse, D. T. Young, D. Bass, J. Lilensten, Doris Breuer, M. Blanc, Eric Quémerais, Karoly Szego, Ph. Lognonné, G. Hulot, H. Rème, K. Issautier, Jean-Pierre Barriot, D. T. Lyons, Jean-Gabriel Trotignon, Stephen W. Bougher, N. Meyer, P.-L. Blelly, Michel Menvielle, K. Sperveslage, A. Nagy, Jean-Claude Cerisier, Jean-Loup Bertaux, F. Vial, D. Vignes, C. Berger, Gérard Chanteur, M. Pätzold, M. Parmentier, F. Hourdin, J.-A. Sauvaud, C. Sotin, M. Acuna, Sho Sasaki, G. M. Keating, J. L. Bougeret, Robert E. Johnson, H. Waite, F. Barlier, Jean-Jacques Berthelier, P. Pinet, P. Touboul, Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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, 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), Laboratoire de Planétologie de Grenoble (LPG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), ONERA - The French Aerospace Lab [Palaiseau], ONERA-Université Paris Saclay (COmUE), Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique du Globe de Paris (IPGP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), 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), 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), Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Bretagne Occidentale - UFR Sciences et Techniques (UBO UFR ST), Université de Brest (UBO), Institut für Planetologie [Münster], Westfälische Wilhelms-Universität Münster (WWU), Institut für Geophysik und Meteorologie [Köln], Universität zu Köln, University of Sussex, Hungarian Academy of Sciences (MTA), The University of Tokyo (UTokyo), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, NASA Goddard Space Flight Center (GSFC), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, University of Virginia [Charlottesville], University of Michigan [Ann Arbor], University of Michigan System, University of Arizona, The George Washington University (GW), NASA Ames Research Center (ARC), University of Colorado [Boulder], University of Texas at Dallas [Richardson] (UT Dallas), Brown University, Southwest Research Institute [San Antonio] (SwRI), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Université 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 national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Westfälische Wilhelms-Universität Münster = University of Münster (WWU), Universität zu Köln = University of Cologne, NASA-California Institute of Technology (CALTECH), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), and University of Virginia

Subjects
Atmospheric Science, 010504 meteorology & atmospheric sciences, Aerospace Engineering, 01 natural sciences, Astrobiology, law.invention, Orbiter, law, 0103 physical sciences, Mercury's magnetic field, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Atmospheric escape, Astronomy and Astrophysics, Mars Exploration Program, Aerobraking, Solar wind, Geophysics, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Physics::Space Physics, General Earth and Planetary Sciences, Timekeeping on Mars, Astrophysics::Earth and Planetary Astrophysics, Thermosphere
Abstract

International audience; DYNAMO is a small Mars orbiter planned to be launched in 2005 or 2007, in the frame of the NASA/ CNES Mars exploration program. It is aimed at improving gravity and magnetic field resolution, in order to better understand the magnetic, geologic and thermal history of Mars, and at characterizing current atmospheric escape, which is still poorly constrained. These objectives are achieved by using a low periapsis orbit, similar to the one used by the Mars Global Surveyor spacecraft during its aerobraking phases. The proposed periapsis altitude for DYNAMO of 120–130 km, coupled with the global distribution of periapses to be obtained during one Martian year of operation, through about 5000 low passes, will produce a magnetic/gravity field data set with approximately five times the spatial resolution of MGS. Additional data on the internal structure will be obtained by mapping the electric conductivity. Low periapsis provides a unique opportunity to investigate the chemical and dynamical properties of the deep ionosphere, thermosphere, and the interaction between the atmosphere and the solar wind, therefore atmospheric escape, which may have played a crucial role in removing atmosphere and water from the planet.

Published
2001

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