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32 results on '"G. Hulot"'

1. Total Root Electron Content: A New Metric for the Ionosphere Below Low Earth Orbiting Satellites

Author

M. Jenner, P. Coïsson, G. Hulot, D. Buresova, V. Truhlik, and L. Chauvet

Subjects
total root electron content, whistlers, swarm, ionospheric radio propagation, magnetometer, low Earth orbiting satellites, Geophysics. Cosmic physics, QC801-809
Abstract

Abstract Powerful lightning strikes generate broadband electromagnetic signals. At Extremely Low Frequencies (ELF), the signal partly leaks into the ionosphere and produces whistlers that can be detected by satellites. Indeed, the satellites of the European Space Agency (ESA) Swarm Earth Explorer mission can detect those signals during 250 Hz burst‐mode acquisition campaigns of their Absolute Scalar Magnetometers (ASM). The dispersion of these whistlers depends on their propagation path and the distribution of ionization in the ionosphere crossed along that path. In this paper, we introduce a technique to derive a new measure of ionosphere electron content, the Total square‐Root Electron Content (TREC), using the arrival times of two frequencies of the whistler signal. We validate this approach by using data from ionosondes and from in situ measurements of the electron density at Swarm location. This technique brings new opportunities for sounding the ionosphere in regions poorly observed by other techniques.

Published
2024
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2. Evaluation of candidate models for the 13th generation International Geomagnetic Reference Field

Author

P. Alken, E. Thébault, C. D. Beggan, J. Aubert, J. Baerenzung, W. J. Brown, S. Califf, A. Chulliat, G. A. Cox, C. C. Finlay, A. Fournier, N. Gillet, M. D. Hammer, M. Holschneider, G. Hulot, M. Korte, V. Lesur, P. W. Livermore, F. J. Lowes, S. Macmillan, M. Nair, N. Olsen, G. Ropp, M. Rother, N. R. Schnepf, C. Stolle, H. Toh, F. Vervelidou, P. Vigneron, and I. Wardinski

Subjects
IGRF, Magnetic field modeling, Geomagnetism, Geography. Anthropology. Recreation, Geodesy, QB275-343, Geology, QE1-996.5
Abstract

Abstract In December 2019, the 13th revision of the International Geomagnetic Reference Field (IGRF) was released by the International Association of Geomagnetism and Aeronomy (IAGA) Division V Working Group V-MOD. This revision comprises two new spherical harmonic main field models for epochs 2015.0 (DGRF-2015) and 2020.0 (IGRF-2020) and a model of the predicted secular variation for the interval 2020.0 to 2025.0 (SV-2020-2025). The models were produced from candidates submitted by fifteen international teams. These teams were led by the British Geological Survey (UK), China Earthquake Administration (China), Universidad Complutense de Madrid (Spain), University of Colorado Boulder (USA), Technical University of Denmark (Denmark), GFZ German Research Centre for Geosciences (Germany), Institut de physique du globe de Paris (France), Institut des Sciences de la Terre (France), Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation (Russia), Kyoto University (Japan), University of Leeds (UK), Max Planck Institute for Solar System Research (Germany), NASA Goddard Space Flight Center (USA), University of Potsdam (Germany), and Université de Strasbourg (France). The candidate models were evaluated individually and compared to all other candidates as well to the mean, median and a robust Huber-weighted model of all candidates. These analyses were used to identify, for example, the variation between the Gauss coefficients or the geographical regions where the candidate models strongly differed. The majority of candidates were sufficiently close that the differences can be explained primarily by individual modeling methodologies and data selection strategies. None of the candidates were so different as to warrant their exclusion from the final IGRF-13. The IAGA V-MOD task force thus voted for two approaches: the median of the Gauss coefficients of the candidates for the DGRF-2015 and IGRF-2020 models and the robust Huber-weighted model for the predictive SV-2020-2025. In this paper, we document the evaluation of the candidate models and provide details of the approach used to derive the final IGRF-13 products. We also perform a retrospective analysis of the IGRF-12 SV candidates over their performance period (2015–2020). Our findings suggest that forecasting secular variation can benefit from combining physics-based core modeling with satellite observations.

Published
2021
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3. International Geomagnetic Reference Field: the thirteenth generation

Author

P. Alken, E. Thébault, C. D. Beggan, H. Amit, J. Aubert, J. Baerenzung, T. N. Bondar, W. J. Brown, S. Califf, A. Chambodut, A. Chulliat, G. A. Cox, C. C. Finlay, A. Fournier, N. Gillet, A. Grayver, M. D. Hammer, M. Holschneider, L. Huder, G. Hulot, T. Jager, C. Kloss, M. Korte, W. Kuang, A. Kuvshinov, B. Langlais, J.-M. Léger, V. Lesur, P. W. Livermore, F. J. Lowes, S. Macmillan, W. Magnes, M. Mandea, S. Marsal, J. Matzka, M. C. Metman, T. Minami, A. Morschhauser, J. E. Mound, M. Nair, S. Nakano, N. Olsen, F. J. Pavón-Carrasco, V. G. Petrov, G. Ropp, M. Rother, T. J. Sabaka, S. Sanchez, D. Saturnino, N. R. Schnepf, X. Shen, C. Stolle, A. Tangborn, L. Tøffner-Clausen, H. Toh, J. M. Torta, J. Varner, F. Vervelidou, P. Vigneron, I. Wardinski, J. Wicht, A. Woods, Y. Yang, Z. Zeren, and B. Zhou

Subjects
IGRF, Magnetic field modeling, Geomagnetism, Geography. Anthropology. Recreation, Geodesy, QB275-343, Geology, QE1-996.5
Abstract

Abstract In December 2019, the International Association of Geomagnetism and Aeronomy (IAGA) Division V Working Group (V-MOD) adopted the thirteenth generation of the International Geomagnetic Reference Field (IGRF). This IGRF updates the previous generation with a definitive main field model for epoch 2015.0, a main field model for epoch 2020.0, and a predictive linear secular variation for 2020.0 to 2025.0. This letter provides the equations defining the IGRF, the spherical harmonic coefficients for this thirteenth generation model, maps of magnetic declination, inclination and total field intensity for the epoch 2020.0, and maps of their predicted rate of change for the 2020.0 to 2025.0 time period.

Published
2021
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4. Can Machine Learning Reveal Precursors of Reversals of the Geomagnetic Axial Dipole Field?

Author

Kyle Gwirtz, T Davis, M Morzfeld, C Constable, A Fournier, and G Hulot

Subjects
Geophysics
Abstract

It is well known that the axial dipole part of Earth’s magnetic field reverses polarity, so that the magnetic North Pole becomes the South Pole and vice versa. The timing of reversals is well documented for the past 160 Myr, but the conditions that lead to a reversal are still not well understood. It is not known if there are reliable ‘precursors’ of reversals (events that indicate that a reversal is upcoming) or what they might be. We investigate if machine learning (ML) techniques can reliably identify precursors of reversals based on time-series of the axial magnetic dipole field. The basic idea is to train a classifier using segments of time-series of the axial magnetic dipole. This training step requires modification of standard ML techniques to account for the fact that we are interested in rare events—a reversal is unusual, while a non-reversing field is the norm. Without our tweak, the ML classifiers lead to useless predictions. Perhaps even more importantly, the usable observational record is limited to 0–2 Ma and contains only five reversals, necessitating that we determine if the data are even sufficient to reliably train and validate an ML algorithm. To answer these questions we use several ML classifiers (linear/non-linear support vector machines and long short-term memory networks), invoke a hierarchy of numerical models (from simplified models to 3-D geodynamo simulations), and two palaeomagnetic reconstructions (PADM2M and Sint-2000). The performance of the ML classifiers varies across the models and the observational record and we provide evidence that this is not an artefact of the numerics, but rather reflects how ‘predictable’ a model or observational record is. Studying models of Earth’s magnetic field via ML classifiers thus can help with identifying shortcomings or advantages of the various models. For Earth’s magnetic field, we conclude that the ability of ML to identify precursors of reversals is limited, largely due to the small amount and low frequency resolution of data, which makes training and subsequent validation nearly impossible. Put simply: the ML techniques we tried are not currently capable of reliably identifying an axial dipole moment (ADM) precursor for geomagnetic reversals. This does not necessarily imply that such a precursor does not exist, and improvements in temporal resolution and length of ADM records may well offer better prospects in the future.

Published
2022
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7. Can machine learning reveal precursors of reversals of the geomagnetic axial dipole field?

Author

K Gwirtz, T Davis, M Morzfeld, C Constable, A Fournier, and G Hulot

Subjects
Geophysics, Geochemistry and Petrology, Physics::Space Physics, Computer Science::Databases, Physics::Geophysics
Abstract

SUMMARY It is well known that the axial dipole part of Earth’s magnetic field reverses polarity, so that the magnetic North Pole becomes the South Pole and vice versa. The timing of reversals is well documented for the past 160 Myr, but the conditions that lead to a reversal are still not well understood. It is not known if there are reliable ‘precursors’ of reversals (events that indicate that a reversal is upcoming) or what they might be. We investigate if machine learning (ML) techniques can reliably identify precursors of reversals based on time-series of the axial magnetic dipole field. The basic idea is to train a classifier using segments of time-series of the axial magnetic dipole. This training step requires modification of standard ML techniques to account for the fact that we are interested in rare events—a reversal is unusual, while a non-reversing field is the norm. Without our tweak, the ML classifiers lead to useless predictions. Perhaps even more importantly, the usable observational record is limited to 0–2 Ma and contains only five reversals, necessitating that we determine if the data are even sufficient to reliably train and validate an ML algorithm. To answer these questions we use several ML classifiers (linear/non-linear support vector machines and long short-term memory networks), invoke a hierarchy of numerical models (from simplified models to 3-D geodynamo simulations), and two palaeomagnetic reconstructions (PADM2M and Sint-2000). The performance of the ML classifiers varies across the models and the observational record and we provide evidence that this is not an artefact of the numerics, but rather reflects how ‘predictable’ a model or observational record is. Studying models of Earth’s magnetic field via ML classifiers thus can help with identifying shortcomings or advantages of the various models. For Earth’s magnetic field, we conclude that the ability of ML to identify precursors of reversals is limited, largely due to the small amount and low frequency resolution of data, which makes training and subsequent validation nearly impossible. Put simply: the ML techniques we tried are not currently capable of reliably identifying an axial dipole moment (ADM) precursor for geomagnetic reversals. This does not necessarily imply that such a precursor does not exist, and improvements in temporal resolution and length of ADM records may well offer better prospects in the future.

Published
2022
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8. Impact of the Earth’s magnetic field secular drift on the low altitude proton radiation belt from years 1900 to 2050

Author

Denis Standarovski, S. Bourdarie, Robert Ecoffet, Julien Aubert, G. Hulot, Angélica Sicard, Alexandre Fournier, ONERA / DPHY, Université de Toulouse [Toulouse], ONERA-PRES Université de Toulouse, Institut de Physique du Globe de Paris (IPGP), 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), Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), PRES Université de Toulouse-ONERA, and Institut de Physique du Globe de Paris

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Nuclear and High Energy Physics, 010504 meteorology & atmospheric sciences, Proton, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Radiation, 01 natural sciences, Space exploration, CHAMP MAGNETIQUE, Altitude, Proton radiation, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Electrical and Electronic Engineering, Aerospace engineering, TRAPPED PROTONS, 0105 earth and related environmental sciences, Spacecraft, 010308 nuclear & particles physics, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, SOUTH ATLANTIC ANOMALY FORECAST, CEINTURES DE RADIATION, RADIATION BELTS, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Magnetic field, [SPI.ELEC]Engineering Sciences [physics]/Electromagnetism, Earth's magnetic field, Nuclear Energy and Engineering, 13. Climate action, Physics::Space Physics, Environmental science, Index Terms-radiation belts, Astrophysics::Earth and Planetary Astrophysics, business
Abstract

International audience; The effects of the space radiation environment on spacecraft systems and instruments are significant design considerations for space missions. In order to meet these challenges and have reliable, cost-effective designs, the radiation environment must be understood and accurately modeled. The low altitude proton environment varies slowly in time due to the secular drift of the Earth’s main magnetic field and due to the evolution of the solar cycle. The purpose of this paper is to extend the OPAL model [1] capabilities by introducing a prediction of the Earth’s main magnetic field model up to year 2050. Impact on low altitude spacecraft radiation specification for next space missions is then assessed.

Published
2018

9. Chemical studies of marine invertebrates. XXXVII(1). Three novel meroditerpenoids from the sponge strongylophora durissima(2)

Author

J. C. Braekman, Désiré Daloze, G. Hulot, Bernard Tursch, M. Van Meerssche, Jean-Paul Declercq, and Gabriel Germain

Subjects
Sponge, biology, Chemical engineering, Chemistry, Spectral properties, Organic chemistry, General Chemistry, Marine invertebrates, biology.organism_classification
Abstract

Three novel meroditerpenoids, strongylophorine‐1 (1), ‐2 (2) and ‐3 (3) have been isolated from the sponge Strongylophora durissima, Strongylophorine‐1 and ‐3 possess structure 1 and 3 respectively, as established by their spectral properties, hemisynthesis and chemical intercorrelation. The structure of strongylophorine‐2 has been shown to be 2 by X‐ray diffraction analysis on its monoacetylderivative (13). Copyright © 1978 Wiley‐VCH Verlag GmbH & Co. KGaA, Weinheim

Published
2010

10. The Earth’s Magnetic Field in the Space Age: An Introduction to Terrestrial Magnetism

Author

Ulrich R. Christensen, Nils Olsen, G. Hulot, Catherine Constable, André Balogh, and Mioara Mandea

Subjects
Solar System, Engineering, Planetary science, Earth's magnetic field, Space and Planetary Science, business.industry, Magnetism, Astronomy, Astronomy and Astrophysics, Space Science, business, Space Age
Abstract

The series of papers presented in this issue of Space Science Research (reprinted as Volume 36 in the Space Science Series of ISSI) is the result of a fruitful workshop that took place at the International Space Science Institute (ISSI), in Bern, Switzerland, during the week of March 9–13, 2009. Focussing on the (still very broad) topic of Terrestrial Magnetism, this workshop was the last of a series of three that aimed to present, discuss and summarize recent advances in our understanding of magnetic fields in the solar system. The earlier workshops, on solar and on planetary magnetism, were held in January and September 2008

Published
2010

11. Sources of the Geomagnetic Field and the Modern Data That Enable Their Investigation

Author

Nils Olsen, Terence J. Sabaka, and G. Hulot

Subjects
Superposition principle, Earth's magnetic field, Field (physics), Physics::Space Physics, Magnetosphere, Geophysics, Ionosphere, Outer core, Geology, Physics::Geophysics, Dynamo, Magnetic field
Abstract

The geomagnetic field one can measure at the Earth’s surface or on board satellites is the sum of contributions from many different sources. These sources have different physical origins and can be found both below (in the form of electrical currents and magnetized material) and above (only in the form of electrical currents) the Earth’s surface. Each source happens to produce a contribution with rather specific spatio-temporal properties. This fortunate situation is what makes the identification and investigation of the contribution of each source possible, provided appropriate observational data sets are available and analyzed in an adequate way to produce the so-called geomagnetic field models. Here we provide a general overview of the various sources that contribute to the observed geomagnetic field, and of the modern data that enable their investigation via such procedures. The Earth has a large and complicated magnetic field, a major part of which is produced by a self-sustaining dynamo operating in the fluid outer core. What is measured at or near the surface of the Earth, however, is the superposition of the core field and of additional fields caused by magnetized rocks in the Earth’s crust, by electric currents flowing in the ionosphere, magnetosphere and oceans, and by currents induced in the Earth by the time-varying external fields. The sophisticated separation of these various fields and the accurate determination of their spatial and temporal structure based on magnetic field observations is a significant challenge, which requires advanced modeling techniques (see e.g., Hulot et al. 2007). These techniques rely on a number of mathematical properties which we review in the accompanying chapter by Sabaka et al. (2010), entitled “Mathematical Properties Relevant to Geomagnetic Field Modelling”. But as many of those properties have been derived by relying on assumptions motivated by the nature of the various sources of the Earth’s magnetic field and of the available observations, it is important that a general overview of those sources and observations be given. This is precisely the purpose of the present chapter. It will first describe the various sources that contribute to the Earth’s magnetic field (Sect. 1) and next discuss the observations currently available to investigate them (Sect. 2). Special emphasis is given on data collected by satellites, since these are extensively used for modeling the present magnetic field. We will conclude with a few words with respect to the way the fields those sources produce can be identified and investigated, thanks to geomagnetic field modeling. E-mail: nio@space.dtu.dk

Published
2015

12. The Present and Future Geomagnetic Field

Author

Nils Olsen, Terence J. Sabaka, G. Hulot, and Alexandre Fournier

Subjects
Field (physics), Magnetism, Magnetometer, Magnetosphere, Dipole model of the Earth's magnetic field, Geophysics, Physics::Geophysics, law.invention, Magnetic field, Earth's magnetic field, Geography, law, Physics::Space Physics, Dynamo theory
Abstract

The Earth's magnetic field is the result of the superposition of a main field produced by the geodynamo within the core and of many other fields produced by a variety of secondary sources. Unfortunately, magnetometers can only measure the resulting field, and a single measurement cannot distinguish the contributions from each source. However, provided enough ground and satellite measurements are being acquired and processed in appropriate ways, a separation of the contributions from each type of field can be achieved and global models of the Earth's magnetic field constructed. The main purpose of this chapter is to provide an up-to-date review of such global models. We introduce the relevant types of magnetic data, review the models, and focus on the current behavior of the main field. We also report on the emerging field of geomagnetic data assimilation, which aims at both improving our understanding of the geodynamo and forecasting the main field evolution.

Published
2015

13. DYNAMO: a Mars upper atmosphere package for investigating solar wind interaction and escape processes, and mapping Martian fields

Author

Jean-Claude Gérard, Jean-André Sauvaud, Jacques Porteneuve, Andrew F. Nagy, Fritz Primdahl, Janet G. Luhmann, Mustapha Meftah, François Leblanc, David L. Mitchell, Eric Chassefière, Sándor Szalai, G. Cerutti-Maori, Sue Smrekar, Sho Sasaki, F. Barlier, Michael E. Purucker, M. Mandea, Karoly Szego, Jean-Jacques Berthelier, Mario H. Acuña, G. Hulot, Thomas H. Zurbuchen, Doris Breuer, Robert Lin, Stephen W. Bougher, G. M. Keating, Michel Parrot, Eric Quémerais, Jean Lilensten, Jean-Pierre Barriot, H. Waite, John Clarke, Christian Malique, Pierre Rochus, François Forget, Jean-Gabriel Trotignon, Stefano Orsini, Jean-Loup Bertaux, Gérard Chanteur, S. Barabash, Bruce M. Jakosky, Henri Rème, Michel Menvielle, P. Touboul, D. T. Young, 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), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Institut de Physique du Globe de Paris (IPGP), 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), Danish Space Research Institute (DSRI), Centre d'étude spatiale des rayonnements (CESR), 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), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Swedish Institute of Space Physics [Kiruna] (IRF), 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), Southwest Research Institute [San Antonio] (SwRI), Boston University [Boston] (BU), 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), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), 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), 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), Observatoire Midi-Pyrénées (OMP), 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, NASA Goddard Space Flight Center (GSFC), Institut für Planetologie [Münster], Westfälische Wilhelms-Universität Münster = University of Münster (WWU), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], The University of Tokyo (UTokyo), The George Washington University (GW), ONERA - The French Aerospace Lab [Châtillon], ONERA-Université Paris Saclay (COmUE), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Istituto di Fisica dello Spazio Interplanetario (IFSI), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Institut Pierre-Simon-Laplace (IPSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), 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)-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, University of California [Berkeley], University of California-University of California, Université d'Orléans (UO)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), 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), Westfälische Wilhelms-Universität Münster (WWU), California Institute of Technology (CALTECH)-NASA, and Consiglio Nazionale delle Ricerche (CNR)

Subjects
Atmospheric Science, 010504 meteorology & atmospheric sciences, Mars, Aerospace Engineering, Magnetosphere, 7. Clean energy, 01 natural sciences, Astrobiology, 0103 physical sciences, Gravity field, Upper atmosphere, Mercury's magnetic field, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Martian, Atmospheric escape, Astronomy and Astrophysics, Mars Exploration Program, Solar wind, Escape, Magnetic field, Geophysics, [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, Physics::Space Physics, General Earth and Planetary Sciences, Timekeeping on Mars, Astrophysics::Earth and Planetary Astrophysics, Thermosphere, Geology
Abstract

International audience; DYNAMO is a small multi-instrument payload aimed at characterizing current atmospheric escape, which is still poorly constrained, and improving gravity and magnetic field representations, in order to better understand the magnetic, geologic and thermal history of Mars. The internal structure and evolution of Mars is thought to have influenced climate evolution. The collapse of the primitive magnetosphere early in Mars history could have enhanced atmospheric escape and favored transition to the present arid climate. These objectives are achieved by using a low periapsis orbit. DYNAMO has been proposed in response to the AO released in February 2002 for instruments to be flown as a complementary payload onboard the CNES Orbiter to Mars (MO-07), foreseen to be launched in 2007 in the framework of the French PREMIER Mars exploration program. MO-07 orbital phase 2b (with an elliptical orbit of periapsis 170 km), and in a lesser extent 2a, offers an unprecedented opportunity to investigate by in situ probing the chemical and dynamical properties of the deep ionosphere, thermosphere, and the interaction between the atmosphere and the solar wind, and therefore the present atmospheric escape rate. Ultraviolet remote sensing is an essential complement to characterize high, tenuous, layers of the atmosphere. One Martian year of operation, with about 5,000 low passes, should allow DYNAMO to map in great detail the residual magnetic field, together with the gravity field. Additional data on the internal structure will be obtained by mapping the electric conductivity, sinergistically with the NETLANDER magnetic data. Three options have been recommended by the International Science and Technical Review Board (ISTRB), who met on July 1st and 2nd, 2002. One of them is centered on DYNAMO. The final choice, which should be made before the end of 2002, will depend on available funding resources at CNES.

Published
2004

15. Swarm SCARF Dedicated Lithospheric Field Inversion chain

Author

E. Thébault, P. Vigneron, S. Maus, A. Chulliat, O. Sirol, G. Hulot, Institut de Physique du Globe de Paris (IPGP), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), NOAA National Geophysical Data Center (NGDC), National Oceanic and Atmospheric Administration (NOAA), and 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)

Subjects
010504 meteorology & atmospheric sciences, Space and Planetary Science, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Physics::Space Physics, space magnetometry, Lithospheric magnetic field, Swarm, Geology, 010502 geochemistry & geophysics, 01 natural sciences, 0105 earth and related environmental sciences
Abstract

International audience; The forthcoming Swarm satellite mission is a constellation of three satellites dedicated to the study of the geomagnetic field. The orbital characteristics of the mission, which includes a pair of satellites flying side by side, has prompted new efforts in data processing and modeling. A consortium of several research institutions has been selected by the European Space Agency (ESA) to provide a number of Level-2 data products which will be made available to the scientific community. Within this framework, specific tools have been tailor-made to better recover the lithospheric magnetic field contribution. These tools take advantage of gradient properties measured by the lower pair of Swarm satellites and rely on a regional modeling scheme designed to better detect signatures of small spatial scales. We report on a processing chain specifically designed for the Swarm mission. Using an End-to-End simulation, we show that the tools developed are operational. The chain generates a model that meets the primary scientific objectives of the Swarm mission. We also discuss refinements that could also be implemented during the Swarm operational phase to further improve lithospheric field models and reach unprecedented spatial resolution.

Published
2013

17. Mathematical Properties Relevant to Geomagnetic Field Modeling

Author

Terence J. Sabaka, Nils Olsen, and G. Hulot

Subjects
Earth's magnetic field, Variables, Field (physics), Basis (linear algebra), Computer science, Completeness (order theory), media_common.quotation_subject, Spherical coordinate system, Uniqueness, Statistical physics, Linear combination, media_common
Abstract

Geomagnetic field modeling consists in converting large numbers of magnetic observations into a linear combination of elementary mathematical functions that best describes those observations.The set of numerical coefficients defining this linear combination is then what one refers to as a geomagnetic field model. Such models can be used to produce maps. More importantly, they form the basis for the geophysical interpretation of the geomagnetic field, by providing the possibility of separating fields produced by various sources and extrapolating those fields to places where they cannot be directly measured. In this chapter, the mathematical foundation of global (as opposed to regional) geomagnetic field modeling is reviewed, and the spatial modeling of the field in spherical coordinates is focussed. Time can be dealt with as an independent variable and is not explicitly considered. The relevant elementary mathematical functions are introduced, their properties are reviewed, and how they can be used to describe the magnetic field in a source-free (such as the Earth’s neutral atmosphere) or source-dense (such as the ionosphere) environment is explained. Completeness and uniqueness properties of those spatial mathematical representations are also discussed, especially in view of providing a formal justification for the fact that geomagnetic field models can indeed be constructed from ground-based and satellite-born observations, provided those reasonably approximate the ideal situationwhere relevant components of the field can be assumed perfectly known on spherical surfaces or shells at the time for which the model is to be recovered.

Published
2010

20. ArcheoInt: An upgraded compilation of geomagnetic field intensity data for the past ten millennia and its application to the recovery of the past dipole moment

Author

A. Genevey, Y. Gallet, C. G. Constable, Monika Korte, G. Hulot, Centre de recherche et de restauration des musées de France (C2RMF), Ministère de la Culture et de la Communication (MCC)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique du Globe de Paris, Institute of Geophysics and Planetary Physics [San Diego] (IGPP), Scripps Institution of Oceanography (SIO), University of California [San Diego] (UC San Diego), University of California-University of California-University of California [San Diego] (UC San Diego), University of California-University of California, and GeoForschungsZentrum - Helmholtz-Zentrum Potsdam (GFZ)

Subjects
data compilation, dipole evolution, Holocene, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], regional variations, 550 - Earth sciences, archeointensity
Abstract

This paper presents a compilation of intensity data covering the past 10 millennia (ArcheoInt). This compilation, which upgrades the one of Korte et al. (2005), contains 3648 data and incorporates additional intensity and directional data sets. A large majority of these data (∼87%) were acquired on archeological artifacts, and the remaining ∼13% correspond to data obtained from volcanic products. The present compilation also includes important metadata for evaluating the intensity data quality and providing a foundation to guide improved selection criteria. We show that ∼50% of the data set fulfill reasonable reliability standards which take into account the anisotropic nature of most studied objects (potsherds), the stability of the magnetization, and the data dispersion. The temporal and geographical distributions of this sub–data set are similar to those of the main data set, with ∼72% of the data dated from the past three millennia and ∼76% obtained from western Eurasia. Approximately half of the selected intensity data are associated with at least an inclination value. To constrain the axial and full dipole evolution over the past three millennia requires that we avoid any overrepresentation of the western Eurasian data. We introduce a first-order regional weighting scheme based on the definition of eight widely distributed regions of 30° width within which the selected data are numerous enough. The regional curves of virtual axial dipole moments (VADM) and of mixed VADM-virtual dipole moments (VDM) averaged over sliding windows of 200 years and 500 years testify for strong contributions from either equatorial dipole or nondipole components. The computation of global VADM and mixed VADM/VDM variation curves, assuming an equal weight for each region, yields a dipole evolution marked by a distinct minimum around 0 B.C./A.D. followed by a maximum around the third-fourth century A.D. A second minimum is present around the eighth century A.D. This variation pattern is compatible with the one deduced from earlier, more sophisticated analysis based on the inversion of both intensity and directional data. In particular, there is a good agreement among all VADMs and dipole moment estimates over the historical period, which further strengthens the validity of our weighting scheme.

Published
2008

21. Swarm End-to-End mission performance simulator study : Final Report

Author

N. Olsen, E. Friis-Christensen, G. Hulot, Monika Korte, A. Kuvshinov, Vincent Lesur, Hermann Lühr, S. Macmillan, M. Mandea, S. Maus, M. Purucker, C. Reigber, Patricia Ritter, Martin Rother, T. Sabaka, P. Tarits, and A. Thomson

Subjects
550 - Earth sciences
Published
2004

22. The Lavoisier mission : A system of descent probe and balloon flotilla for geochemical investigation of the deep atmosphere and surface of Venus

Author

V. Linkin, M. Roos-Serote, G. Vitter, G. Hulot, Fredric W. Taylor, Rafael Rodrigo, Albert Jambon, Dmitri Titov, Jean-Jacques Berthelier, Jean-Christophe Sabroux, Mioara Mandea, Bruno Bézard, H. U. Keller, François Raulin, Ari-Matti Harri, B. Landeau, Y. Cohen, S. Vergniole, Cs. Ferencz, J. L. Bertaux, D. Coscia, Jean-Pierre Pommereau, Oleg Korablev, Karoly Szego, Patrice Coll, Doris Breuer, Eric Quémerais, Ph. Lognonné, A. Le Pichon, J. F. Pineau, Eric Chassefière, Philippe Sarda, Pascal Rannou, Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-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), 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), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire Magie, Université Pierre et Marie Curie - Paris 6 (UPMC), Université Paris-Sud - Paris 11 (UP11), Institut de Protection et Sûreté Nucléaire (IPSN), Laboratoire d'Electrochimie et de Physico-chimie des Matériaux et des Interfaces (LEPMI ), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National Polytechnique de Grenoble (INPG)-Institut de Chimie du CNRS (INC)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut de Physique du Globe de Paris (IPGP), 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), Société ALBEDO Technologies, 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), Pôle Planétologie du LESIA, 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)-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), Max-Planck-Institut für Aeronomie (MPI Aeronomie), Max-Planck-Gesellschaft, Institut für Planetologie [Münster], Westfälische Wilhelms-Universität Münster = University of Münster (WWU), Hungarian Academy of Sciences (MTA), Eötvös Loránd Geophysical Institute (ELGI), Observatório Astronómico de Lisboa, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), University of Oxford, Finnish Meteorological Institute (FMI), Université Pierre et Marie Curie - Paris 6 (UPMC)-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), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), and University of Oxford [Oxford]

Subjects
Physics, Atmospheric Science, geography, geography.geographical_feature_category, biology, Meteorology, Aerospace Engineering, Astronomy and Astrophysics, Venus, Crust, Geophysics, biology.organism_classification, Atmosphere, Outgassing, Volcano, Space and Planetary Science, Very-long-baseline interferometry, Radiative transfer, General Earth and Planetary Sciences, Radiometry, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Lavoisier mission is a joint effort of eight European countries and a technological challenge aimed at investigating the lower atmosphere and the surface of Venus. The mission consists of a descent probe and three balloons to be deployed below the cloud deck. Its main scientific objectives may be summarized as following : (i) composition of the deep atmosphere : noble gas (elemental/isotopic), molecular species (elemental/isotopic), oxygen fugacity; vertical/horizontal/temporal variability; (ii) infrared spectroscopy and radiometry (molecular composition, radiative transfer); (iii) dynamics of the atmosphere : p, T, acceleration measurements, balloon localization through VLBI, meteorological events signed by acoustic waves, atmospheric mixing as imprinted on radioactive tracers; (iv) surface morphology and mineralogy through near infrared imaging on dayside, surface temperature through NIR imaging on nightside. Additional tentative objectives are search for (a) atmospheric electrical activity (optically, radioelectrically, acoustically), (b) crustal outgassing and/or volcanic activity : acoustic activity, horizontal/vertical distribution of radioactive tracers, (c) seismic activity : acoustic waves transmitted from crust to atmosphere, and (d) remanent and/or intrinsic magnetic field. Lavoisier was proposed to ESA in response to the F2/F3 mission Announcement of Opportunity at the beginning of 2000, but it was not selected for the assessment study, A wide international partnership was created for this occasion, including Finland (FMI), France (IPSL, MAGIE, Universite Orsay, IPSN, INPG, CEA, IPGP, Obs. Paris-Meudon), Germany (MPAe, Univ. Muenster), Hungary (KFKI, Univ. Eotvos), Portugal (OAL), Russia (IKI), Spain (IAA), United Kingdom (Univ. Oxford). (C) 2002 COSPAR. Published by Elsevier Science Ltd. All rights reserved.

Published
2002

23. 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

24. [Diagnostic difficulties of myocardial infarct in an admissions and emergency service: influence of age]

Author

P, Le Conte, G, Hulot de Collart, J C, Chevalier, D, Yatim, M D, Touzé, F, Garrec, and D, Baron

Subjects
Aged, 80 and over, Male, Age Factors, Myocardial Infarction, Clinical Enzyme Tests, Isoenzymes, Electrocardiography, Humans, Female, Emergency Service, Hospital, Creatine Kinase, Biomarkers, Aged, Retrospective Studies
Abstract

To analyze the clinical signs and electrocardiographic and enzyme data in patients admitted to an emergency ward for myocardial infarction in order to highlight diagnostic pitfalls.All patients admitted to our emergency ward between October 1995 and October 1996 with elevated myoglobulin or creatinine phosphokinase (CPK) levels (n = 457 patients) were included in the study series. Patient files were randomly selected (n = 257 files) for review by an emergency ward specialist and a cardiologist to identify cases of myocardial infarction (n = 88 patients, mean age 73.4 +/- 15.2 years). Clinical, electrical and enzyme data (including CPK-MB) were analyzed.The patients had been referred for chest pain (69%), dyspnea (24%) or another disorder (7%). Pain was located in the retrosternal area in 51%, in the lower chest in 19% and elsewhere in 30%. Delay between onset of pain and transfer to the emergency ward was 5 h 20 min +/- 6 h. Signs of left heart failure were observed in 50% of the patients. The admission electrocardiogram showed complete criteria for myocardial infarction in 43% of the cases, incomplete criteria in 21% and was non-contributive in 36%. Enzyme results were elevated in 78% of the cases at the first assay and in 98.2% at the second assay. Both typical chest pain and ECG were observed in only 30% of the cases. Chest pain was present in 55% of the patients over 75 years of age and in 81% of those under 75 years (p = 0.007).A typical syndrome is observed in less than one-third of all patients with myocardial infarction admitted to emergency wards. The frequency of atypical presentations increases with age.

Published
1998

25. Reducing the Backus effect given some knowledge of the dip-equator

Author

G. Hulot, P. Ultré-Guérard, M. Hamoudi, Institut de Physique du Globe de Paris (IPGP), 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), Université des Sciences et de la Technologie Houari Boumediene [Alger] (USTHB), and Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
Ideal (set theory), 010504 meteorology & atmospheric sciences, Computer science, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Perspective (graphical), Equator, 010502 geochemistry & geophysics, Geodesy, 01 natural sciences, Field (geography), Secular variation, Geophysics, Earth's magnetic field, General Earth and Planetary Sciences, Satellite, Intensity (heat transfer), 0105 earth and related environmental sciences
Abstract

International audience; Geomagnetic field models computed from intensity measurements on or near the Earth's surface are plagued with strong errors known as the "Backus ef-fect". These errors are related to the mathematical non-uniqueness of the solution which can be theoretically removed by the knowledge of the dip-equator location. Here, we present. a new method for computing models using intensity data and additional information about the location of the dip-equator. We first give a numerical validation of this approach in an ideal case in which the dip-equator can be assumed to be perfectly located. We then show that in practice, updating a good past model of the field with a model of secular variation can constrain the location of the dip-equator sufficiently for our method to be useful. Implications for the planning of future satellite missions are briefly discussed.

Published
1998

29. The impact of active delivery of the anterior arm during vacuum-assisted vaginal delivery on perineal tears: a clinical practice evaluation.

Author

Hulot G, Ramanah R, Riethmuller D, and Mottet N

Subjects
Anal Canal injuries, Arm, Delivery, Obstetric, Episiotomy adverse effects, Female, Humans, Perineum injuries, Pregnancy, Retrospective Studies, Risk Factors, Lacerations therapy, Obstetric Labor Complications etiology, Obstetric Labor Complications therapy
Abstract

Objective: Our purpose was to evaluate the impact of active delivery of the anterior arm with Couder's Maneuver (CM) during vacuum-assisted vaginal delivery (VAVD) on perineal tears. This maneuver can be beneficial because it has the advantage of reducing fetal biacromial diameter. Methods: This monocentric retrospective study compared two non-concurrent cohorts of nulliparous women before and after implementation of a systematic CM during VAVD: Cohort 1 from 1 January to 31 December 2006 without CM and Cohort 2 from 1 January to 31 December 2016 with systematic CM. This study reviewed all births during these two periods. All live-born singleton pregnancies where VAVD occurred after 37 weeks of gestation were included. The principal endpoint was the type of perineal tear. Results: In total, there were 179 VAVD in the Cohort 1 and 267 VAVD in the Cohort 2. In the Cohort 2, 233 VAVD (87.3%) were performed with systematic CM. No episiotomy was performed in both cohorts. There was a significant decrease in the rate of second-degree perineal tears between the two cohorts (42.4 versus 15%, p  < .001) and a significant increase in the rate of intact perineum (34.1 versus 54.7%, p  < .001). There was no influence of CM on the rate of obstetrical anal sphincter injury (3.9 versus 2.6%, p  = .44). Conclusions: Practicing this maneuver could improve the perineal prognosis during VAVD in nulliparous women.

Published
2020
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30. Thermochemical flows couple the Earth's inner core growth to mantle heterogeneity.

Author

Aubert J, Amit H, Hulot G, and Olson P

Abstract

Seismic waves sampling the top 100 km of the Earth's inner core reveal that the eastern hemisphere (40 degrees E-180 degrees E) is seismically faster, more isotropic and more attenuating than the western hemisphere. The origin of this hemispherical dichotomy is a challenging problem for our understanding of the Earth as a system of dynamically coupled layers. Previously, laboratory experiments have established that thermal control from the lower mantle can drastically affect fluid flow in the outer core, which in turn can induce textural heterogeneity on the inner core solidification front. The resulting texture should be consistent with other expected manifestations of thermal mantle control on the geodynamo, specifically magnetic flux concentrations in the time-average palaeomagnetic field over the past 5 Myr, and preferred eddy locations in flows imaged below the core-mantle boundary by the analysis of historical geomagnetic secular variation. Here we show that a single model of thermochemical convection and dynamo action can account for all these effects by producing a large-scale, long-term outer core flow that couples the heterogeneity of the inner core with that of the lower mantle. The main feature of this thermochemical 'wind' is a cyclonic circulation below Asia, which concentrates magnetic field on the core-mantle boundary at the observed location and locally agrees with core flow images. This wind also causes anomalously high rates of light element release in the eastern hemisphere of the inner core boundary, suggesting that lateral seismic anomalies at the top of the inner core result from mantle-induced variations in its freezing rate.

Published
2008
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31. Small-scale structure of the geodynamo inferred from Oersted and Magsat satellite data.

Author

Hulot G, Eymin C, Langlais B, Mandea M, and Olsen N

Abstract

The 'geodynamo' in the Earth's liquid outer core produces a magnetic field that dominates the large and medium length scales of the magnetic field observed at the Earth's surface. Here we use data from the currently operating Danish Oersted satellite, and from the US Magsat satellite that operated in 1979/80, to identify and interpret variations in the magnetic field over the past 20 years, down to length scales previously inaccessible. Projected down to the surface of the Earth's core, we found these variations to be small below the Pacific Ocean, and large at polar latitudes and in a region centred below southern Africa. The flow pattern at the surface of the core that we calculate to account for these changes is characterized by a westward flow concentrated in retrograde polar vortices and an asymmetric ring where prograde vortices are correlated with highs (and retrograde vortices with lows) in the historical (400-year average) magnetic field. This pattern is analogous to those seen in a large class of numerical dynamo simulations, except for its longitudinal asymmetry. If this asymmetric state was reached often in the past, it might account for several persistent patterns observed in the palaeomagnetic field. We postulate that it might also be a state in which the geodynamo operates before reversing.

Published
2002
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32. [Diagnostic difficulties of myocardial infarct in an admissions and emergency service: influence of age].

Author

Le Conte P, Hulot de Collart G, Chevalier JC, Yatim D, Touzé MD, Garrec F, and Baron D

Subjects
Age Factors, Aged, Aged, 80 and over, Biomarkers blood, Clinical Enzyme Tests, Creatine Kinase blood, Electrocardiography, Female, Humans, Isoenzymes, Male, Myocardial Infarction physiopathology, Retrospective Studies, Emergency Service, Hospital, Myocardial Infarction diagnosis
Abstract

Objective: To analyze the clinical signs and electrocardiographic and enzyme data in patients admitted to an emergency ward for myocardial infarction in order to highlight diagnostic pitfalls., Patients and Methods: All patients admitted to our emergency ward between October 1995 and October 1996 with elevated myoglobulin or creatinine phosphokinase (CPK) levels (n = 457 patients) were included in the study series. Patient files were randomly selected (n = 257 files) for review by an emergency ward specialist and a cardiologist to identify cases of myocardial infarction (n = 88 patients, mean age 73.4 +/- 15.2 years). Clinical, electrical and enzyme data (including CPK-MB) were analyzed., Results: The patients had been referred for chest pain (69%), dyspnea (24%) or another disorder (7%). Pain was located in the retrosternal area in 51%, in the lower chest in 19% and elsewhere in 30%. Delay between onset of pain and transfer to the emergency ward was 5 h 20 min +/- 6 h. Signs of left heart failure were observed in 50% of the patients. The admission electrocardiogram showed complete criteria for myocardial infarction in 43% of the cases, incomplete criteria in 21% and was non-contributive in 36%. Enzyme results were elevated in 78% of the cases at the first assay and in 98.2% at the second assay. Both typical chest pain and ECG were observed in only 30% of the cases. Chest pain was present in 55% of the patients over 75 years of age and in 81% of those under 75 years (p = 0.007)., Conclusion: A typical syndrome is observed in less than one-third of all patients with myocardial infarction admitted to emergency wards. The frequency of atypical presentations increases with age.

Published
1998

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