Author: "Miguel A. Valverde" / Publisher: hal ccsd - Searchworks@Jio Institute Digital Library Search Results

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1. Annual Appearance of Hydrogen Chloride on Mars and a Striking Similarity With the Water Vapor Vertical Distribution Observed by TGO/NOMAD

Author: Frank Daerden, Franck Lefèvre, Frédéric Schmidt, Ann Carine Vandaele, Alexander Trokhimovskiy, Frank Montmessin, James A. Whiteway, Giuliano Liuzzi, Ian Thomas, Sébastien Viscardy, Geronimo Villanueva, Justin Erwin, S. Aoki, Manish R. Patel, Jose-Juan Lopez-Moreno, Anna Fedorova, Oleg Korablev, R. T. Clancy, Bojan Ristic, Lori Neary, Giancarlo Bellucci, Miguel Lopez-Valverde, Séverine Robert, Loïc Trompet, Matteo Crismani, Kevin Olsen, Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Institut de la matière condensée et des nanosciences / Institute of Condensed Matter and Nanosciences (IMCN), Université Catholique de Louvain = Catholic University of Louvain (UCL), NASA Goddard Space Flight Center (GSFC), Department of Physics [Washington], American University Washington D.C. (AU), California State University [San Bernardino] (CSUSB), Space Science Institute [Boulder] (SSI), Centre for Research in Earth and Space Science [Toronto] (CRESS), York University [Toronto], Géosciences Paris Saclay (GEOPS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Space Science and Technology Department [Didcot] (RAL Space), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Department of Physics [Oxford], University of Oxford [Oxford], PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), European Space Agency. Grant Numbers: PEA 4000103401, 4000121493, European. Grant Number: PGC2018-101836-B-I00 and ESP2017-87143-R, Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), European Commission, European Space Agency, Agenzia Spaziale Italiana, Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Belgian Science Policy Office, National Aeronautics and Space Administration (US), and UK Space Agency
Subjects: geography, geography.geographical_feature_category, 010504 meteorology & atmospheric sciences, Atmosphere of Mars, Mars Exploration Program, 010502 geochemistry & geophysics, Atmospheric sciences, 01 natural sciences, Sink (geography), law.invention, Trace gas, chemistry.chemical_compound, Orbiter, Geophysics, chemistry, 13. Climate action, Dust storm, law, [SDU]Sciences of the Universe [physics], General Earth and Planetary Sciences, Environmental science, Hydrogen chloride, Water vapor, 0105 earth and related environmental sciences
Abstract: Hydrogen chloride (HCl) was recently discovered in the atmosphere of Mars by two spectrometers onboard the ExoMars Trace Gas Orbiter. The reported detection made in Martian Year 34 was transient, present several months after the global dust storm during the southern summer season. Here, we present the full data set of vertically resolved HCl detections obtained by the NOMAD instrument, which covers also Martian year 35. We show that the particular increase of HCl abundances in the southern summer season is annually repeated, and that the formation of HCl is independent from a global dust storm event. We also find that the vertical distribution of HCl is strikingly similar to that of water vapor, which suggests that the uptake by water ice clouds plays an important role. The observed rapid decrease of HCl abundances at the end of the southern summer would require a strong sink independent of photochemical loss. © 2021. American Geophysical Union., ExoMars is a space mission of the European Space Agency and Roscosmos. The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (IASB- BIRA), assisted by Co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS), and the United Kingdom (Open University). This project acknowledges funding by the Belgian Science Policy Office, with the financial and contractual coordination by the European Space Agency Prodex Office (PEA 4000103401 and 4000121493), by the Spanish MICINN through its Plan Nacional and by European funds under grants PGC2018-101836-B-I00 and ESP2017-87143-R (MINECO/FEDER), as well as by UK Space Agency through grants ST/V002295/1, ST/V005332/1 ST/S00145X/1 ST/S00145X/1 and ST/T002069/1, and Italian Space Agency through grant 2018-2-HH.0. This work was supported by NASA's Mars Program Office under WBS 604796, "Participation in the TGO/NOMAD Investigation of Trace Gases on Mars." The IAA/CSIC team acknowledges financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). This work was supported by the Belgian Fonds de la Recherche Scientifique-FNRS under grant numbers 30442502 (ET_HOME) and T.0171.16 (CRAMIC) and Belgian Science Policy Office BrainBe SCOOP and MICROBE Projects. S. A. is "Charge de Recherches" at the F.R.S.-FNRS. U.S. investigators were supported by the National Aeronautics and Space Administration. We acknowledge support from the Institut National des Sciences de l'Univers" (INSU), the "Centre National de la Recherche Scientifique" (CNRS) and "Centre National d'Etudes Spatiales" (CNES) through the "Programme National de Planetologie".
Published: 2021

2. On the derivation of thermospheric temperatures from dayglow emissions on Mars

Author: Maya García-Comas, Miguel Lopez-Valverde, Sergio Jiménez-Monferrer, François Forget, Francisco Gonzalez-Galindo, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 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 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), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Ministerio de Economía y Competitividad (España), and Ministerio de Ciencia e Innovación (España)
Subjects: 010504 meteorology & atmospheric sciences, Solar zenith angle, Mars, Astrophysics, Ultraviolet observations, 01 natural sciences, 7. Clean energy, Global model, Atmosphere, Altitude, 0103 physical sciences, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, Aeronomy, Astronomy and Astrophysics, Scale height, Mars Exploration Program, On board, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics]
Abstract: The Cameron bands and the UV doublet are two of the most prominent emission systems in the UV in Mars dayside. Their altitude variation has been exploited in the past to derive thermospheric temperatures from measurements obtained by the Mariner 6, 7, and 9 missions, the SPICAM instrument on board Mars Express, and the IUVS instrument on board MAVEN. Here we identify and quantify possible biases in these temperature determinations. For this purpose, we use a global model able to simulate these two emission systems, and we compare the temperature derived from the simulated emission with that predicted by the model at the same location and time. We find that an exponential fit to the scale height of the UV doublet can be used to derive temperatures with an error less than 10 K at altitudes above about 170 km and for low and moderate values of the Solar Zenith Angle. The temperature derived from the Cameron bands is biased towards higher values due to the non-negligible contribution of CO to the emission. We find that, at 170 km, the difference between the temperature derived from the Cameron bands and the UV doublet can be related to the CO abundance. Our results have implications for previous temperature determinations from the Mariners, SPICAM/MEx and IUVS/MAVEN, some of them being biased by about 25 K. © 2021 Elsevier Inc. All rights reserved., The IAA team acknowledges financial support from the Agencia Estatal de Investigacion (AEI) of the Spanish Ministerio de Ciencia, Innovacion y Universidades (MCIU) through the "Center of Excellence Severo Ochoa'' award to the Instituto de Astrofisica de Andalucia (SEV-2017-0709). FG-G and MALV are funded by the Spanish MCIU, the AEI, and EU FEDER funds under projects RTI2018-100920-J-I00 and PGC2018-101836-B-100, respectively.
Published: 2021

3. Thermal structure of the upper atmosphere of Venus simulated by a ground-to-thermosphere GCM

Author: François Lott, Gabriella Gilli, Jean-Yves Chaufray, Francisco Gonzalez-Galindo, Miguel Lopez-Valverde, Franck Lefèvre, Sébastien Lebonnois, Aurélien Stolzenbach, 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), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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)-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), HELIOS - LATMOS, Spanish MINECO, 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
Subjects: Daytime, 010504 meteorology & atmospheric sciences, biology, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astronomy and Astrophysics, Venus, Atmospheric sciences, biology.organism_classification, 01 natural sciences, Mesosphere, Atmosphere of Venus, Atmosphere, Depth sounding, 13. Climate action, Space and Planetary Science, Planet, 0103 physical sciences, Environmental science, Thermosphere, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: International audience; We present here the thermal structure of the upper atmosphere of Venus predicted by a full self-consistent Venus General Circulation Model (VGCM) developed at Laboratoire de MMétéorologie Dynamique (LMD) and extended up to the thermosphere of the planet. Physical and photochemical processes relevant at those altitudes, plus a non-orographic GW parameterisation, have been added. All those improvements make the LMD-VGCM the only existing ground-to-thermosphere 3D model for Venus: a unique tool to investigate the atmosphere of Venus and to support the exploration of the planet by remote sounding. The aim of this paper is to present the model reference results, to describe the role of radiative, photochemical and dynamical effects in the observed thermal structure in the upper mesosphere/lower thermosphere of the planet. The predicted thermal structure shows a succession of warm and cold layers, as recently observed. A cooling trend with increasing latitudes is found during daytime at all altitudes, while at nighttime the trend is inverse above about 110 km, with an atmosphere up to 15 K warmer towards the pole. The latitudinal variation is even smaller at the terminator, in agreement with observations. Below about 110 km, a nighttime warm layer whose intensity decreases with increasing latitudes is predicted by our GCM. A comparison of model results with a selection of recent measurements shows an overall good agreement in terms of trends and order of magnitude. Significant data-model discrepancies may be also discerned. Among them, thermospheric temperatures are about 40-50 K colder and up to 30 K warmer than measured at terminator and at nighttime, respectively. The altitude layer of the predicted mesospheric local maximum (between 100 and 120 km) is also higher than observed. Possible interpretations are discussed and several sensitivity tests performed to understand the data-model discrepancies and to propose future model improvements.
Published: 2017

4. MAVEN and the total electron content of the Martian ionosphere

Author: Paul R. Mahaffy, František Němec, Bruce A. Campbell, Michael Mendillo, François Forget, Majd Mayyasi, Francisco Gonzalez-Galindo, François Leblanc, Miguel Lopez-Valverde, Marissa F. Vogt, Laila Andersson, Y. J. Ma, Mehdi Benna, Jean-Yves Chaufray, Bruce M. Jakosky, Clara Narvaez, Center for Space Physics [Boston] (CSP), Boston University [Boston] (BU), NASA Goddard Space Flight Center (GSFC), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Smithsonian Institution, Faculty of Mathematics and Physics [Praha/Prague], Charles University [Prague] (CU), University of California [Los Angeles] (UCLA), University of California, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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)-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), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 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), University of California (UC), 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
Subjects: Martian, Physics, Electron density, Daytime, 010504 meteorology & atmospheric sciences, Total electron content, TEC, MAVEN, Mars, Mars Exploration Program, Atmospheric sciences, 01 natural sciences, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Geophysics, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Ionosphere, 010303 astronomy & astrophysics, Zenith, 0105 earth and related environmental sciences
Abstract: International audience; Model studies of the ionosphere of Mars under daytime conditions reveal that for solar zenith angles (SZAs) of 0°-40°, the shapes and magnitudes of the electron density profiles Ne(h) change by only small amounts. This suggests that mid-day observations made by MAVEN instruments along slanted orbit segments can be used to represent vertical profiles. The total electron content (TEC), defined as the height integral of Ne(h), is a measure of the cold plasma reservoir of the martian ionosphere. During MAVEN's Deep-Dip-#2 campaign of April 2015, observations of total ion density by NGIMS and electron density by LPW from periapse (~130 km) to 400 km were used to form topside—validated by independent diagnostics and models. Orbit-by-orbit changes in topside TEC were then used to assess the magnitudes of plasma escape associated with both large and small changes in the topside slope of Ne(h)—called an “ionopause episode.” The TEC changes due to these episodes, generalized to a global change, resulted in an escape flux of ~3 - 6 x 1024 ions/sec, an escape rate consistent with prior observation by Phobos-2, Mars Express, and MAVEN's own in-situ studies.
Published: 2017

5. In vitro and in vivo evidence for an inflammatory role of the calcium channel TRPV4 in lung epithelium: Potential involvement in cystic fibrosis

Author: Rainer Kiefmann, Lhousseine Touqui, Marie Potier-Cartereau, Christelle Coraux, Cristina Plata, Clémence Henry, Eric Morello, Mustapha Si-Tahar, Antoine Guillon, Emilie Dalloneau, Christophe Vandier, Rose-France Aimar, Maria-Teresa Pérez-Berezo, Frédéric Esnard, Nicolas Cenac, Yongzheng Wu, Miguel A. Valverde, Christian Börnchen, Centre d’Etude des Pathologies Respiratoires (CEPR), UMR 1100 (CEPR), Université de Tours (UT)-Institut National de la Santé et de la Recherche Médicale (INSERM), Université Francois Rabelais [Tours], Centre de Physiopathologie Toulouse Purpan (CPTP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées, Laboratory of Molecular Physiology and Channelopathies, Universitat Pompeu Fabra [Barcelona] (UPF), Défense innée et inflammation, Institut Pasteur [Paris]-Institut National de la Santé et de la Recherche Médicale (INSERM), Nutrition, croissance et cancer (U 1069) (N2C), Network 'Ion channels and Cancer-Canceropole Grand Ouest', Cancéropôle Grand-Ouest, Plasticité de l'épithélium respiratoire dans les conditions normales et pathologiques - UMR-S 903 (PERPMP), Université de Reims Champagne-Ardenne (URCA)-Centre Hospitalier Universitaire de Reims (CHU Reims)-Institut National de la Santé et de la Recherche Médicale (INSERM)-SFR CAP Santé (Champagne-Ardenne Picardie Santé), Université de Reims Champagne-Ardenne (URCA)-Université de Picardie Jules Verne (UPJV)-Université de Reims Champagne-Ardenne (URCA)-Université de Picardie Jules Verne (UPJV), Cardiovascular Research Center Hamburg (CVRC), University Hamburg, Universitaetsklinikum Hamburg-Eppendorf = University Medical Center Hamburg-Eppendorf [Hamburg] (UKE), This work was financially supported by the 'Johanna und Fritz Buch-Gedächtnisstiftung.' C. O. Henry was funded by 'Fonds de Dotation Recherche en Santé Respiratoire' (Paris, France), and E. Dalloneau was funded by 'Vaincre la Mucoviscidose' and by a Fédération de recherche en infectiologie travel grant. A. Guillon was funded by an Inserm 'poste d'accueil.' Part of the research was funded by fundings from the French 'Conseil Régional Centre-Val de Loire,' the Spanish Ministry of Economy and Competitiveness(SAF2012-38140), Maria de Maeztu Programme for Units of Excellence in R&D (MDM-2014-0370), Fondo de Investigación Sanitaria(RD12/0042/0014), and FEDER Funds., Université de Toulouse (UT)-Université de Toulouse (UT)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT), Institut Pasteur [Paris] (IP)-Institut National de la Santé et de la Recherche Médicale (INSERM), Université de Reims Champagne-Ardenne (URCA)-Université de Reims Champagne-Ardenne (URCA), Université de Tours-Institut National de la Santé et de la Recherche Médicale (INSERM), Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut Pasteur [Paris], Institut National de la Santé et de la Recherche Médicale (INSERM)-Université de Tours, SFR CAP Santé (Champagne-Ardenne Picardie Santé), and Université de Reims Champagne-Ardenne (URCA)-Université de Picardie Jules Verne (UPJV)-Université de Reims Champagne-Ardenne (URCA)-Université de Picardie Jules Verne (UPJV)-Centre Hospitalier Universitaire de Reims (CHU Reims)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université de Reims Champagne-Ardenne (URCA)
Subjects: 0301 basic medicine, Male, Pathology, Chemokine, Cystic Fibrosis, Physiology, [SDV]Life Sciences [q-bio], Cystic Fibrosis Transmembrane Conductance Regulator, MESH: Cystic Fibrosis/pathology, chemokines, MESH: Rats, Sprague-Dawley, Cystic fibrosis, MESH: Mice, Knockout, Rats, Sprague-Dawley, 0302 clinical medicine, MESH: TRPV Cation Channels/physiology, MESH: Cystic Fibrosis/metabolism, MESH: Cystic Fibrosis Transmembrane Conductance Regulator/metabolism, MESH: Animals, ComputingMilieux_MISCELLANEOUS, Mice, Knockout, biology, 3. Good health, medicine.anatomical_structure, 030220 oncology & carcinogenesis, MESH: Alveolar Epithelial Cells/metabolism, Female, medicine.symptom, Signal transduction, signal transduction, Pulmonary and Respiratory Medicine, TRPV4, medicine.medical_specialty, Mice, 129 Strain, MESH: Cystic Fibrosis/immunology, TRPV Cation Channels, Inflammation, MESH: Calcium Signaling, eicosanoids, 03 medical and health sciences, MESH: Mice, 129 Strain, In vivo, MESH: Mice, Inbred C57BL, Physiology (medical), medicine, Animals, Humans, Calcium Signaling, Lung, MESH: Humans, Calcium channel, lung inflammation, Cell Biology, medicine.disease, MESH: Male, Mice, Inbred C57BL, 030104 developmental biology, A549 Cells, Alveolar Epithelial Cells, Immunology, biology.protein, calcium channel, MESH: A549 Cells, MESH: Female
Abstract: Cystic fibrosis (CF) is an inherited disease associated with chronic severe lung inflammation, leading to premature death. To develop innovative anti-inflammatory treatments, we need to characterize new cellular and molecular components contributing to the mechanisms of lung inflammation. Here, we focused on the potential role of “transient receptor potential vanilloid-4” (TRPV4), a nonselective calcium channel. We used both in vitro and in vivo approaches to demonstrate that TRPV4 expressed in airway epithelial cells triggers the secretion of major proinflammatory mediators such as chemokines and biologically active lipids, as well as a neutrophil recruitment in lung tissues. We characterized the contribution of cytosolic phospholipase A2, MAPKs, and NF-κB in TRPV4-dependent signaling. We also showed that 5,6-, 8,9-, 11,12-, and 14,15-epoxyeicosatrienoic acids, i.e., four natural lipid-based TRPV4 agonists, are present in expectorations of CF patients. Also, TRPV4-induced calcium mobilization and inflammatory responses were enhanced in cystic fibrosis transmembrane conductance regulator-deficient cellular and animal models, suggesting that TRPV4 is a promising target for the development of new anti-inflammatory treatments for diseases such as CF.
Published: 2016

6. CO2 non-LTE limb emissions in Mars' atmosphere as observed by OMEGA/Mars Express

Author: Francesca Altieri, François Forget, Miguel Lopez-Valverde, Brigitte Gondet, Arianna Piccialli, Joachim Audouard, Jean-Pierre Bibring, Pierre Drossart, F. Gonzalez-Galindo, Anni Määttänen, 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), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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)-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 Geosciences [Stony Brook], Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), 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), European Union, Centre National d'Etudes Spatiales (CNES), European Project: 633127,H2020,H2020-COMPET-2014,UPWARDS(2015), European Commission, Université Paris-Sud - Paris 11 (UP11)-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), and 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)
Subjects: 010504 meteorology & atmospheric sciences, non-LTE emissions, Solar zenith angle, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Atmospheric sciences, 01 natural sciences, 7. Clean energy, Omega, Atmosphere, Altitude, Mars atmosphere, Geochemistry and Petrology, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Physics::Atmospheric and Oceanic Physics, 0105 earth and related environmental sciences, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Atmospheric models, Infrared observations, Atmospheric wave, Astrophysics::Instrumentation and Methods for Astrophysics, Mars Exploration Program, Atmosphere of Mars, Remote sensing, Geophysics, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Environmental science, Astrophysics::Earth and Planetary Astrophysics, Planetary atmospheres
Abstract: We report on daytime limb observations of Mars upper atmosphere acquired by the OMEGA instrument on board the European spacecraft Mars Express. The strong emission observed at 4.3m is interpreted as due to CO2 fluorescence of solar radiation and is detected at a tangent altitude in between 60 and 110km. The main value of OMEGA observations is that they provide simultaneously spectral information and good spatial sampling of the CO2 emission. In this study we analyzed 98 dayside limb observations spanning over more than 3 Martian years, with a very good latitudinal and longitudinal coverage. Thanks to the precise altitude sounding capabilities of OMEGA, we extracted vertical profiles of the non-local thermodynamic equilibrium (non-LTE) emission at each wavelength and we studied their dependence on several geophysical parameters, such as the solar illumination and the tangent altitude. The dependence of the non-LTE emission on solar zenith angle and altitude follows a similar behavior to that predicted by the non-LTE model. According to our non-LTE model, the tangent altitude of the peak of the CO2 emission varies with the thermal structure, but the pressure level where the peak of the emission is found remains constant at approximate to 0.03 0.01Pa, . This non-LTE model prediction has been corroborated by comparing SPICAM and OMEGA observations. We have shown that the seasonal variations of the altitude of constant pressure levels in SPICAM stellar occultation retrievals correlate well with the variations of the OMEGA peak emission altitudes, although the exact pressure level cannot be defined with the spectroscopy for the investigation of the characteristics of the atmosphere of Venus (SPICAM) nighttime data. Thus, observed changes in the altitude of the peak emission provide us information on the altitude of the 0.03Pa pressure level. Since the pressure at a given altitude is dictated by the thermal structure below, the tangent altitude of the peak emission represents then an important piece of information of the atmosphere, of great value for validating general circulation models. We thus compared the altitude of OMEGA peak emission with the altitude of the 0.03Pa level predicted by the Laboratoire de meteorologie dynamique (LMD)-Mars global circulation model and found that the peak emission altitudes from OMEGA present a much larger variability than the tangent altitude of the 0.03Pa level predicted by the general circulation model. This variability could be possibly due to unresolved atmospheric waves. Further studies using this strong CO2 limb emission data are proposed., A.P. acknowledges funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement 246556.This work has received funding from the European Union's Horizon 2020 Programme (H2020-Compet-08-2014) under grant agreement UPWARDS-633127.
Published: 2016

7. Unique Spectroscopy and Imaging of Mars with the James Webb Space Telescope

Author: Miguel Lopez-Valverde, Paul Hartogh, Robert E. Novak, Ann Carine Vandaele, Pierre Ferruit, Francesca Altieri, Michael J. Wolff, Geronimo L. Villanueva, R. Todd Clancy, Thérèse Encrenaz, Michael J. Mumma, Thierry Fouchet, Michael D. Smith, Stefanie N. Milam, Emmanuel Lellouch, NASA Goddard Space Flight Center (GSFC), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Space Science Institute [Boulder] (SSI), 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), Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), and Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS)
Subjects: Martian, [PHYS]Physics [physics], 010504 meteorology & atmospheric sciences, James Webb Space Telescope, Astronomy and Astrophysics, Atmosphere of Mars, Spectral bands, Mars Exploration Program, Exploration of Mars, 01 natural sciences, Astrobiology, 13. Climate action, Space and Planetary Science, Martian surface, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Geology, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Infrared photography
Abstract: In this paper, we summarize the main capabilities of the James Webb Space Telescope (JWST) for performing observations of Mars. The distinctive vantage point of JWST at the Sun-Earth Lagrange point (L2) will allow sampling the full observable disk, permitting the study of short-term phenomena, diurnal processes (across the east-west axis), and latitudinal processes between the hemispheres (including seasonal effects) with excellent spatial resolutions (0.''07 at 2 micron). Spectroscopic observations will be achievable in the 0.7-5 micron spectral region with NIRSpec at a maximum resolving power of 2700 and with 8000 in the 1-1.25 micron range. Imaging will be attainable with the Near-Infrared Camera at 4.3 micrometers and with two narrow filters near 2 micron, while the nightside will be accessible with several filters in 0.5 to 2 micron. Such a powerful suite of instruments will be a major asset for the exploration and characterization of Mars. Some science cases include the mapping of the water D/H ratio, investigations of the Martian mesosphere via the characterization of the non-local thermodynamic equilibrium CO2 emission at 4.3 micron, studies of chemical transport via observations of the O2 nightglow at 1.27 micron, high-cadence mapping of the variability dust and water-ice clouds, and sensitive searches for trace species and hydrated features on the Martian surface. In-flight characterization of the instruments may allow for additional science opportunities.
Published: 2016

8. Dayside temperatures in the Venus upper atmosphere from Venus Express/VIRTIS nadir measurements at 4.3 μm

Author: Javier Peralta, Gabriella Gilli, Miguel Lopez-Valverde, Arianna Piccialli, Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 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), 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), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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)-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), Ministerio de Economía y Competitividad (España), European Commission, 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
Subjects: Daytime, 010504 meteorology & atmospheric sciences, Radiation mechanisms: non-thermal, Satellites, Data analysis, Planets, Venus, Instrumentation: spectrographs, Astrophysics, Atmospheric sciences, 01 natural sciences, Molecular processes, Mesosphere, Atmosphere, Planet, Methods: data analysis, Spectrographs, 0103 physical sciences, Nadir, Radiation mechanisms, Planets and satellites: atmospheres, Radiative transfer, spectrographs [Instrumentation], data analysis [Methods], 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, non-thermal [Radiation mechanisms], biology, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy and Astrophysics, Atmospheric temperature, biology.organism_classification, 3. Good health, 13. Climate action, Space and Planetary Science, atmospheres [Planets and satellites], Thermosphere
Abstract: In this work, we analysed nadir observations of atmospheric infrared emissions carried out by VIRTIS, a high-resolution spectrometer on board the European spacecraft Venus Express. We focused on the ro-vibrational band of CO at 4.3 μm on the dayside, whose fluorescence originates in the Venus upper mesosphere and above. This is the first time that a systematic sounding of these non-local thermodynamic equilibrium (NLTE) emissions has been carried out in Venus using this geometry. As many as 143,218 spectra have been analysed on the dayside during the period 14/05/2006 to 14/09/2009. We designed an inversion method to obtain the atmospheric temperature from these non-thermal observations, including a NLTE line-by-line forward model and a pre-computed set of spectra for a set of thermal structures and illumination conditions. Our measurements sound a broad region of the upper mesosphere and lower thermosphere of Venus ranging from 10-10 mb (which in the Venus International Reference Atmosphere, VIRA, is approximately 100-150 km during the daytime) and show a maximum around 195 ± 10 K in the subsolar region, decreasing with latitude and local time towards the terminator. This is in qualitative agreement with predictions by a Venus Thermospheric General Circulation Model (VTGCM) after a proper averaging of altitudes for meaningful comparisons, although our temperatures are colder than the model by about 25 K throughout. We estimate a thermal gradient of about 35 K between the subsolar and antisolar points when comparing our data with nightside temperatures measured at similar altitudes by SPICAV, another instrument on Venus Express (VEx). Our data show a stable temperature structure through five years of measurements, but we also found episodes of strong heating/cooling to occur in the subsolar region of less than two days., J.P. and MA.L-V acknowledge the Spanish MICINN for funding support through the CONSOLIDER program >ASTROMOL> CSD2009-00038 and project AYA2011-23552. J.P. also thanks the JAXA International Top Young Fellowship program, GG thanks CNES postdoc contract and A.P. acknowledges funding from the European Union Seventh Framework Programme (FP7/2007-2013) under Grant agreement No. 246556.
Published: 2016

9. Carbon monoxide and temperature in the upper atmosphere of Venus from VIRTIS/Venus Express non-LTE limb measurements

Author: Amanda Brecht, Pierre Drossart, Gabriella Gilli, Javier Peralta, Miguel Lopez-Valverde, Giuseppe Piccioni, Stephen W. Bougher, Observatório Astronómico de Lisboa, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, 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), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), and Istituto Nazionale di Astrofisica (INAF)
Subjects: [PHYS]Physics [physics], 010504 meteorology & atmospheric sciences, biology, Equator, Astronomy and Astrophysics, Venus, Noon, biology.organism_classification, Atmospheric sciences, 01 natural sciences, Mesosphere, Atmosphere of Venus, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Radiative transfer, Terrestrial planet, Environmental science, Thermosphere, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract: The upper mesosphere and the lower thermosphere of Venus (from 90 to 150 km altitude) seems to play a transition region in photochemistry, dynamics and radiation, but is still very poorly constrained observationally. Since 2006 VIRTIS on board Venus Express has been obtaining limb observations of CO fluorescent infrared emissions in a systematic manner. This study represents the scientific exploitation of this dataset and reports new information on the composition and temperature at those altitudes. This work is focused on the 4.7 μ m emission of CO as observed by VIRTIS, which contains two emission bands, the fundamental and the first hot of the main CO isotope. A specific scheme for a simultaneous retrieval of CO and temperature is proposed, based on results of a comprehensive non-LTE model of these molecular emissions. A forward model containing such non-LTE model is used at the core of an inversion scheme that consists of two steps: (i) a minimization procedure of model-data differences and (ii) a linear inversion around the solution of the first step. A thorough error analysis is presented, which shows that the retrievals of CO and temperature are very noisy but can be improved by suitable averaging of data. These averages need to be consistent with the non-LTE nature of the emissions. Unfortunately, the data binning process reduced the geographical coverage of the results. The obtained retrieval results indicate a global distribution of the CO in the Venus dayside with a maximum around the sub-solar point, and a decrease of a factor 2 towards high latitudes. Also a gradient from noon to the morning and evening sides is evident in the equator, this being smaller at high latitudes. No morning–afternoon differences in the CO concentration are observed, or are comparable to our retrieval errors. All this argues for a CO distribution controlled by dynamics in the lower thermosphere, with a dominant sub-solar to anti-solar gradient. Similar variations are found with the Venus Thermospheric General Circulation Model (VTGCM), but the VIRTIS CO is systematically larger than in the model. The thermal structure obtained by VIRTIS presents a hint of local maximum around 115 km near the terminator at equatorial latitudes, but not at noon, in clear contrast to VTGCM predictions and to an upper mesosphere in pure radiative balance. A few tentative ideas to explain these model-data discrepancies are discussed.
Published: 2015

10. Variability of the hydrogen in the martian upper atmosphere as simulated by a 3D atmosphere–exosphere coupling

Author: Francisco Gonzalez-Galindo, François Leblanc, Miguel Lopez-Valverde, François Forget, Ronan Modolo, Jean-Yves Chaufray, Sebastien Hess, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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)-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), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 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), 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
Subjects: [PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], 010504 meteorology & atmospheric sciences, Hydrogen, Atmosphere, Northern Hemisphere, chemistry.chemical_element, Mars, Astronomy and Astrophysics, Atmospheric sciences, 01 natural sciences, Corona, Solar cycle, chemistry, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Environmental science, Solstice, Thermosphere, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Exosphere
Abstract: International audience; We present the temporal variability of the atomic and molecular hydrogen density derived from a 3D General Circulation Model describing the Martian atmosphere from the surface to the exobase. A kinetic exospheric model is used to compute the hydrogen density above the exobase. We use these models to study the diurnal and seasonal variations of the hydrogen density and the Jeans escape rate as well as their variations with solar activity, assuming a classic dust scenario. We find that the diurnal variations of the hydrogen density are important with a peak in the dawn region during equinoxes and a peak on the nightside during solstices. These features result from the dynamics of the Martian upper atmosphere. The variations of the atomic hydrogen Jeans escape with seasons and solar activity are in the range 1.3x1025 s-1 – 4.4x1026 s-1. A factor ∼8 is due to the seasonal variations with a maximum during the winter solstice in the northern hemisphere and a minimum during the summer solstice in the northern hemisphere that we attribute to the variation of the Mars-Sun distance. A factor ∼5 is due to the solar cycle with a maximum escape rate at high solar activity. The variations of the molecular hydrogen Jeans escape with seasons and solar activity are in the range 3x1022 s-1 – 6x1024 s-1. A factor ∼10 is due to the seasonal variations with a maximum during the winter solstice in the northern hemisphere and a minimum during the summer solstice in the northern hemisphere. A factor ∼20 is due to the solar cycle with a maximum escape rate at high solar activity. If Jeans escape is the major escape channel for hydrogen, the hydrogen escape is never limited by diffusion. The hydrogen density above 10,000 km presents seasonal and solar cycle variations similar to the Jeans escape rate at all latitudes and local times. This 3D temporal model of the hydrogen thermosphere/exosphere will be useful to interpret future MAVEN observations and the consequences of the hydrogen corona variability on the Martian plasma environment.
Published: 2015

11. Three-dimensional Martian ionosphere model: II. Effect of transport processes due to pressure gradients

Author: François Forget, Jean-Yves Chaufray, Miguel Lopez-Valverde, Ronan Modolo, Olivier Witasse, Pierre-Louis Blelly, F. Gonzalez-Galindo, Sebastien Hess, Manabu Yagi, François Leblanc, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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)-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 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), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 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), Planetary Plasma and Atmospheric Research Center [Sendai] (PPARC), Tohoku University [Sendai], Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and European Space Agency (ESA)
Subjects: Martian, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Mars, Mars Exploration Program, Atmospheric sciences, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Solar cycle, Physics::Geophysics, Dynamics, Atmosphere, Solar wind, Geophysics, Flow velocity, 13. Climate action, Space and Planetary Science, Geochemistry and Petrology, Physics::Space Physics, Earth and Planetary Sciences (miscellaneous), Environmental science, Astrophysics::Earth and Planetary Astrophysics, Ionosphere, Pressure gradient, Physics::Atmospheric and Oceanic Physics
Abstract: International audience; To study the transport of the ionospheric plasma on Mars, we have included a 3D multifluid dynamical core in a Martian General Circulation Model (GCM). Vertical transport modifies the ion density above ~160 km on the dayside, especially the ions produced at high altitudes like O+, N+ and C+. Near the exobase, the dayside to nightside flow velocity reaches few hundreds of m/s, due to a large horizontal pressure gradient. Comparison with MEX/ASPERA-3 measurements between 290 - 500 km, suggests this flow could account for at least 20% of the flow produced by the solar wind. This flow is not sufficient to populate substantially the nightside ionosphere at high altitudes, in agreement with recent observations, because of a strong nightside downward flow produced by vertical pressure gradient. The O2+ and NO+ ion densities on the nightside at low altitudes (~130 km) are modified by this downward flow, compared to simulated densities without ion dynamics, while other ions are lost by chemical reactions. Variability at different time scales (diurnal, seasonal and solar cycle) are studied. We simulate diurnal and seasonal variations of the ionospheric composition due to the variability of the neutral atmosphere and solar flux at the top of the atmosphere. The ionospheric dynamics are not strongly affected by seasons and solar cycles and the retroaction of the ionosphere on the neutral atmosphere temperature and velocity is negligible compared to other physical processes below the exobase.
Published: 2014

12. Io’s contracting atmosphere post 2011 perihelion: Further evidence for partial sublimation support on the anti-Jupiter hemisphere

Author: Henry G. Roe, Thomas K. Greathouse, John R. Spencer, Constantine Tsang, Emmanuel Lellouch, Matthew J. Richter, Miguel Lopez-Valverde, 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), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), University of California [Davis] (UC Davis), University of California, Southwest Research Institute [San Antonio] (SwRI), and University of California (UC)
Subjects: Physics, ICARUS, [PHYS]Physics [physics], 010504 meteorology & atmospheric sciences, Astronomy, Astronomy and Astrophysics, Scale height, 01 natural sciences, Jovian, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Sublimation (phase transition), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract: New 19 μm spectroscopy of Io’s SO 2 atmosphere in 2012 and 2013, when combined with our earlier observations starting in 2001, provides a near-yearly record of atmospheric density in the lowest scale height, spanning almost an entire jovian year. We find that the anti-Jupiter hemisphere atmospheric density is decreasing following Jupiter’s 2011 perihelion passage, confirming our model (Tsang, C.C.C., Spencer, J.R., Lellouch, E., Lopez-Valverde, M.A., Richter, M.J., Greathouse, T.K., [2012]. Icarus 217, 277–296) that the anti-jovian atmosphere has a large sublimation-supported component that peaks near perihelion.
Published: 2013

13. Thermal and wind structure of the Martian thermosphere as given by two General Circulation Models

Author: François Forget, James R. Murphy, Miguel Lopez-Valverde, Stephen W. Bougher, Francisco Gonzalez-Galindo, 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
Subjects: Martian, Astronomy and Astrophysics, Mars Exploration Program, Atmosphere of Mars, Atmospheric sciences, Mesosphere, Atmosphere, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Physics::Space Physics, Thermal, Astrophysics::Solar and Stellar Astrophysics, Environmental science, Solstice, Astrophysics::Earth and Planetary Astrophysics, Thermosphere, Physics::Atmospheric and Oceanic Physics
Abstract: International audience; We have used two different General Circulation Models to study the thermal and wind structure of the Martian upper atmosphere (mesosphere and thermosphere). Both models take into account the effects of waves propagating from the lower atmosphere, although they use different methods for this purpose. We present the results of three simulations that allow us to take into account the seasonal variability of the Martian atmosphere. Simplified dust scenarios and a common set of input parameters are used. The temperatures and winds predicted by both models show an overall good agreement. However, some differences have been identified, generally of a local nature. The magnitude of these differences tends to increase with the amount of dust in the lower atmosphere. The different heating terms of the upper atmosphere predicted by both models are in good agreement, which suggests that the differences between the models have their origin in the propagation of waves from the lower atmosphere. This study has allowed us to confirm the important role of the redistribution of the energy by the winds in producing the longitude-latitude structure of the temperatures. Both models predict also a thermospheric polar warming during the Southern summer solstice, although its intensity seems to be model-dependent and connected to lower atmosphere dust loading.
Published: 2010

14. Mars Environment and Magnetic Orbiter Scientific and Measurement Objectives

Author: Miguel Lopez-Valverde, François Leblanc, Benoit Langlais, Michel Menvielle, A. Pais, Stephen R. Lewis, Andrew J. Coates, T. Fouchet, Helmut Lammer, François Forget, Eric Chassefière, Martin Paetzold, Doris Breuer, Pascal Tarits, Peter L. Read, Susanne Vennerstrøm, Christophe Sotin, Véronique Dehant, S. Barabash, Mioara Mandea, PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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)-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 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 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), Swedish Institute of Space Physics [Uppsala] (IRF), Deutsches Zentrum für Luft- und Raumfahrt (DLR), Department of Space and Climate Physics [UCL London], Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL)-University College of London [London] (UCL), Royal Observatory of Belgium [Brussels] (ROB), 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), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Department of Physics and Astronomy [Milton Keynes], The Open University [Milton Keynes] (OU), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), HELIOS - LATMOS, Department of Physics [Coimbra], University of Coimbra [Portugal] (UC), Universität zu Köln, Université de Brest (UBO), National Space Institute [Lyngby] (DTU Space), Technical University of Denmark [Lyngby] (DTU), 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), Universität zu Köln = University of Cologne, Danmarks Tekniske Universitet = Technical University of Denmark (DTU), and 2.3 Earth's Magnetic Field, 2.0 Physics of the Earth, Departments, GFZ Publication Database, Deutsches GeoForschungsZentrum
Subjects: Time Factors, Cosmic Vision, Extraterrestrial Environment, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mars, 550 - Earth sciences, 01 natural sciences, Astrobiology, law.invention, Atmosphere, Magnetics, Orbiter, law, Planet, Exobiology, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Computer Simulation, 010303 astronomy & astrophysics, Physics::Atmospheric and Oceanic Physics, 0105 earth and related environmental sciences, Martian, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Altitude, Astrophysics::Instrumentation and Methods for Astrophysics, Mars Exploration Program, Space Flight, Satellite Communications, Agricultural and Biological Sciences (miscellaneous), Solar wind, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Environmental science, Planetary Evolution, Astrophysics::Earth and Planetary Astrophysics, Evolution, Planetary
Abstract: International audience; In this paper, we summarize our present understanding of Mars' atmosphere, magnetic field, and surface and address past evolution of these features. Key scientific questions concerning Mars' surface, atmosphere, and magnetic field, along with the planet's interaction with solar wind, are discussed. We also define what key parameters and measurements should be performed and the main characteristics of a martian mission that would help to provide answers to these questions.Such a mission—Mars Environment and Magnetic Orbiter (MEMO)—was proposed as an answer to the Cosmic Vision Call of Opportunity as an M-class mission (corresponding to a total European Space Agency cost of less than 300 M€). MEMO was designed to study the strong interconnection between the planetary interior, atmosphere, and solar conditions, which is essential to our understanding of planetary evolution, the appearance of life, and its sustainability.The MEMO main platform combined remote sensing and in situ measurements of the atmosphere and the magnetic field during regular incursions into the martian upper atmosphere. The micro-satellite was designed to perform simultaneous in situ solar wind measurements. MEMO was defined to conduct:• Four-dimensional mapping of the martian atmosphere from the surface up to 120 km by measuring wind, temperature, water, and composition, all of which would provide a complete view of the martian climate and photochemical system;• Mapping of the low-altitude magnetic field with unprecedented geographical, altitude, local time, and seasonal resolutions;• A characterization of the simultaneous responses of the atmosphere, magnetic field, and near-Mars space to solar variability by means of in situ atmospheric and solar wind measurements.
Published: 2009

15. Gravity waves in the upper atmosphere of Venus revealed by CO2 nonlocal thermodynamic equilibrium emissions

Author: Raphaël F. Garcia, Giovanni Occhipinti, Miguel Lopez-Valverde, Pierre Drossart, Giuseppe Piccioni, Services communs OMP (UMS 831), 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), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique du Globe de Paris (IPGP), and 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)
Subjects: Atmospheric Science, Soil Science, Venus, Aquatic Science, Oceanography, Atmosphere of Venus, Geochemistry and Petrology, Polar vortex, Dispersion relation, Earth and Planetary Sciences (miscellaneous), Gravity wave, Physics::Atmospheric and Oceanic Physics, Earth-Surface Processes, Water Science and Technology, Physics, Ecology, biology, Paleontology, Forestry, biology.organism_classification, Geodesy, Wavelength, Geophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Phase velocity, Thermosphere
Abstract: International audience; The imaging capabilities of the Visible and Infrared Thermal Imaging Spectrometer-Mapper (VIRTIS-M) onboard Venus Express mission are used to analyze perturbations of CO2 nonlocal thermodynamic equilibrium emissions in the thermosphere of Venus. These emissions with a wavelength of 4.3 μm originate from the 110-140 km altitude range and are sensitive to density perturbations. They show wave-like perturbations of about 0.5% root-mean-square amplitude of the background signal with horizontal wavelengths in the 90-400 km range. The horizontal phase velocities are similar in magnitude and direction from one orbit to the next, with averages of 70 m/s westward and 30 m/s northward. The geographical wave distribution and the orientation of wavefronts demonstrate that the polar vortex at work in the cloud layer is the source of these gravity waves. The large westward zonal phase velocity in the 0900-1500 local time range argues in favor of the superrotation dynamics within 30° from the south pole to an altitude of at least 115 km. The gravity wave dispersion relation and the geographical distribution of wavefront amplitudes suggest the presence of a solar to antisolar wind close to the south pole. Because the centroid altitude and the sensitivity of these emissions to gravity wave perturbations are only roughly estimated, it is not possible to make a quantitative estimate of the upward energy transfer. However, this study demonstrates the strong influence of the polar vortex on the circulation in the atmosphere of Venus up to the thermosphere.
Published: 2009

16. Mars environment and magnetic orbiter model payload

Author: J.E. Walhund, A. Pais, Pascal Tarits, S. Barabash, François Leblanc, T. Ott, Mioara Mandea, Stephen R. Lewis, Benoit Langlais, Helmut Lammer, Jean-Gabriel Trotignon, Eric Chassefière, J.G.M. Merayo, Martin Paetzold, Peter L. Read, Henri Rème, Gabriele Cremonese, François Forget, Andrew J. Coates, Susanne Vennerstrøm, Christophe Sotin, Michel Menvielle, Véronique Dehant, Miguel Lopez-Valverde, Doris Breuer, T. Fouchet, Graziella Branduardi-Raymont, 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), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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)-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 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), Swedish Institute of Space Physics [Uppsala] (IRF), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), 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), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Royal Observatory of Belgium [Brussels] (ROB), 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), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Department of Physics and Astronomy [Milton Keynes], The Open University [Milton Keynes] (OU), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), GeoForschungsZentrum - Helmholtz-Zentrum Potsdam (GFZ), HELIOS - LATMOS, Department of Physics [Coimbra], University of Coimbra [Portugal] (UC), Universität zu Köln, Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford [Oxford], Institut Universitaire Européen de la Mer (IUEM), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS), National Space Institute [Lyngby] (DTU Space), Technical University of Denmark [Lyngby] (DTU), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Swedish Space Corporation (SSC), 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, Laboratoire de physique et chimie de l'environnement (LPCE), Université d'Orléans (UO)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géodynamique de Nantes ( LPGN ), Université de Nantes ( UN ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), 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 ) -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 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 Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Swedish Institute of Space Physics [Uppsala] ( IRF ), Deutsches Zentrum für Luft- und Raumfahrt [Berlin] ( DLR ), 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 ), Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), Royal Observatory of Belgium [Brussels], 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 Paris ) -École normale supérieure - Paris ( ENS Paris ), Space Research Institute of Austrian Academy of Sciences ( IWF ), Austrian Academy of Sciences ( OeAW ), The Open University [Milton Keynes] ( OU ), Instituto de Astrofísica de Andalucía ( IAA ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), GeoForschungsZentrum - Helmholtz-Zentrum Potsdam ( GFZ ), HEPPI - LATMOS, University of Coimbra [Portugal] ( UC ), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] ( AOPP ), Institut Universitaire Européen de la Mer ( IUEM ), Institut de Recherche pour le Développement ( IRD ) -Université de Brest ( UBO ) -Centre National de la Recherche Scientifique ( CNRS ), National Space Institute [Lyngby] ( DTU Space ), Technical University of Denmark [Lyngby] ( DTU ), INAF - Osservatorio Astronomico di Padova ( OAPD ), Istituto Nazionale di Astrofisica ( INAF ), Swedish Space Corporation ( SSC ), Centre d'étude spatiale des rayonnements ( CESR ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), 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 ), 2.3 Earth's Magnetic Field, 2.0 Physics of the Earth, Departments, GFZ Publication Database, Deutsches GeoForschungsZentrum, 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), Universität zu Köln = University of Cologne, University of Oxford, Danmarks Tekniske Universitet = Technical University of Denmark (DTU), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Solar System, Cosmic Vision, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], planetary interior, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], 550 - Earth sciences, 01 natural sciences, 7. Clean energy, law.invention, Atmosphere, Orbiter, law, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing, Orbital elements, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Space vehicles, Mars Exploration Program, M-class mission, planetary evolution, solar conditions, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Solar wind, [ PHYS.ASTR.EP ] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], 13. Climate action, Space and Planetary Science, MEMO, Magnetic fields, atmosphere, Physics::Space Physics, Solar-terrestrial relations, Mars Environment and Magnetic Orbiter, Timekeeping on Mars, Astrophysics::Earth and Planetary Astrophysics, Planets and satellites, Solar system
Abstract: International audience; Mars Environment and Magnetic Orbiter was proposed as an answer to the Cosmic Vision Call of Opportunity as a M-class mission. The MEMO mission is designed to study the strong interconnections between the planetary interior, atmosphere and solar conditions essential to understand planetary evolution, the appearance of life and its sustainability. MEMO provides a high-resolution, complete, mapping of the magnetic field (below an altitude of about 250 km), with an yet unachieved full global coverage. This is combined with an in situ characterization of the high atmosphere and remote sensing of the middle and lower atmospheres, with an unmatched accuracy. These measurements are completed by an improved detection of the gravity field signatures associated with carbon dioxide cycle and to the tidal deformation. In addition the solar wind, solar EUV/UV and energetic particle fluxes are simultaneously and continuously monitored. The challenging scientific objectives of the MEMO mission proposal are fulfilled with the appropriate scientific instruments and orbit strategy. MEMO is composed of a main platform, placed on a elliptical (130 × 1,000 km), non polar (77° inclination) orbit, and of an independent, higher apoapsis (10,000 km) and low periapsis (300 km) micro-satellite. These orbital parameters are designed so that the scientific return of MEMO is maximized, in terms of measurement altitude, local time, season and geographical coverage. MEMO carry several suites of instruments, made of an ‘exospheric-upper atmosphere’ package, a ‘magnetic field’ package, and a ‘low-middle atmosphere’ package. Nominal mission duration is one Martian year.
Published: 2009

17. Density and temperatures of the upper martian atmosphere measured by stellar occultations with Mars Express SPICAM

Author: Aurélie Reberac, Franck Montmessin, Emmanuel Dimarellis, Eric Quémerais, François Forget, Francisco Gonzalez-Galindo, Jean-Loup Bertaux, Miguel Lopez-Valverde, Sébastien Lebonnois, 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), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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)-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), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 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), and 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)
Subjects: Atmospheric Science, 010504 meteorology & atmospheric sciences, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Soil Science, Density, Mars, Aquatic Science, Noon, Oceanography, Atmospheric sciences, 01 natural sciences, Latitude, Atmosphere, Geochemistry and Petrology, Diurnal cycle, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Earth-Surface Processes, Water Science and Technology, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Ecology, Temperature, Paleontology, Forestry, Scale height, Mars Exploration Program, Atmosphere of Mars, Stellar occultation, Geophysics, 13. Climate action, Space and Planetary Science, Mesopause, Environmental science
Abstract: International audience; We present one Martian year of observations of the density and temperature in the upper atmosphere of Mars (between 60 and 130 km) obtained by the Mars Express ultraviolet spectrometer Spectroscopy for Investigation of Characteristics of the Atmosphere of Mars (SPICAM). Six hundred sixteen profiles were retrieved using stellar occultations technique at various latitude and longitude. The atmospheric densities exhibit large seasonal fluctuations due to variations in the dust content of the lower atmosphere which controls the temperature and, thus, the atmospheric scale height, below 50 km. In particular, the year observed by SPICAM was affected by an unexpected dust loading around Ls = 130° which induced a sudden increase of density above 60 km. The diurnal cycle could not be analyzed in detail because most data were obtained at nighttime, except for a few occultations observed around noon during northern winter. There, the averaged midday profile is found to slightly differ from the corresponding midnight profile, with the observed differences being consistent with propagating thermal tides and variations in local solar heating. About 6% of the observed mesopause temperatures exhibits temperature below the CO2 frost point, especially during northern summer in the tropics. Comparison with atmospheric general circulation model predictions shows that the existing models overestimate the temperature around the mesopause (above 80 to 100 km) by up to 30 K, probably because of an underestimation of the atomic oxygen concentration which controls the CO2 infrared cooling.
Published: 2009

18. Limb observations of CO2 and CO non-LTE emissions in the Venus atmosphere by VIRTIS/Venus Express

Author: A. Cardesín Moinelo, Miguel Lopez-Valverde, Giuseppe Piccioni, P. Drossart, S. Erard, Gabriella Gilli, Instituto de Astrofisica de Andalucia, CSIC (IAA), Observatoire de Paris, Université Paris sciences et lettres (PSL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), and Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Roma)
Subjects: Atmospheric Science, Daytime, Infrared, Solar zenith angle, Soil Science, Venus, Aquatic Science, Oceanography, Atmospheric sciences, Mesosphere, Atmosphere, Atmosphere of Venus, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Earth-Surface Processes, Water Science and Technology, Ecology, biology, Paleontology, Astronomy, Forestry, biology.organism_classification, Geophysics, Space and Planetary Science, Environmental science, Thermosphere, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; We report and analyze here observations of strong infrared emissions from the limb of the Venus upper atmosphere during daytime, taken by the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) aboard Venus Express. We focus on the measurements taken during the first 4 months of nominal operations. The emissions observed at 4.3 mum and at 2.7 mum are attributed to CO2 fluorescence of solar radiation and are detected up to about 160 km and 130 km, respectively, while the CO fluorescence at 4.7 mum is observed up to about 120 km. The emissions are detected in both the channels of VIRTIS, at different spatial and spectral resolutions (resolving powers about 1800 and 400), for the periapsis and the apoapsis of the Venus Express orbit. From these data sets we built up 2-D maps of the emissions as well as vertical profiles, which are then studied in order to characterize their variations with geophysical parameters, like solar illumination and emission altitude. Several analyses are performed in order to understand the VIRTIS behavior, to determine systematic effects in the data, and to propose appropriate corrections. We also present comparisons with a theoretical nonlocal thermodynamic equilibrium (non-LTE) model of the Venus upper atmosphere. The agreement is very encouraging, in general, and the main variability observed in the data, with solar zenith angle and altitude, can be understood with the model. We conclude that the present data set opens brilliant perspectives for deriving densities and rotational temperatures in the upper mesosphere and lower thermosphere of Venus.
Published: 2009

19. Murine embryonic stem cell-derived pancreatic acinar cells recapitulate features of early pancreatic differentiation

Author: Mohammad Massumi, Selma A. Serra, Josep Lloreta, Fabien Delaspre, Miguel A. Valverde, Bruno Payré, Francisco X. Real, Stephen F. Konieczny, Pierre Savatier, Marlène Dufresne, Meritxell Rovira, Anouchka Skoudy, Cancer Research Program, Institut Municipal d' Investigacio Mèdica, Laboratory of Molecular Physiology and Channelopathies, Barcelona, Laboratory of Molecular Physiology and Channelopathies, Department de Patologia, Hospital del Mar, Universitat Pompeu Fabra [Barcelona] (UPF), Institut de médecine moléculaire de Rangueil (I2MR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-IFR150-Institut National de la Santé et de la Recherche Médicale (INSERM), Centre de Microscopie Électronique Appliquée à la Biologie (CMEAB), Hôpital de Rangueil, CHU Toulouse [Toulouse]-CHU Toulouse [Toulouse]-Toulouse Réseau Imagerie-Genotoul ( TRI-Genotoul), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Department of Biological Sciences [West Lafayette], Purdue University [West Lafayette], Institut cellule souche et cerveau (U846 Inserm - UCBL1), Institut National de la Recherche Agronomique (INRA)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de la Santé et de la Recherche Médicale (INSERM), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées- Institut Fédératif de Recherche Bio-médicale Institution (IFR150)-Institut National de la Santé et de la Recherche Médicale (INSERM), Toulouse Réseau Imagerie-Genotoul ( TRI-Genotoul), and Simon, Marie Francoise
Subjects: MESH: Cell Differentiation, MESH: Pancreatic Elastase, Cellular differentiation, [SDV]Life Sciences [q-bio], Embryoid body, Biology, MESH: Calcium Signaling, 03 medical and health sciences, 0302 clinical medicine, Directed differentiation, MESH: Microscopy, Immunoelectron, Pancreatic cancer, MESH: Basic Helix-Loop-Helix Transcription Factors, MESH: Gene Expression Regulation, Developmental, medicine, MESH: Amylases, MESH: Animals, MESH: Pancreas, Exocrine, MESH: Embryonic Stem Cells, Pancreatic elastase, MESH: Mice, 030304 developmental biology, 0303 health sciences, MESH: Cell Culture Techniques, MESH: Exocytosis, Hepatology, MESH: Transfection, MESH: Gene Expression Regulation, Enzymologic, MESH: Genes, Reporter, Gastroenterology, MESH: Transcription Factors, medicine.disease, Embryonic stem cell, Molecular biology, MESH: Carboxypeptidases A, [SDV] Life Sciences [q-bio], MESH: Carbachol, medicine.anatomical_structure, MESH: Chymotrypsinogen, Cell culture, 030220 oncology & carcinogenesis, MESH: Cholinergic Agonists, MESH: Cell Division, Pancreas, MESH: Cells, Cultured
Abstract: International audience; BACKGROUND & AIMS: Acinar cells constitute 90% of the pancreas epithelium, are polarized, and secrete digestive enzymes. These cells play a crucial role in pancreatitis and pancreatic cancer. However, there are limited models to study normal acinar cell differentiation in vitro. The aim of this work was to generate and characterize purified populations of pancreatic acinar cells from embryonic stem (ES) cells. METHODS: Reporter ES cells (Ela-pur) were generated that stably expressed both beta-galactosidase and puromycin resistance genes under the control of the elastase I promoter. Directed differentiation was achieved by incubation with conditioned media of cultured fetal pancreatic rudiments and adenoviral-mediated co-expression of p48/Ptf1a and Mist1, 2 basic helix-loop-helix transcription factors crucial for normal pancreatic acinar development and differentiation. RESULTS: Selected cells expressed multiple markers of acinar cells, including digestive enzymes and proteins of the secretory pathway, indicating activation of a coordinated differentiation program. The genes coding for digestive enzymes were not regulated as a single module, thus recapitulating what occurs during in vivo pancreatic development. The generated cells displayed transient agonist-induced Ca(2+) mobilization and showed a typical response to physiologic concentrations of secretagogues, including enzyme synthesis and secretion. Importantly, these effects did not imply the acquisition of a mixed acinar-ductal phenotype. CONCLUSIONS: These studies allow the generation of almost pure acinar-like cells from ES cells, providing a normal cell-based model for the study of the acinar differentiation program in vitro.
Published: 2008

20. Non-LTE infrared observations at Venus: From NIMS/Galileo to VIRTIS/Venus Express

Author: R. W. Carlson, M. Roos-Serote, Miguel Lopez-Valverde, Pierre Drossart, R. Mehlman, Instituto de Astrofisica de Andalucia, CSIC (IAA), 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), Jet Propulsion Laboratory, California Institute of Technology (JPL), Institute of Geophysics, University of California, and Observatorio Astronomico de Lisboa, Centro de Astronomia e Astrofisica da Universidade de Lisboa (CAAUL)
Subjects: Physics, Martian, Spectrometer, biology, Infrared, Planetary Fourier Spectrometer, Imaging spectrometer, Astronomy and Astrophysics, Venus, biology.organism_classification, Atmosphere of Venus, Space and Planetary Science, Nadir, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Remote sensing
Abstract: International audience; Recent improvements in a comprehensive non-local thermodynamic equilibrium (non-LTE) model of CO 2 atmospheres has permitted a better understanding of a number of Venusian atmospheric measurements taken more than a decade ago by the "Near Infrared Mapping Spectrometer" (NIMS) on board the Galileo spacecraft during its Venus fly-by. Those data, containing a strong non-LTE component, showed a structure in the 4.3-mum spectral region which was challenging for non-LTE models so far. The model used in this work was refined after analysis of Martian CO 2 atmospheric emission taken by the "Planetary Fourier Spectrometer" (PFS) and the "Visible and Infrared Mineralogical Mapping Spectrometer" (OMEGA) instruments on board Mars Express. Here we show that both the limb and the nadir measurements of the Venus daylight atmosphere taken at 4.3-mum by NIMS can be fitted reasonably well with the revised model. This gives confidence in the usage of such model for the analysis of the Venus Express mission, in particular for the "Visible Infrared Thermal Imaging Spectrometer" (VIRTIS) instrument which will systematically observe these emissions. We present here non-LTE simulations for VIRTIS which demonstrate its capabilities and potential for detecting atmospheric emissions of CO and CO 2 under non-LTE, both in limb and nadir observations and we discuss briefly the perspectives to use them in order to improve our understanding of the physics of the upper atmosphere of Venus.
Published: 2007

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20 results on '"Miguel A. Valverde"'

1. Annual Appearance of Hydrogen Chloride on Mars and a Striking Similarity With the Water Vapor Vertical Distribution Observed by TGO/NOMAD

2. On the derivation of thermospheric temperatures from dayglow emissions on Mars

3. Thermal structure of the upper atmosphere of Venus simulated by a ground-to-thermosphere GCM

4. MAVEN and the total electron content of the Martian ionosphere

5. In vitro and in vivo evidence for an inflammatory role of the calcium channel TRPV4 in lung epithelium: Potential involvement in cystic fibrosis

6. CO2 non-LTE limb emissions in Mars' atmosphere as observed by OMEGA/Mars Express

7. Unique Spectroscopy and Imaging of Mars with the James Webb Space Telescope

8. Dayside temperatures in the Venus upper atmosphere from Venus Express/VIRTIS nadir measurements at 4.3 μm

9. Carbon monoxide and temperature in the upper atmosphere of Venus from VIRTIS/Venus Express non-LTE limb measurements

10. Variability of the hydrogen in the martian upper atmosphere as simulated by a 3D atmosphere–exosphere coupling

11. Three-dimensional Martian ionosphere model: II. Effect of transport processes due to pressure gradients

12. Io’s contracting atmosphere post 2011 perihelion: Further evidence for partial sublimation support on the anti-Jupiter hemisphere

13. Thermal and wind structure of the Martian thermosphere as given by two General Circulation Models

14. Mars Environment and Magnetic Orbiter Scientific and Measurement Objectives

15. Gravity waves in the upper atmosphere of Venus revealed by CO2 nonlocal thermodynamic equilibrium emissions

16. Mars environment and magnetic orbiter model payload

17. Density and temperatures of the upper martian atmosphere measured by stellar occultations with Mars Express SPICAM

18. Limb observations of CO2 and CO non-LTE emissions in the Venus atmosphere by VIRTIS/Venus Express

19. Murine embryonic stem cell-derived pancreatic acinar cells recapitulate features of early pancreatic differentiation

20. Non-LTE infrared observations at Venus: From NIMS/Galileo to VIRTIS/Venus Express

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20 results on '"Miguel A. Valverde"'

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