156 results on '"López-Valverde, M. A."'
Search Results
152. The latest (version 4.3) Mars Climate Database
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Millour, E., Forget, F., González-Galindo, F., Spiga, A., Lebonnois, S., Montabone, L., Lewis, S. R., Read, P. L., López-Valverde, M. A., Gilli, G., Lefèvre, F., Montmessin, F., Desjean, M.-C., Huot, J.-P., Millour, E., Forget, F., González-Galindo, F., Spiga, A., Lebonnois, S., Montabone, L., Lewis, S. R., Read, P. L., López-Valverde, M. A., Gilli, G., Lefèvre, F., Montmessin, F., Desjean, M.-C., and Huot, J.-P.
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Introduction: The Mars Climate Database (MCD) is a database of meteorological fields derived from General Circulation Model (GCM) numerical simulations of the Martian atmosphere and validated using available observational data. The MCD includes complementary post-processing schemes such as high spatial resolution interpolation of environmental data and means of reconstructing the variability thereof. The GCM is developed at Laboratoire de Météorologie Dynamique du CNRS (Paris, France) [1,2] in collaboration with the Open University (UK), the Oxford University (UK) and the Instituto de Astrofisica de Andalucia (Spain) with support from the European Space Agency (ESA) and the Centre National d'Etudes Spatiales (CNES).
153. Water vapor vertical distribution on Mars during perihelion season of MY 34 and MY 35 with ExoMars‐TGO/NOMAD observations
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Brines, A., López‐Valverde, M. A., Stolzenbach, A., Modak, A., Funke, B., Galindo, F. G., Aoki, S., Villanueva, G. L., Liuzzi, G., Thomas, I. R., Erwin, J. T., Grabowski, U., Forget, F., Lopez‐Moreno, J. J., Rodriguez‐Gomez, J., Daerden, F., Trompet, L., Ristic, B., Patel, M. R., Bellucci, G., Vandaele, A. C., Brines, A., López‐Valverde, M. A., Stolzenbach, A., Modak, A., Funke, B., Galindo, F. G., Aoki, S., Villanueva, G. L., Liuzzi, G., Thomas, I. R., Erwin, J. T., Grabowski, U., Forget, F., Lopez‐Moreno, J. J., Rodriguez‐Gomez, J., Daerden, F., Trompet, L., Ristic, B., Patel, M. R., Bellucci, G., and Vandaele, A. C.
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The water vapor in the Martian atmosphere plays a significant role in the planet’s climate, being crucial in most of the chemical and radiative transfer processes. Despite its importance, the vertical distribution of H2O in the atmosphere has not still been characterized precisely enough. The recent ExoMars Trace Gas Orbiter (TGO) mission, with its Nadir and Occultation for MArs Discovery (NOMAD) instrument, has allowed us to measure the H2O vertical distribution with unprecedented resolution. Recent studies of vertical profiles have shown that high dust concentration in the atmosphere, in particular during dust storms, induces an efficient transport of the H2O to higher altitudes, from 40 km up to 80 km. We study the H2O vertical distribution in a subset of solar occultations during the perihelion of two Martian years (MYs), including the 2018 Global Dust Storm (GDS), in order to compare the same Martian season under GDS and non-GDS conditions. We present our state-of-the-art retrieval scheme, and we apply it to a combination of two diffraction orders, which permits sounding up to about 100 km. We confirm recent findings of H2O increasing at high altitudes during Ls = 190-205° in MY 34, reaching abundances of about 150 ppmv at 80 km in both hemispheres not found during the same period of MY 35. We found a hygropause’s steep rising during the GDS from 30 up to 80 km. Furthermore, strong supersaturation events have been identified at mesospheric altitudes even in presence of water ice layers retrieved by the IAA team.
154. First Observation of the Oxygen 630 nm Emission in the Martian Dayglow
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Gérard, J.‐C., Aoki, S., Gkouvelis, L., Soret, L., Willame, Y., Thomas, I.R., Depiesse, C., Ristic, B., Vandaele, A. C., Hubert, B., Daerden, F., Patel, M. R., López‐Moreno, J.‐J., Bellucci, G., Mason, J. P., López‐Valverde, M. A., Gérard, J.‐C., Aoki, S., Gkouvelis, L., Soret, L., Willame, Y., Thomas, I.R., Depiesse, C., Ristic, B., Vandaele, A. C., Hubert, B., Daerden, F., Patel, M. R., López‐Moreno, J.‐J., Bellucci, G., Mason, J. P., and López‐Valverde, M. A.
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Following the recent detection of the oxygen green line airglow on Mars, we have improved the statistical analysis of the data recorded by the NOMAD/UVIS instrument on board the ExoMars Trace Gas Orbiter mission by summing up hundreds of spectra to increase the signal to noise ratio. This led to the observation of the OI 630 nm emission, a first detection in a planetary atmosphere outside the Earth. The average limb profile shows a broad peak intensity of 4.8 kR near 150 km. Comparison with a photochemical model indicates that it is well predicted by current photochemistry, considering the sources of uncertainty. The red/green line intensity ratio decreases dramatically with altitude as a consequence of the efficient quenching of O(1D) by CO2. Simultaneous observations of the green and red dayglow will provide information on variations in the thermosphere in response to seasonal changes and the effects of solar events.
155. NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance
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Vandaele, A. C., Lopez-Moreno, J. -J., Patel, M. R., Bellucci, G., Daerden, F., Ristic, B., Robert, S., Thomas, I. R., Wilquet, V., Allen, M., Alonso-Rodrigo, G., Altieri, F., Aoki, S., Bolsée, D., Clancy, R. T., Cloutis, E., Depiesse, C., Drummond, R. J., Fedorova, A., Formisano, V., Funke, B., González-Galindo, F., Geminale, A., Gérard, J. -C., Giuranna, M., Hetey, L., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Leese, M., Lefèvre, F., Lewis, S. R., López-Puertas, M., López-Valverde, M., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Renotte, E., Rodriguez-Gomez, J., Sindoni, G., Smith, M., Stiepen, A., Trokhimovsky, A., Vander Auwera, J., Villanueva, G., Viscardy, S., Whiteway, J., Willame, Y., Wolff, M. J., the NOMAD team, Vandaele, A. C., Lopez-Moreno, J. -J., Patel, M. R., Bellucci, G., Daerden, F., Ristic, B., Robert, S., Thomas, I. R., Wilquet, V., Allen, M., Alonso-Rodrigo, G., Altieri, F., Aoki, S., Bolsée, D., Clancy, R. T., Cloutis, E., Depiesse, C., Drummond, R. J., Fedorova, A., Formisano, V., Funke, B., González-Galindo, F., Geminale, A., Gérard, J. -C., Giuranna, M., Hetey, L., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Leese, M., Lefèvre, F., Lewis, S. R., López-Puertas, M., López-Valverde, M., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Renotte, E., Rodriguez-Gomez, J., Sindoni, G., Smith, M., Stiepen, A., Trokhimovsky, A., Vander Auwera, J., Villanueva, G., Viscardy, S., Whiteway, J., Willame, Y., Wolff, M. J., and the NOMAD team
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The NOMAD (“Nadir and Occultation for MArs Discovery”) spectrometer suite on board the ExoMars Trace Gas Orbiter (TGO) has been designed to investigate the composition of Mars’ atmosphere, with a particular focus on trace gases, clouds and dust. The detection sensitivity for trace gases is considerably improved compared to previous Mars missions, compliant with the science objectives of the TGO mission. This will allow for a major leap in our knowledge and understanding of the Martian atmospheric composition and the related physical and chemical processes. The instrument is a combination of three spectrometers, covering a spectral range from the UV to the mid-IR, and can perform solar occultation, nadir and limb observations. In this paper, we present the science objectives of the instrument and explain the technical principles of the three spectrometers. We also discuss the expected performance of the instrument in terms of spatial and temporal coverage and detection sensitivity.
156. CO2 retrievals in the Mars daylight thermosphere from 4.3 µm limb emissions
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Jiménez Monferrer, Sergio, López Valverde, M. A., Funke, Bernd, European Commission, and Ministerio de Economía, Industria y Competitividad (España)
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Mars ,Martian atmosphere ,Marte ,Atmósfera marciana - Abstract
[EN] Mars is a vast and complex world. It is a terrestrial planet with a reddish appearance, due to a surface mostly covered by ferric oxide dust and rocks. Mars has a faint atmosphere mainly composed of carbon dioxide (CO2), with atmospheric circulation and weather patters, like Earth.It has, however, remarkable diurnal oscillation of winds, due to a considerable thermal excursion. Despite the importance of the thermosphere, for instance, to the atmospheric escape to space, this is maybe the less known region of the Martian atmosphere. Most of the information we have of these altitudes comes from very disperse and unconnected sources. Among them,a few in situ profiles taken during the descent of some missions, like Viking 1 and 2, the aerobraking manoeuvres by the Mars Global Surveyor and Mars Reconnaissance Orbiter spacecrafts, the SPICAM instrument on board Mars Express, and the instruments on board the MAVEN mission. These measurements allowed to obtain density and temperature profiles, and to study the seasonal and geographical variabilities of the thermosphere. According to these observations and their numerical simulations, the thermosphere of Mars is a complex and dynamic region, strongly coupled to lower layers. Concretely, the effects caused by the dust storms and the temperature variability in the low atmosphere are propagated upwards up to the thermosphere. To understand this region, it is therefore necessary a global view of the atmosphere, from its interactions with the surface, to the exchanges of species with the exosphere. The thermospheric data previously described have a limited temporal and geographical coverage. Some important issues, like the influence of solar activity, are difficult to understand from the available data. Most of them, except aerobraking measurements, concentrate in the night side of the planet, leaving the diurnal thermosphere almost unexplored. It is in the dayside thermosphere where the strongest infrared atmospheric non-thermal emissions are produced. These infrared emissions offer an interesting possibility for remote sounding at these heights in all terrestrial planets. There are indeed thermospheric observations of Mars in the infrared, but they have not been sufficiently exploited so far, due to the complexity of the physical interpretation and the numeric difficulty of the required mathematical inversion. These observations were acquired by two instruments on board Mars Express, OMEGA and PFS. Their analysis is expected to provide a wider and deeper understanding of the dayside thermosphere at the maximum sensitivity altitudes., [EN]In the Group of Terrestrial Planetary Atmospheres (GAPT, for its Spanish acronym) at the Instituto de Astrofı́sica de Andalucı́a (IAA), a large experience on non-thermal atmospheric emissions, physical models for the Mars atmosphere, and tools for the inversion of such emissions are available. Molecular species, like CO2 , produce strong non-thermal emissions in the infrared in the higher layers of the atmosphere. At those altitudes, the density is so low and molecular collisions are so rare that local thermodynamic equilibrium (LTE) conditions no longer apply. The departure from LTE typically occurs in the diurnal hemisphere when such species are excited by solar radiation in the rotational-vibrational bands in the near and medium infrared (between 1 and 10 um). The emissions produced contain information on the densities of the emitting species, and therefore contribute to the extraction of density and temperature profiles in the higher atmosphere. Some difficulties arise with this type of observations. First, the emission of these tenuous layers is low, so the observation in limb geometry, where the emission of a large atmospheric path is integrated on the detector, is extremely helpful. Besides, inherent difficulties arise when dealing with non-LTE conditions, as this approximation is not valid. This issue is solved by the use of inversion codes including a non-LTE model in the forward calculation (fundamental tool of the inverse problem). Finally, the lack of local measurements of the atmospheric magnitudes involved, needed to start and guide the retrieval, is overcame by the assumption of a priori conditions predicted by 3-D numerical simulations by state-of-the-art General Circulation Models of Mars. We analysed limb infrared CO2 emissions, in the region around 4.3 um, obtained by OMEGA in the daylight thermosphere of Mars, in order to infer information on fundamental atmospheric parameters, like density and temperature. These emissions are caused by CO2 fluorescence of solar radiation, and the investigation needs to take into account non-LTE conditions. We performed a radiometric calibration on the data provided by OMEGA, cleaned the available spectra, including the use of clustering techniques, and generated radiance vertical profiles for each orbital dataset. The distribution and geometry of the spectra acquired by OMEGA are highly heterogeneous, leading to very different projections in the limb of the Martian atmosphere. For this reason, a series of geometric criteria was established in order to allow for an easier and consistent comparison among the results of the retrievals., [EN]Once the radiance vertical profiles were generated, we applied a non-LTE retrieval scheme based on a extensively validated scheme working for Earth, which we adapted to Martian conditions. In this work we present information on the inversion set up, and a discussion on the retrieved CO2 density profiles. A total of 742 profiles were formed from the 47 OMEGA orbits with limb observations previously selected. The convergence rate achieved considering the entire dataset was 94%, which is considered as very satisfactory. From the retrieved CO2 densities, we derived temperature profiles, assuming hydrostatic equilibrium. For this, we made use of an algorithm developed for that task. For 60% of the orbits analysed we found a minimum in the temperature profile at 140–150 km, indicating a thermosphere colder than that of the model used, the LMD-MGCM. On the opposite side, a thermosphere warmer than that predicted by the model was obtained in 30% of the orbits. An extensive sensitivity study of the retrieval scheme was also carried out. We found that, in general, the uncertainty due to the instrumental Gain calibration and that caused by the retrieval noise error itself are of primary importance, while the influence of the temperatures in the reference atmosphere used as a priori, provided by our General Circulation Model (GCM), is minor. According to our study, CO2 profiles can be derived with a precision of around 20% and a vertical resolution of around 15 km between 120 and 160 km tangent altitude. Finally, we compared the density and temperature profiles obtained to the predictions of the LMD-MGCM and to the results recently provided by other instruments studying the Martian thermosphere. In general, no clear correlation of the data-model discrepancies obtained with any temporal or spatial dimension is observed, neither from a global study nor when a more homogeneous subset of OMEGA observations, i.e., at constrained geolocation, is analysed. There is one exception, the solar zenith angle, which affects the atmospheric emission. Most observations from other instruments, like in situ or remote measurements by NGIMS and by IUVS (both on board MAVEN), respectively, have uncertainties of the order of those presented in this work. The results from these experiments also bring to light important differences when compared to the LMD-MGCM or other General Circulation Models. This global comparison with numeric simulations indicates an atmospheric variability in line with that found in our OMEGA data. This result points to the necessity of validation of global models at thermospheric altitudes. The thermosphere of Mars is, indeed, a complex and dynamic region., [ES] Marte es un mundo vasto y complejo. Un planeta rojizo, debido a su superficie, ampliamente cubierta por polvo y rocas de óxido férrico. Marte tiene una atmósfera tenue, principalmente compuesta por dióxido de carbono (CO2), con circulación atmosférica y patrones climáticos, como la Tierra. Sin embargo, tiene destacadas oscilaciones diurnas de viento, debido a una excursión térmica considerable. Las oscilaciones tienen un efecto en todas las capas de la atmósfera, y ejercen una influencia apreciable sobre el resto de la circulación atmosférica global de Marte. En la ultima década, varias misiones han viajado al Planeta Rojo y algunas más han sido aprobadas para ser lanzadas en los próximos años. Dos de estas misiones han sido diseñadas, construidas y operadas por/desde Europa, y son especialmente relevantes para esta Tesis: Mars Express y ExoMars, This work was conducted as part of the project UPWARDS-633127 under the European Union's Horizon 2020 research and innovation Programme. The IAA team was supported by the Spanish Ministry of Economy, Industry and Competitiveness and by FEDER funds under grant ESP2015-65064-C2-1-P (MINECO/FEDER)
- Published
- 2019
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