Persona: Yela González, Margarita
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Instituto Nacional de Técnica Aeroespacial
El Instituto Nacional de Técnica Aeroespacial es el Organismo Público de Investigación (OPI) dependiente del Ministerio de Defensa. Además de realizar actividades de investigación científica y de desarrollo de sistemas y prototipos en su ámbito de conocimiento, presta servicios tecnológicos a empresas, universidades e instituciones.
El INTA está especializado en la investigación y el desarrollo tecnológico, de carácter dual, en los ámbitos de la Aeronáutica, Espacio, Hidrodinámica, Seguridad y Defensa.
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Yela González
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Margarita
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Publicación Acceso Abierto Dust Devil Frequency of Occurrence and Radiative Effects at Jezero Crater, Mars, as Measured by MEDA Radiation and Dust Sensor (RDS)(GU Advancing Earth and Space Science, 2023-01-17) Toledo, D.; Apéstigue, Víctor; Arruego, Ignacio; Lemmon, M. T.; Gómez Martín, L.; Montoro, F.; Hueso, R.; Newman, C. E.; Smith, Michael D.; Viúdez Moreiras, Daniel; Martínez, Germán M.; Vicente Retortillo, Álvaro; Sánchez Lavega, Agustín; De la Torre Juárez, M.; Rodríguez Manfredi, J. A.; Carrasco, I.; Yela González, Margarita; Jiménez Martín, Juan José; García-Menéndez, Elisa; Navarro López, Sara; Gómez Elvira, J.; Harri, Ari-Matti; Polkko, J.; Hieta, M.; Genzer, María; Murdoch, N.; Sebastián, E.; Agencia Estatal de Investigación (AEI); Ministerio de Ciencia e Innovación (MICINN); Ministerio de Economía y Competitividad (MINECO); NASA Jet Propulsion Laboratory (JPL); National Aeronautics and Space Administration (NASA); Gobierno VascoThe Mars Environmental Dynamics Analyzer, onboard the Perseverance rover, is a meteorological station that is operating on Mars and includes, among other sensors, the radiometer Radiation and Dust Sensor (RDS). From RDS irradiance observations, a total of 374 dust devils (DDs) were detected for the first 365 sols of the mission (Ls = 6°–182°), which along with wind and pressure measurements, we estimated a DD frequency of formation at Jezero between 1.3 and 3.4 DD km−2 sol−1 (increasing as we move from spring into summer). This frequency is found to be smaller than that estimated at the Spirit or Pathfinder landing sites but much greater than that derived at InSight landing site. The maximum in DD frequency occurs between 12:00 and 13:00 local true solar time, which is when the convective heat flux and lower planetary boundary layer IR heating are both predicted to peak in Jezero crater. DD diameter, minimum height, and trajectory were studied showing (a) an average diameter of 29 m (or a median of 25 m) and a maximum and minimum diameter of 132 ± 63.4 and 5.6 ± 5.5 m; (b) an average minimum DD height of 231 m and a maximum minimum-height of 872 m; and (c) the DD migration direction is in agreement with wind measurements. For all the cases, DDs decreased the UV irradiance, while at visible or near-IR wavelengths both increases and decreases were observed. Contrary to the frequency of formation, these results indicate similar DD characteristics in average for the studied period.Publicación Restringido Measurement of dust optical depth using the solar irradiance sensor (SIS) onboard the ExoMars 2016 EDM(Elsevier, 2017-01-20) Toledo, D.; Arruego, Ignacio; Apéstigue, Víctor; Jiménez Martín, Juan José; Gómez Martín, L.; Yela González, Margarita; Rannou, P.; Pommereau, J. P.; Instituto Nacional de Técnica Aeroespacial (INTA); Ministerio de Economía y Competitividad (MINECO)"The solar irradiance sensor (SIS) was included in the DREAMS package onboard the ExoMars 2016 Entry Descent and Landing Demonstrator Module, and has been selected in the METED meteorological station onboard the ExoMars 2020 Lander. This instrument is designed to measure at different time intervals the scattered flux or the sum of direct flux and scattered flux in UVA (315-400 nm) and NIR (700-1100 nm) bands. For SIS'16, these measurements are performed by a total of 3 sensors per band placed at the faces of a truncated tetrahedron with face inclination angles of 60. The principal goal of SIS'16 design is to perform measurements of the dust opacity in UVA and NIR wavelengths ranges, crucial parameters in the understanding of the Martian dust cycle. The retrieval procedure is based on the use of radiative transfer simulations to reproduce SIS observations acquired during daytime as a function of dust opacity. Based on different sensitivity analysis, the retrieval procedure also requires to include as free parameters (1) the, dust effective radius; (2) the dust effective variance; and (3) the imaginary part of the refractive index of dust particles in UVA band. We found that the imaginary part of the refractive index of dust particles does not have a big impact on NIR signal, and hence we can kept constant this parameter in the retrieval of dust opacity at this channel. In addition to dust opacity measurements, this instrument is also capable to detect and characterize clouds by looking at the time variation of the color index (CI), defined as the ratio between the observations in NIR and UVA channels, during daytime or twilight. By simulating CI signals with a radiative transfer model, the cloud opacity and cloud altitude (only during twilight) can be retrieved. Here the different retrieval procedures that are used to analyze SIS measurements, as well as the results obtained in different sensitivity analysis, are presented and discussed."Publicación Acceso Abierto Polar Stratospheric Clouds Detection at Belgrano II Antarctic Station with Visible Ground-Based Spectroscopic Measurements(Multidisciplinary Digital Publishing Institute (MDPI), 2021-04-07) Gómez Martín, L.; Toledo, D.; Prados Roman, C.; Jose, Adame; Ochoa, H.; Yela González, Margarita; Agencia Estatal de Investigación (AEI); Gómez Martín, L. [0000-0002-6655-7659]; Prados Roman, C. [0000-0001-8332-0226]; Adame, J. A. [0000-0002-6302-7193]By studying the evolution of the color index (CI) during twilight at high latitudes, polar stratospheric clouds (PSCs) can be detected and characterized. In this work, this method has been applied to the measurements obtained by a visible ground-based spectrometer and PSCs have been studied over the Belgrano II Antarctic station for years 2018 and 2019. The methodology applied has been validated by full spherical radiative transfer simulations, which confirm that PSCs can be detected and their altitude estimated with this instrumentation. Moreover, our investigation shows that this method is useful even in presence of optically thin tropospheric clouds or aerosols. PSCs observed in this work have been classified by altitude. Our results are in good agreement with the stratospheric temperature evolution obtained by the global meteorological model ECMWF (European Centre for Medium Range Weather Forecasts) and with satellite PSCs observations from CALIPSO (Cloud-Aerosol-Lidar and Infrared Pathfinder Satellite Observations). To investigate the presence and long-term evolution of PSCs, the methodology used in this work could also be applied to foreseen and/or historical observations obtained with ground-based spectrometers such e. g. those dedicated to Differential Optical Absorption Spectroscopy (DOAS) for trace gas observation in Arctic and Antarctic sites.Publicación Acceso Abierto A trajectory-based estimate of the tropospheric ozone column using the residual method(AGU Publishing, 2007-12-19) Schoeberl, M. R.; Ziemke, J. R.; Bojkov, B. ; Livesey, N.; Duncan, B.; Strahan, S.; Froidevaux, L.; Kulawik, S.; Bhartia, P. K.; Chandra, S.; Levelt, P. F.; Witte, J. C.; Thompson, A. M.; Cuevas, E.; Redondas, A.; Tarasick, D. W.; Davies, Jonathan; Bodeker, G.; Hansen, G.; Johnson, B. J. ; Oltmans, S. J.; Vömel, H.; Allaart, M.; Kelder, H.; Newchurch, M.; Godin Beekmann, S.; Ancellet, G.; Claude, H.; Andersen, S. B.; Kyrö, Esko; Parrondo, María Concepción; Yela González, Margarita; Zablocki, G.; Moore, D.; Dier, H.; Von der Gathen, P.; Viatte, P.; Stübi, R.; Calpini, B.; Skrivankova, P.; Dorokhov, V.; De Backer, H.; Schmidlin, F. J.; Coetzee, G.; Fujiwara, M.; Thouret, V.; Posny, F.; Morris, G.; Merrill, J.; Leong, C. P.; Koenig Langlo, G.; Joseph, E.[1] We estimate the tropospheric column ozone using a forward trajectory model to increase the horizontal resolution of the Aura Microwave Limb Sounder (MLS) derived stratospheric column ozone. Subtracting the MLS stratospheric column from Ozone Monitoring Instrument total column measurements gives the trajectory enhanced tropospheric ozone residual (TTOR). Because of different tropopause definitions, we validate the basic residual technique by computing the 200-hPa-to-surface column and comparing it to the same product from ozonesondes and Tropospheric Emission Spectrometer measurements. Comparisons show good agreement in the tropics and reasonable agreement at middle latitudes, but there is a persistent low bias in the TTOR that may be due to a slight high bias in MLS stratospheric column. With the improved stratospheric column resolution, we note a strong correlation of extratropical tropospheric ozone column anomalies with probable troposphere-stratosphere exchange events or folds. The folds can be identified by their colocation with strong horizontal tropopause gradients. TTOR anomalies due to folds may be mistaken for pollution events since folds often occur in the Atlantic and Pacific pollution corridors. We also compare the 200-hPa-to-surface column with Global Modeling Initiative chemical model estimates of the same quantity. While the tropical comparisons are good, we note that chemical model variations in 200-hPa-to-surface column at middle latitudes are much smaller than seen in the TTOR.Publicación Acceso Abierto Methane precipitation in ice giant atmospheres(EDP Sciences, 2025-02-04) Toledo, D. ; Rannou, P.; Irwin, P.; De Batz de Trenquelléon, B.; Roman, Michael , M.; Apéstigue, Víctor; Arruego, Ignacio; Yela González, Margarita; Agencia Estatal de Investigación (AEI)Context. Voyager-2 radio occultation measurements have revealed changes in the atmospheric refractivity within a 2–4 km layer near the 1.2-bar level in Uranus and the 1.6-bar level in Neptune. These changes were attributed to the presence of a methane cloud, consistent with the observation that methane concentration decreases with altitude above these levels, closely following the saturation vapor pressure. However, no clear spectral signatures of such a cloud have been detected thus far in the spectra acquired from both planets. Aims. We examine methane cloud properties in the atmospheres of the ice giants, including vertical ice distribution, droplet radius, precipitation rates, timescales, and total opacity, employing microphysical simulations under different scenarios. Methods. We used a one-dimensional (1D) cloud microphysical model to simulate the formation of methane clouds in the ice giants. The simulations include the processes of nucleation, condensation, coagulation, evaporation, and precipitation, with vertical mixing simulated using an eddy-diffusion profile (Keddy). Results. Our simulations show cloud bases close to 1.24 bars in Uranus and 1.64 bars in Neptune, with droplets up to 100 µm causing high settling velocities and precipitation rates (∼370 mm per Earth year). The high settling velocities limit the total cloud opacity, yielding values at 0.8 µm of ∼0.19 for Uranus and ∼0.35 for Neptune, using Keddy = 0.5 m2 s−1 and a deep methane mole fraction (μCH4) of 0.04. In addition, lower Keddy or μCH4 values result in smaller opacities. Methane supersaturation is promptly removed by condensation, controlling the decline in μCH4 with altitude in the troposphere. However, the high settling velocities prevent the formation of a permanent thick cloud. Stratospheric hazes made of ethane or acetylene ice are expected to evaporate completely before reaching the methane condensation level. Since hazes are required for methane heterogeneous nucleation, this suggests either a change in the solid phase properties of the haze particles, inhibiting evaporation, or the presence of photochemical hazes.Publicación Acceso Abierto Drying of the Martian mesosphere during aphelion induced by lower temperatures(Springer Nature, 2024-11-20) Toledo, D.; Rannou, P.; Apéstigue, Víctor; Rodríguez Veloso, Raúl; Rodríguez Manfredi, J. A.; Arruego, Ignacio; Martínez, Germán M.; Tamppari, L. K.; Munguira, A.; Lorenz, Ralph; Stcherbinine, Aurélien; Montmessin, F.; Sánchez Lavega, Agustín; Patel, P.; Smith, Michael D.; Lemmon, M. T.; Vicente Retortillo, Álvaro; Newman, C. E.; Viúdez Moreiras, Daniel; Hueso, R.; Bertrand, T.; Pla García, J.; Yela González, Margarita; De la Torre Juárez, M.; Ministerio de Ciencia e Innovación (MICINN); Jet Propulsion Laboratory (JPL); National Aeronautics and Space Administration (NASA); Gobierno Vasco; Agencia Estatal de Investigación (AEI); Unidad de Excelencia Científica María de Maeztu Instituto de Astrofísica de Cantabria, MDM-2017-0765The formation of water ice clouds or hazes on Mars imposes substantial limitations on the vertical transport of water into the middle-upper atmosphere, impacting the planet’s hydrogen loss. Recent observations made by the Mars Environmental Dynamics Analyzer instrument onboard Mars 2020 Perseverance rover have shown a marked decline in water ice abundance within the mesosphere (above 35-40 km) when Mars is near its aphelion (near the northern summer solstice), notably occurring during solar longitudes (Ls) between Ls 70∘ and 80∘. Orbital observations around the same latitudes indicate that temperatures between ~ 30-40 km reach a minimum during the same period. Using cloud microphysics simulations, we demonstrate that this decrease in temperature effectively increases the amount of water cold-trapped at those altitudes, confining water ice condensation to lower altitudes. Similarly, the reinforcement of the cold trap induced by the lower temperatures results in significant reductions in the water vapor mixing ratio above 35–40 km, explaining the confinement of water vapor observed around aphelion from orbiters.Publicación Acceso Abierto Ground-based validation of the Copernicus Sentinel-5P TROPOMI NO2 measurements with the NDACC ZSL-DOAS, MAX-DOAS and Pandonia global networks(European Geoscience Union (EGU), 2021-01-22) Verhoelst, T.; Compernolle, S.; Pinardi, G.; Lambert, J. C.; Eskes, H. J.; Eichmann, K. U.; Fjaeraa, A. M.; Granville, J.; Niemeijer, S.; Cede, A.; Tiefengraber, M.; Hendrick, F.; Pazmiño, A.; Bais, A.; Bazureau, A.; Folkert Boersma, K.; Bognar, K.; Dehn, A.; Donner, S.; Elokhov, A.; Gebetsberger, M.; Goutail, F.; Grutter de la Mora, M.; Gruzdev, A.; Gratsea, M.; Hansen, G. H.; Irie, H.; Jepsen, N.; Kanaya, Y.; Karagkiozidis, D.; Kivi, R.; Kreher, K.; Levelt, P. F.; Liu, C.; Müller, M.; Navarro-Comas, Mónica; Piters, Ankie; Pommereau, J. P.; Portafaix, T.; Prados Roman, C.; Puentedura, O.; Querel, R.; Remmers, J.; Richter, A.; Rimmer, J.; Rivera Cárdenas, C.; Saavedra de Miguel, Lidia; Sinyakov, V. P.; Stremme, W.; Strong, K.; Van Roozendael, M.; Pepijn Veefkind, J.; Wagner, T.; Wittrock, F.; Yela González, Margarita; Zehner, C.; European Space Agency (ESA); French Institut National des Sciences de l'Univers (INSU); Centre National D'Etudes Spatiales (CNES); Centre National de la Recherche Scientifique (CNRS); Institut polaire français Paul Emile Victor (IPEV); Belgian Science Policy Office (BELSPO); Verhoelst, T. [0000-0003-0163-9984]; Compernolle, S. [0000-0003-0872-0961]; Pinardi, G. [0000-0001-5428-916X]; Eskes, H. [0000-0002-8743-4455]; Bais, A. [0000-0003-3899-2001]; Folkert Boersma, K. [0000-0002-4591-7635]; Bognar, K. [0000-0003-4619-2020]; Donner, S. [0000-0001-8868-167X]; Elokhov, A. [0000-0003-4725-9186]; Grutter de la Mora, M. [0000-0001-9800-5878]; Gruzdev, A. [0000-0003-3224-1012]; Karagkiozidis, D. [0000-0002-3595-0538]; Kivi, R. [0000-0001-8828-2759]; Liu, C. [0000-0002-3759-9219]; Müller, M. [0000-0001-5284-5425]; Pommereau, J. P. [0000-0002-8285-9526]; Prados Roman, C. [0000-0001-8332-0226]; Puentedura, O. [0000-0002-4286-1867]; Querel, R. [0000-0001-8792-2486]; Richter, A. [0000-0003-3339-212X]; Rivera Cárdenas, C. [0000-0002-8617-265X]; Stremme, W. [0000-0003-0791-3833]; Strong, K. [0000-0001-9947-1053]; Pepijn Veefkind, J. [0000-0003-0336-6406]This paper reports on consolidated ground-based validation results of the atmospheric NO2 data produced operationally since April 2018 by the TROPOspheric Monitoring Instrument (TROPOMI) on board of the ESA/EU Copernicus Sentinel-5 Precursor (S5P) satellite. Tropospheric, stratospheric, and total NO2 column data from S5P are compared to correlative measurements collected from, respectively, 19 Multi-Axis Differential Optical Absorption Spectroscopy (MAX-DOAS), 26 Network for the Detection of Atmospheric Composition Change (NDACC) Zenith-Scattered-Light DOAS (ZSL-DOAS), and 25 Pandonia Global Network (PGN)/Pandora instruments distributed globally. The validation methodology gives special care to minimizing mismatch errors due to imperfect spatio-temporal co-location of the satellite and correlative data, e.g. by using tailored observation operators to account for differences in smoothing and in sampling of atmospheric structures and variability and photochemical modelling to reduce diurnal cycle effects. Compared to the ground-based measurements, S5P data show, on average, (i) a negative bias for the tropospheric column data, of typically −23 % to −37 % in clean to slightly polluted conditions but reaching values as high as −51 % over highly polluted areas; (ii) a slight negative median difference for the stratospheric column data, of about −0.2 Pmolec cm−2, i.e. approx. −2 % in summer to −15 % in winter; and (iii) a bias ranging from zero to −50 % for the total column data, found to depend on the amplitude of the total NO2 column, with small to slightly positive bias values for columns below 6 Pmolec cm−2 and negative values above. The dispersion between S5P and correlative measurements contains mostly random components, which remain within mission requirements for the stratospheric column data (0.5 Pmolec cm−2) but exceed those for the tropospheric column data (0.7 Pmolec cm−2). While a part of the biases and dispersion may be due to representativeness differences such as different area averaging and measurement times, it is known that errors in the S5P tropospheric columns exist due to shortcomings in the (horizontally coarse) a priori profile representation in the TM5-MP chemical transport model used in the S5P retrieval and, to a lesser extent, to the treatment of cloud effects and aerosols. Although considerable differences (up to 2 Pmolec cm−2 and more) are observed at single ground-pixel level, the near-real-time (NRTI) and offline (OFFL) versions of the S5P NO2 operational data processor provide similar NO2 column values and validation results when globally averaged, with the NRTI values being on average 0.79 % larger than the OFFL values.Publicación Acceso Abierto Using the Perseverance MEDA-RDS to identify and track dust devils and dust-lifting gust fronts(Frontiers, 2023-10-11) Toledo, D.; Apéstigue, Víctor; Martínez Oter, J.; Franchi, Fulvio; Serrano, F.; Yela González, Margarita; De la Torre Juárez, M.; Rodríguez Manfredi, J. A.; Arruego, Ignacio; European Commission (EC); Agencia Estatal de Investigación (AEI); Ministerio de Economía y Competitividad (MINECO)In the framework of the Europlanet 2024 Research Infrastructure Transnational Access programme, a terrestrial field campaign was conducted from 29 September to 6 October 2021 in Makgadikgadi Salt Pans (Botswana). The main goal of the campaign was to study in situ the impact of the dust devils (DDs) on the observations made by the radiometer Radiation and Dust Sensor (RDS), which is part of the Mars Environmental Dynamics Analyzer instrument, on board NASA’s Mars 2020 Perseverance rover. Several DDs and dust lifting events caused by non-vortex wind gusts were detected using the RDS, and the different impacts of these events were analyzed in the observations. DD diameter, advection velocity, and trajectory were derived from the RDS observations, and then, panoramic videos of such events were used to validate these results. The instrument signal variations produced by dust lifting (by vortices or wind gusts) in Makgadikgadi Pans are similar to those observed on Mars with the RDS, showing the potential of this location as a Martian DD analog.Publicación Restringido OClO, NO2 and O3 total column observations over Iceland during the winter 1993/94(AGU Publishing, 1996-11-15) Gil, M.; Puentedura, O.; Yela González, Margarita; Parrondo, María Concepción; Jadhav, D. B.; Thorkelsson, B.Ground-based observation of OClO, NO2, and O3 columns by differential UV-Visible spectroscopy at twilight during the fall winter of 1993/94 at the sub-Arctic station of Reykjavik (64°N, 23°W) are presented. Results show no direct evidence of ozone depletion during the period but significant amounts of OClO were observed in December and January when NO2 abundances were at the annual minimum. NO2 columns are found to be controlled by the hours of light available but highly modulated by the lower stratosphere temperature. OClO was observed outside the vortex as well, but only at times when NO2 was low.Publicación Restringido DREAMS-SIS: The Solar Irradiance Sensor on-board the ExoMars 2016 lander(Elsevier, 2017-07-01) Arruego, Ignacio; Apéstigue, Víctor; Jiménez Martín, Juan José; Martínez Oter, Javier; Álvarez Ríos, F. J.; González Guerrero, M.; Rivas, J.; Azcue, J.; Martín, I.; Toledo, D.; Gómez Martín, L.; Jiménez Michavila, M.; Yela González, Margarita; Instituto Nacional de Técnica Aeroespacial (INTA); Ministerio de Economía y Competitividad (MINECO)The Solar Irradiance Sensor (SIS) was part of the DREAMS (Dust characterization, Risk assessment, and Environment Analyzer on the Martian Surface) payload package on board the ExoMars 2016 Entry and Descent Module (EDM), “Schiaparelli”. DREAMS was a meteorological station aimed at the measurement of several atmospheric parameters, as well as the presence of electric fields, during the surface operations of EDM. DREAMS-SIS is a highly miniaturized lightweight sensor designed for small meteorological stations, capable of estimating the aerosol optical depth (AOD) several times per sol, as well as performing a direct measurement of the global (direct plus scattered) irradiance on the Martian surface in the spectral range between 200 and 1100 nm. AOD is estimated from the irradiance measurements at two different spectral bands – Ultraviolet (UV) and near infrared (NIR) – which also enables color index (CI) analysis for the detection of clouds. Despite the failure in the landing of Schiaparelli, DREAMS-SIS is a valuable precursor for new developments being carried-on at present. The concept and design of DREAMS-SIS are here presented and its operating principles, supported by preliminary results from a short validation test, are described. Lessons learnt and future work towards a new generation of Sun irradiance sensors is also outlined.
