(Espacio) Comunicaciones de Congresos
URI permanente para esta colecciónhttps://digitalpre.inta.es/handle/123456789/57
Buscar
Suscribirse para recibir un correo electrónico cada vez que se introduzca un ítem en esta colección.
Envíos recientes
Ítem Acceso Abierto Front-End Electronic for Miniaturized LIDAR Signal Conditioning(Europlanet, 2024-07-03) Andrés Velasco, Santiago; Rivas Abalo, Joaquín; Arruego, I.; Vázquez Yañez, G. A.; Montalvo Chacón, S.; Muñoz García, E.; Martín Ortega, A.; Jiménez Martín, Juan José; García Menéndez, Elisa; Moya Señas, AlbertoThe Miniaturized LIDAR for MARS Atmospheric Research (MiLi) project falls within the European Union funding program called Horizon Europe [1]. Within this general framework, the project being presented is classified under cluster 4 - Digital, Industry, and Space [2]. The investment in the different projects within this fourth point pursues the idea of global leadership of the European industry in key areas, through the development of competitive and trustworthy technologies. This sets the foundation for a competitive, digital, sustainable, and circular industry that allows for progress and innovation in global societal challenges.Ítem Acceso Abierto Lunar In-situ Navigation and Communication Node - LUNINA(Europlanet, 2024-07-03) Haukka, H.; Kestilä, Antti; Arruego, I.; Harri, Ari-Matti; Genzer, María; Apéstigue, V.; Hieta, M.; Camañes, Carmen; Ortega, Cristina; Kivekäs. Jarmo; Koskimaa, PetriLUNINA is an in-situ navigation and communication node. Proposed LUNINA platform is designed to be a compact, independent, cost effective, robust, and location independent navigation beacon and communication relay on the Moon that can operate 24/7.Ítem Acceso Abierto Microphysical modeling of methane ice clouds in the atmospheres of the Ice Giants(Europlanet, 2024-07-03) Toledo, D.; Rannou, P.; Irwin, Patrick Gerard Joseph; De Batz de Trenquelléon, Bruno; Apéstigue, V.; Roman, Michael; Arruego, I.; Yela González, M.Voyager 2 radio occultation measurements of Uranus and Neptune revealed a layer approximately 2-4 km thick near 1.2 and 1.6 bars, respectively, wherein the atmospheric refractivity exhibited a slope variation (1, 2). These findings were interpreted as indicating a region where methane gas was undergoing condensation, forming an ice cloud centered around this pressure level. While the formation of this putative cloud would explain the observed decrease in methane abundance with height above 1.2 and 1.6 bars, or the banded structure of Uranus through latitudinal variations in the opacity of this cloud, several recent works and observations do not provide direct evidence in favor of this cloud (3): (i) radiative transfer models show an enhancement in the scattering opacity at pressures near 4-6 bars, more consistent with the presence of H2S ice (4, 5); (ii) observations from ground-based telescopes (or observations from telescopes in orbit around the Earth) of methane clouds indicate cloud tops near 0.4 bars in both planets (6), approximately a scale height above the base of the putative methane cloud.Ítem Acceso Abierto Aerosol optical properties observed by MEDA Radiation an Dust Sensor (RDS) at Jezero Crater, Mars(Europlanet, 2024-07) Rodríguez Veloso, Raúl; Toledo, D.; Apéstigue, V.; Arruego, I.; Lemmon, M. T.; Smith, Michael D.; Martínez, Germán M.; Vicente Retortillo, Álvaro; Jiménez Martín, Juan José; García Menéndez, Elisa; Viúdez Moreiras, Daniel; Sánchez Lavega, Agustín; Pérez Hoyos, S.; Sebastián, E.; De la Torre Juárez, M.; Rodríguez Manfredi, J. A.Aerosols on Mars are a primary elements for studying the interaction between the solar radiation and the atmosphere and surface. Depending on properties such as aerosol number density, particle radius, or refractive index, the impact of the aerosols can provide positive or negative radiative feedbacks on the dynamics of the atmosphere. Previous studies have revealed large temporal and spatial variability in the aerosol optical properties, emphasizing the necessity for continuous monitoring of these properties throughout the day and at multiple locations. To address these measurements, the Radiation and Dust Sensor (RDS) [1] is part of the Mars Environmental Dynamics Analyzer (MEDA) [2] payload onboard of the Mars 2020 rover Perseverance. RDS instrument compromises two sets of 8 photodiodes (RDS-DP) and a camera (RDS-SkyCam). One set of photodiodes is pointed upward, with each one covering a different wavelength range between 190-1200 nm. The other set is pointed sideways, 20 degrees above the horizon, and they are spaced 45 degrees apart in azimuth to sample all directions at a single wavelength. The analysis of these observations with a radiative transfer model [3] (Fig. 1) allow us to fit aerosol parameters such as the aerosol opacity at different wavelengths or the aerosol particle radius. In this work we will discuss some preliminary results for the first 100 sols of Mars 2020 mission.Ítem Acceso Abierto Decline in Water Ice Abundance in the Martian Mesosphere during Aphelion(Europlanet, 2024-07-03) Toledo, D.; Rannou, P.; Apéstigue, V.; Rodríguez Veloso, Raúl; Arruego, I.; Martínez, Germán M.; Tamppari, L. K.; Munguira, A.; Lorenz, Ralph; Stcherbinine, Aurélien; Montmessin, F.; Sánchez Lavega, Agustín; Patel, P.; Viúdez Moreiras, Daniel; Hueso, R.; Bertrand, T.; Pla García, J.; Yela González, M.; De la Torre Juárez, M.; Rodríguez Manfredi, J. A.Clouds play a crucial role in the past and current climate of Mars. Cloud particles impact the planet's energy balance and atmospheric dynamics, as well as influence the vertical distribution of dust particles through dust scavenging. This process of dust scavenging by clouds has significant consequences for the planet's water cycle. For example, regions in the atmosphere with insufficient quantities of dust particles, or condensation nuclei, can inhibit the formation of H2O clouds, leading to the presence of water vapor in excess of saturation [1]. Recent observations made by the MEDA Radiation and Dust Sensor (RDS) [2,3] have shown a marked decline in mesospheric cloud activity (above 35-40 km) when Mars is near its aphelion (within the Aphelion Cloud Belt-ACB season), notably occurring during solar longitudes (Ls) between Ls 70° and 80° [4] (see Figure 1). In order to investigate the possible factors leading to this decrease in water ice abundance, we used a one-dimensional cloud microphysical model [5,6], which includes the processes of nucleation, condensation, coagulation, evaporation, precipitation, and coalescence, and where the vertical mixing is parameterized using an eddy diffusion profile (Keddy). Combining cloud microphysics modeling with ground-based (Mars 2020 and InSight) and orbital observations (TGO and MRO) of clouds, water vapor, and temperature, we will discuss in this presentation the main factors controlling the water abundance in the Martian mesosphere during the ACB season.Ítem Acceso Abierto Advance Dust Devil Detection with AI using Mars2020 MEDA instrument(Europlanet, 2024-07-03) Apéstigue, V.; Mohino, Inma; Gil, Roberto; Toledo, D.; Arruego, I.; Hueso, R.; Martínez, Germán M.; Lemmon, M. T.; Newman, C. E.; Genzer, María; De la Torre Juárez, M.; Rodríguez Manfredi, J. A.Mars’ dust cycle is a critical factor that drives the weather and climate of the planet. Airborne dust affects the energy balance that drives the atmospheric dynamic. Therefore, for studying the present-day and recent-past climate of Mars we need to observe and understand the different processes involved in the dust cycle. To this end, the Mars Environmental Dynamics Analyser (MEDA) station [1] includes a set of sensors capable of measuring the radiance fluxes, the wind direction and velocity, the pressure, and the humidity over the Martian surface. Combining these observations with radiative transfer (RT) simulations, airborne dust particles can be detected and characterized (optical depth, particle size, refractive index) along the day. The retrieval of these dust properties allows us to analyze dust storms or dust-lifting events, such as dust devils, on Mars [2][3]. Dust devils are thought to account for 50% of the total dust budget, and they represent a continuous source of lifted dust, active even outside the dust storms season. For these reasons, they have been proposed as the main mechanism able to sustain the ever-observed dust haze of the Martian atmosphere. Our radiative transfer simulations indicate that variations in the dust loading near the surface can be detected and characterized by MEDA radiance sensor RDS [4]. This study reanalyzes the dataset of dust devil detections obtained in [3] employing artificial intelligence techniques including anomaly detection based on autoencoders [5] and deep learning models [6] to analyze RDS and pressure sensor data. As we will show, preliminary results indicate that our AI models can successfully identify and characterize these phenomena with high accuracy. The final aim is to develop a powerful tool that can improve the database for the following sols of the mission, and subsequently extend its use for other atmospheric studies.Ítem Acceso Abierto The UMR: Uranus Multi-Experiment Radiometer for Haze and Clouds Characterization(Europlanet, 2024-07-03) Apéstigue, V.; Toledo, D.; Arruego, I.; Irwin, P.; Rannou, P.; Gonzalo Melchor, Alejandro; Martínez Oter, J.; Ceballos Cáceres, J.; Azcue, J.; Jiménez Martín, Juan José; De Mingo, J. R.; Serrano, F.; Nuñez, J.; Andrés, S.; Torres Redondo, J.; Martín Ortega, A.; Yela González, M.; Sorribas, M.; Sebastián, E.; Vázquez García de la Vega, D.; Espejo, S.; Ragel, A.; Arruego, I.The present understanding of Uranus and Neptune has been derived primarily from terrestrial observations and observations conducted using space telescopes. Furthermore, a brief flyby conducted by the Voyager 2 spacecraft nearly three decades ago has contributed to our knowledge of these celestial bodies. Recently, the Decadal Survey [1] has identified a mission to Uranus as a high-priority objective for NASA's space exploration program and its ongoing missions to Mars and Europa. The main mission study [2] establishes the scientific priorities for an orbiter, including analyzing the planet's bulk composition and internal structure, magnetic field, atmosphere circulation, rings, and satellite system. On the other hand, the mission includes a descent probe, whose primary mission is obtaining data on the atmospheric noble gas abundances, noble gas isotope ratios, and thermal structure using a mass spectrometer and a meteorological package. Investigation of the vertically distributed aerosols (hazes and clouds) and their microphysical and scattering properties is required to comprehend the thermal structure and dynamics of Uranus' atmosphere. These aerosols play a crucial role in the absorption and reflection of solar radiation, which directly influences the planet’s energy balance. In this work, we present a lightweight radiometer instrument [3] to be included in the descent probe for studying the aerosols in the first km of the Uranus’ atmosphere. The UMR, the Uranus Multi-experiment Radiometer, takes its heritage from previous missions for Mars exploration [4-6], where its technology, including mixed-signal ASICs radiation hardened by design [7-8], has demonstrated its endurance for extreme environments of operation, using limited resources in terms of power consumption, mass and volume footprints, and data budget. These characteristics make this instrument a valuable probe’s payload for studying Uranus’ atmosphere with a high scientific return. In this contribution, we will present the actual design of the instrument and the future perspective before a possible announcement of opportunity.Ítem Acceso Abierto First detection of visible-wavelength aurora on Mars(Europlanet, 2024-07-03) Wright Knutsen, Elise; McConnochie, Tim H.; Lemmon, M. T.; Tamppari, L. K.; Viet, Shayla; Cousin, Agnes; Wiens, Roger C.; Francis, R.; Donaldson, Chris; Lasue, J.; Forni, O.; Patel, P.; Schneider, Nick; Toledo, D.; Apéstigue, V.Auroras are hallmarks of the interaction between solar particles and the atmosphere of planets. Martian aurora was first discovered in 2005, since then, four different types have been identified: localized discreet aurora (Bertaux et al., 2005), global diffuse aurora (Schneider et al., 2015), dayside proton aurora (Deighan et al., 2018), and large-scale sinuous aurora (Lillis et al., 2022). All previous detections have been made in the UV from orbit. Here we present, from observations with the SuperCam and MastCam-Z instruments on the Mars 2020 Perseverance rover, the first detection of aurora from the Martian surface and the first detection of the green 557.7 nm atomic oxygen auroral emission on Mars. This is the same emission line that is familiar from terrestrial aurora. Charged particles accelerated by interplanetary coronal mass ejections (ICMEs) or solar flares are referred to as solar energetic particles (SEPs) (Reames, 1999). Diffuse aurora is strongly correlated with SEP events. ICME-accelerated SEPs travel nearly radially, as opposed to flare-accelerated SEPs which follow the Parker spiral. If the solar source region is identified, ICME-accelerated SEP events at Mars, and thus diffuse aurora, can be forecasted. The dynamic nature of rover planning and operations allows for a reactive observation strategy that takes advantage of such forecasts. We made several attempts, starting in May 2023, to react to SEP events and observe with the M2020 rover (Farley et al., 2020) instruments at times when we believed the likelihood of emission to be highest. Our fourth attempt, in March 2024, yielded the positive detection reported here.Ítem Restringido Nanostructured metamaterials for the thermal and electromagnetic isolation of cryostats(SPIE, 2024-08-26) Vivas, Laura G.; Ramos Somolinos, D.; Martín Rubio, C.; Rivelles García, Alejandro; Madueño Custodio, Laura; Ruiz Clavijo, Alejandra; Díaz, Alberto; Schneider, Marc; Plaza Gallardo, B.; Poyatos Martínez, D.; Del Hoyo, J. C.; Caballero Calero, Olga; Worgull, M.; Martín Iglesias, Santiago; Martín Vodopivec, B.; Maicas, M.; Navas, David; Martín González, Marisol; Sanz, RuyIn terms of thermal and electromagnetic isolation properties, Nanostructured Metamaterials may present important advantages compared to current employed materials. In this work, we present the synthesis routes and the preliminary characterization results of some metamaterials based on Poly-ether-ether-ketone and nanostructured anodic oxides, with low thermal conductivity, combined with Au nanocolumns and three-dimensional nanonetworks. The results reveals proper magnetic and electromagnetic properties and suggest their suitable use under vacuum and cryogenic conditions.Ítem Acceso Abierto Mars environmental networks through the MarsConnect microprobes(Europlanet, 2025-01-23) Arruego, I.; Apéstigue, V.; Bastide, L.; Azcue, J.; Gonzalo Melchor, Alejandro; Martínez Oter, J.; Caballero, N.; Liaño, G.; Torres, J.; González Guerrero, M.; Serrano, F.; De Mingo, J. R.; Rivas, J.; Andrés Santiuste, N.; Carrasco, I.; Fernández, M.; Reina, M.; Ruiz Carrasco, J. R.; Poyatos Martínez, D.; Scaccabarozzi, D.; Frövel, M.; De la Torre, M. A.; Martín, S.; Pedraza, R.In the last 15 years the Payloads Department of INTA has developed a variety of compact sensors for different Mars exploration missions. This includes a magnetometer (72 g), a dust sensor (35 g; with UC3M, Spain) and a radiometer (114 g) for the MetNet penetrator [1]; a radiometer (25 g optical head, 56 g processor) for DREAMS (Schiaparelli) [2], [3]; a radiometer plus camera (1 kg) for MEDA on Perseverance [4], [5]; a 110 g dust sensor (with UC3M, Spain) [6] and a radiometer plus spectrometer (180 g) for the METEO package [7] on Kazachock lander (ExoMars’22) and a 0.5 kg nephelometer (with INAF and Politecnico di Milano, Italy) [8] for the Dust Complex on the same lander. Equally miniaturized sensors exist for the measurement of the most relevant environmental variables, such as radiative balance, air temperature, wind, humidity, pressure, dust saltation, electric field, etc. with enough flight heritage (or technology readiness level) on the same sensors’ suites on Perseverance and ExoMars, as well as Insight or Curiosity before [9]. In summary, a large portfolio of miniature sensors for environmental research is available at present. However, a qualitative leap on (in-situ) Mars climate science will only happen through the deployment of networks of environmental stations throughout large areas of the planet. Given the relevance of these measurement not only from a scientific point of view but also because of their importance for future human missions to Mars, this is an objective considered in several Mars exploration roadmaps such as ESA’s Terrae Novae 2030+ [10]. With this aim, we propose a microprobe named MarsConnect. It consists of a 10-12 kg probe with a rigid, deployable aeroshell/TPS and a 5-6 kg impactor/penetrator carrying up to 1 kg of environmental sensors. Many of these probes could be launched to Mars with a single carrier, to deploy meteorological networks. This works inherits different concepts from previous similar proposals, very specially MetNet and MiniPINS [11], but simplifying even more the EDL concept and reducing the mass, at the expense of an increased impact speed. The probe’s aeroshell is divided into a backshell and two halves of a frontshield that are opened in the low supersonic regime to drop the penetrator. This one is equipped with a drag-skirt that provides some braking and increases stability. The expected impact speed, highly dependent on the atmospheric density profile, entry conditions and landing altitude, ranges from less than 100 to 140 m/s. The whole system is designed to be compatible with a wide range of scenarios and landing sites and is sized to endure more than one Martian year operating on the planet’s surface.Ítem Acceso Abierto Turbulence statistics of terrestrial Mars-analog and Martian dust devils(EGU General Assembly, 2025-01-16) Karatekin, Özgür; Apéstigue, V.; Toledo, D.; Arruego, I.; Franchi, Fulvio; Martínez, Germán M.; Berk Senel, CemConvective instabilities in the lowermost part of the atmosphere, so called the planetary boundary layer, can lead to the formation of convective vortices and form dust devils both on Earth and Mars. We performed mesoscale simulations for a Mars-analog terrestrial site, Makgadikgadi Pan - Botswana [1,2], where a state-of-the art field campaign was conducted to investigate the terrestrial dust devils, and the InSight landing site [3] using WRF/MarsWRF models [4,5]. We then combined our atmospheric modeling with in-situ observations of wind and pressure to perform a comparative boundary-layer meteorology study. We focused on the length and time of scales of turbulence and investigated the turbulent spectrum.Ítem Acceso Abierto Vortices and Dust Devils on Jezero Crater, Mars: inner thermal structure and dependence on surface properties(EGU General Assembly, 2024-05-16) Hueso, R.; Munguira, A.; Newman, C. E.; Martínez, Germán M.; Sánchez Lavega, Agustín; Del Río Gaztelurrutia, T.; Toledo, D.; Apéstigue, V.; Arruego, I.; Pla García, J.; Lemmon, M. T.; Lorenz, Ralph; Vicente Retortillo, Álvaro; Navarro López, Sara; Stott, Alexander; Murdoch, N.; Gillier, M.; De la Torre Juárez, M.; Rodríguez Manfredi, J. A.Ítem Acceso Abierto Generic Entry Probe Program (GEPP) – an international initiative promoting the development of European descent modules dedicated to the in situ(EGU General Assembly, 2024-05-13) Mousis, O.; Ambrosi, R.; André, N.; Andrews, J.; Apéstigue, V.; Atkinson, D.; Arruego, I.; Blanc, M.; Boithias, H.; Bolton, S.; Bousquet, P.; Canup, R.; Cavalié, T.; Freeman, A.; Faye, F.; Ferri, F.; Glein, C.; Guelhan, A.; Hartogh, P.; Loehle, S.; Hue, V.; Lebreton, J. P.; Lemaistre, S.; Mooij, E.; Pichon, T.; Pinaud, G.; Steuer, D.; Toledo, D.; Rauer, H.; Vorburger, A.; Wurz, P.The international consortium GEPP has been set to conceptualize probe designs with appropriate payloads that would remain within the typical budget allocated for ESA M-class missions (currently 500 M€). The aims of the consortium are i) to conceptualize a line of generic planetary entry probes that could be targeted to the giant planets with very few modifications, ii) to make the international science community, ESA and its member states, conscious that there is an opportunity to supply a series of entry probes as part of future international collaborations, for example as part of the future NASA flagship mission towards Uranus (Uranus Orbiter Probe) or to any future NASA-led mission to the outer planets for an affordable budget, and iii) to demonstrate that an M-class budget could even fund several entry probes with well-prioritized science objectives. The model payload capabilities of each concept will be defined according to a carefully-designed science traceability matrix. Two extreme concepts shall be investigated by the GEPP Consortium, namely a highly capable parachute-descent probe including a typical payload of 30 kg of scientific instruments down to 10 bars, and a smaller parachute-descent probe designed to address top priority science objectives with selected key measurements that would address the ESA Cosmic Vision 2050 science objectives. This presentation will detail the scientific objectives for each entry probe design, as well as the content, organization and planning of the study, which is assumed to be completed by the end of 2025.Ítem Restringido Magnetic study of Cobalt three dimensional nanonetworks: First Order Reversal Curves, hysteresis loops and first magnetization curves(Institute of Electrical and Electronics Engineers, 2023-05-19) Ruiz Clavijo, Alejandra; Caballero Calero, Olga; Navas, David; Martín Rubio, C.; Sanz, Ruy; Martín González, MarisolThree-Dimensional (3D) magnetic nanostructures will be the next generation of functional magnetic nanostructured metamaterials. In this work, we report some of our recent results on the synthesis and characterization of different interconnected Co nanowires forming a dense and ordered magnetic system: Co 3D Nanowire Networks (3DNN). The 3DNN presents anisotropic magnetic responses. We used first magnetization curves, hysteresis loops, and first order reversal curves techniques to characterize the systems, which provide information about the key magnetic properties of the 3D nanostructure.Ítem Restringido Magnetic interactions in ordered cobalt three-dimensional nanonetworks(EMS, 2023-08-27) Ruiz Clavijo, Alejandra; Caballero Calero, Olga; Navas, David; Vivas, Laura G.; Martín Rubio, C.; Sanz, Ruy; Martín González, Marisol; Agencia Estatal de Investigación (AEI)"Three-Dimensional (3D) magnetic nanostructures allow the generation and control of new effects able to give rise to the next generation of functional magnetic nanostructured metamaterials and devices[1]. This work reports the results on the synthesis and characterization of different interconnected Co nanowires forming a dense and ordered magnetic system: Co 3D Nanowire Networks (3DNN). These nanostructures were synthesized by the electrodeposition of Co in 3D ordered porous alumina templates [2] [3] [4]. The route allows to control the order and some geometric features compared to other synthesis approaches [1]. The resulting 3DNN consists of hexagonal ordered nanowires with an inter-wire distance of 65 nm and 50 nm in diameter. These nanowires are interconnected with a net of perpendicular or transversal nanowires (TNW) of ≈ 30 nm in diameter. Meanwhile the TNW are distributed in levels with a well defined distance between them of 550 nm. The magnetic characterization consisted in hysteresis loops, first magnetization curves and first order reversal curves (FORC) at 0º (in-plane, IP) 30º, 60º and 90º (out of plane, OOP) from perpendicular NW main axis. 1.D. Bhattacharya, et al. Nano Lett. (2022), 22, 24, 10010–10017. 2.J. Martín, et. al., Nat. Commun. 5, (2014) 5130. 3.A. Ruiz-Clavijo, et al. Phys. Status Solidi RRL, 13 (2019), 1900263. 4.A. Ruiz-Clavijo, et al., Adv. Electron. Mater. 8, (2022) 2200342"Ítem Restringido RF & MW Characterization of Advanced Materials with High Accuracy for Space Applications(European Space Agency (ESA), 2023-05-12) Ramos Somolinos, D.; Plaza Gallardo, B.; Cidrás Estévez, J.; Poyatos Martínez, D.; Hernández Gómez, Daniel; Instituto Nacional de Técnica Aeroespacial (INTA); Ministerio de Ciencia e Innovación (MICINN)Electromagnetic characterization is a fundamental piece when designing systems that will be present in space missions. These systems must function correctly immersed into the electromagnetic environment they are going to find, preventing electromagnetic interference (EMI) from affecting their characteristics and properties [1]. In addition to the study of the system itself, it is equally important to know the behaviour of the materials with which these systems will be built in the presence of electromagnetic radiation, so that their viability can be established [2] [3]. On the other hand, taking into account the communications in space, the characterization of antennas is essential during their design phase. All these points are taken into account in the development of the project Large European Antenna (LEA) [4] [5], which is focused on how to build powerful antennas for specific Earth observation, telecommunications, etc., that can automatically self-deploy in space. This type of antennas is commonly formed by complex knitted meshes of gold-plated metals [6] [7] [8]. For these structures there are two important issues regarding radiofrequency (RF) characterization which are its reflectance and transmittance properties. In this case, it is important to ensure that the RF behaviour of the mesh surface is well enough to guarantee that the final reflector accomplishes the RF specifications of the antenna. The following communication will present two test benches (POLYBENCH and mmW-BENCH) that allow to electromagnetically characterize materials with high accuracy from 2.6 GHz to 110 GHz; both test benches fully designed and developed by the National Institute of Aerospace Technology (INTA) and both are based in the free space method, which allows measurements in a wide range of frequencies with great precision and with relative simplicity and speed [9]. The tests carried out focus on the measurement of the reflection and transmission coefficients of different test samples, in two orthogonal polarizations and on different points of each sample, with an accuracy below ± 0.1dB in amplitude. This paper is structured as follows: first an explanation of the test benches used to carry out the measurements is provided; then, the procedure of the measurements is explained; after that, an analysis of the measurement errors is given and finally some conclusions are presented.Ítem Acceso Abierto Caracterización electromagnética de urnas de protección planetaria en cámara anecoica biestática para ensayos de EMC(Universidad de Valencia, 2023-11-23) Jimenez Lorenzo, María; Plaza Gallardo, B.; Ramos Somolinos, D.; Poyatos Martínez, D.; Moragrega Langton, María; Instituto Nacional de Técnica Aeroespacial (INTA); Ministerio de Ciencia e Innovación (MICINN)Ítem Acceso Abierto Efecto de la saturación de los materiales magnéticos en el filtrado de interferencias(Universidad de Valencia, 2023-11-21) Morales Blanco, C.; Moragrega Langton, María; López Sanz, Daniel; Instituto Nacional de Técnica Aeroespacial (INTA); Ministerio de Ciencia e Innovación (MICINN)En electrónica, el uso de bobinados con núcleos de ferrita está cada vez más extendido, para filtrar y proteger equipos electrónicos frente a interferencias electromagnéticas (EMI). Por ello, es de gran importancia el conocimiento de las prestaciones de dichos núcleos. Su uso frente a niveles elevados de tensión puede hacer que su comportamiento se aleje del régimen lineal a uno no lineal, conociéndose también como estado de saturación en materiales magnéticos. En estas condiciones, se modifican las características que se esperan de los bobinados destinados a la filtración de interferencias, eso es, impedir el paso de señales interferentes al interior de los equipos electrónicos, ofreciendo alta impedancia en las líneas de alimentación y señal. En esta ponencia, se presentarán los resultados obtenidos en el estudio de este fenómeno. Se demostrará inyectando pulsos de alta energía de diferente amplitud a una bobina, hasta observar comportamientos no lineales que se podrían identificar con la saturación de los materiales magnéticos. Este estudio abre la puerta a futuras líneas de investigación sobre el comportamiento de materiales magnéticos frente a la inyección de altas energías.Ítem Restringido Electrical performance results of multi-junction space solar cells under high temperature high intensity environmental conditions(IEEE Aerospace and Electronic Systems Society 13th European Space Power Conference 2023, 2023-10-02) Martínez de Olcoz, A.; Jüngst, G.; Barber, Christopher; Gras, Ana; Baur, CarstenMissions close to the sun such as BepiColombo or Venus Express always require dedicated testing of solar cells since they operate under non-standard conditions, i.e., High Temperature High Intensity (HTHI). The next mission that falls into the category of HTHI ESA mission is EnVision to Venus, which – in case it will be adopted – is planned to launch in the early 2030s. The space solar cells destined for the PV solar generator are expected to operate at sun intensities of 2 suns and most probably in the temperature range of 130°C-140°C. At INTA-SPASOLAB the temperature coefficient of two cell candidates for the PV solar generator of the ESA EnVision mission, which are a quadruple junction and a triple junction solar cell, have already been determined at 1 sc-AM0 within the range from +25ºC to +100ºC.Ítem Restringido Assessment of Spectrally Matched Cells(AESS, 2023-10-02) Gras, Ana; Barber, Christopher; Baur, Carsten; Instituto Nacional de Técnica Aeroespacial (INTA)The spectral matching criterion for solar cells is crucial for photovoltaic (PV) measurements under simulated sunlight because it helps reducing the uncertainty due to the spectral mismatch correction. It is common practice in both terrestrial and space PV communities to identify spectrally matched cells as those having spectral responsivities identical or at least very similar to each other. A quantitative definition and evaluation of spectrally matched cells is made in this document.
