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The Scanning Habitable Environments with Raman and Luminescence for Organics and Chemicals (SHERLOC) instrument onboard the Mars 2020 Perseverance rover detected so far some of the most intense fluorescence signals in association with sulfates analyzing abraded patches of rocks at Jezero crater, Mars. To assess the plausibility of an organic origin of these signals, it is key to understand if organics can survive exposure to ambient Martian UV after exposure by the Perseverance abrasion tool and prior to analysis by SHERLOC. In this work, we investigated the stability of organo-sulfate assemblages under Martian-like UV irradiation and we observed that the spectroscopic features of phthalic and mellitic acid embedded into hydrated magnesium sulfate do not change for UV exposures corresponding to at least 48 Martian sols and, thus, should still be detectable in fluorescence when the SHERLOC analysis takes place, thanks to the photoprotective properties of magnesium sulfate. In addition, different photoproduct bands diagnostic of the parent carboxylic acid molecules could be observed. The photoprotective behavior of hydrated magnesium sulfate corroborates the hypothesis that sulfates might have played a key role in the preservation of organics on Mars, and that the fluorescence signals detected by SHERLOC in association with sulfates could potentially arise from organic compounds., Tis research was supported by the Italian Space Agency (ASI) through the ASI/INAF agreement no. 2023-3-HH, and by European Union—Next Generation EU through the PRIN MUR 2022 “Experimental and computational analog studies to support identifcation of organics on Mars by the NASA Mars 2020 Perseverance rover”. In addition, T.F. was supported by INAF through Mini Grant Ricerca Fondamentale INAF 2022. I.P., J.A. and J.M.M. acknowledge the support of the PAMMAT project funded by the Spanish Agency for Research, Contract No. PID2022-142750OB-I00. E.A.C. and D.M.A. thank the Natural Sciences and Engineering Research Council Grant No. RGPIN0-2023-03413 and Canadian Space Agency Grant No. 22EXPCOI4 for supporting this project. M.B. acknowledge the COST Action CA21101 “COSY–Confned molecular systems: from a new generation of materials to the stars”. G.P. acknowledge support from Centre National d’Etudes Spatiales (CNES). A. V.-R. is supported by the Spanish Ministry of Science and Innovation (MCIN)/State Agency of Research (AEI) project PID2021-126719OB-C41, funded by MCIN/AEI/10.13039/501100011033/FEDER, UE.

The Scanning Habitable Environments with Raman and Luminescence for Organics and Chemicals (SHERLOC) instrument onboard the Mars 2020 Perseverance rover detected so far some of the most intense fluorescence signals in association with sulfates analyzing abraded patches of rocks at Jezero crater, Mars. To assess the plausibility of an organic origin of these signals, it is key to understand if organics can survive exposure to ambient Martian UV after exposure by the Perseverance abrasion tool and prior to analysis by SHERLOC. In this work, we investigated the stability of organo-sulfate assemblages under Martian-like UV irradiation and we observed that the spectroscopic features of phthalic and mellitic acid embedded into hydrated magnesium sulfate do not change for UV exposures corresponding to at least 48 Martian sols and, thus, should still be detectable in fluorescence when the SHERLOC analysis takes place, thanks to the photoprotective properties of magnesium sulfate. In addition, different photoproduct bands diagnostic of the parent carboxylic acid molecules could be observed. The photoprotective behavior of hydrated magnesium sulfate corroborates the hypothesis that sulfates might have played a key role in the preservation of organics on Mars, and that the fluorescence signals detected by SHERLOC in association with sulfates could potentially arise from organic compounds., Tis research was supported by the Italian Space Agency (ASI) through the ASI/INAF agreement no. 2023-3-HH, and by European Union—Next Generation EU through the PRIN MUR 2022 “Experimental and computational analog studies to support identifcation of organics on Mars by the NASA Mars 2020 Perseverance rover”. In addition, T.F. was supported by INAF through Mini Grant Ricerca Fondamentale INAF 2022. I.P., J.A. and J.M.M. acknowledge the support of the PAMMAT project funded by the Spanish Agency for Research, Contract No. PID2022-142750OB-I00. E.A.C. and D.M.A. thank the Natural Sciences and Engineering Research Council Grant No. RGPIN0-2023-03413 and Canadian Space Agency Grant No. 22EXPCOI4 for supporting this project. M.B. acknowledge the COST Action CA21101 “COSY–Confned molecular systems: from a new generation of materials to the stars”. G.P. acknowledge support from Centre National d’Etudes Spatiales (CNES). A. V.-R. is supported by the Spanish Ministry of Science and Innovation (MCIN)/State Agency of Research (AEI) project PID2021-126719OB-C41, funded by MCIN/AEI/10.13039/501100011033/FEDER, UE.

The Mars Science Laboratory Curiosity rover has monitored the Martian environment in Gale crater since landing in 2012. This study reports the record of optical depth derived from visible and near-infrared images of the Sun. Aerosol optical depth, which is mostly due to dust but also includes ice, dominates the record, with gas optical depth too small to measure. The optical depth record includes the effects of regional dust storms and one planet-encircling dust event, showing the expected peaks during southern spring and summer and relatively lower and more stable optical depth in fall and winter. The measurements show that there is a seasonally varying diurnal change in dust load, with the optical depth peaking in the morning during southern spring and summer, correlated with thermotidal pressure changes. However, there was no systematic diurnal change during autumn and winter, except after one regional storm. There were indications that the dust was relatively enhanced at high altitudes during high-optical-depth periods and that high-altitude ice was significant during winter. The observations did not provide much information about particle size or composition, but they were consistent with a smaller particle size after aphelion (in southern winter). No scattering halos were seen in associated sky images, even when there was visual evidence of ice hazes or clouds, which suggests small or amorphous ice particles. Unexpectedly, the measurement campaign revealed that the cameras collected saltating sand in their sunshades 1.97 m above the surface. As a result, the measurement strategy had to be adjusted to avoid high-elevation imaging to avoid sand covering the optics.

In the search for life in our Solar System, Mars remains a promising target based on its proximity and similarity to Earth. When Mars transitioned from a warmer, wetter climate to its current dry and freezing conditions, any putative extant life probably retreated into habitable refugia such as the subsurface or the interior of rocks. Terrestrial cryptoendolithic microorganisms (i.e., those inhabiting rock interiors) thus represent possible modern-day Mars analogs, particularly those from the hyperarid McMurdo Dry Valleys in Antarctica. As DNA is a strong definitive biosignature, given that there is no known abiotic chemistry that can polymerize nucleobases, we investigated DNA detection with MinION sequencing in Antarctic cryptoendoliths after an ∼58-sol exposure in MARTE, a Mars environmental chamber capable of simulating martian temperature, pressure, humidity, ultraviolet (UV) radiation, and atmospheric composition, in conjunction with protein and lipid detection. The MARTE conditions resulted in changes in community composition and DNA, proteins, and cell membrane-derived lipids remained detectable postexposure. Of the multitude of extreme environmental conditions on Mars, UV radiation (specifically UVC) is the most destructive to both cells and DNA. As such, we further investigated if a UVC exposure corresponding to ∼278 martian years would impede DNA detection via MinION sequencing. The MinION was able to successfully detect and sequence DNA after this UVC radiation exposure, suggesting its utility for life detection in future astrobiology missions focused on finding relatively recently exposed biomarkers inside possible martian refugia.

The pressure sensors on Mars rover Perseverance measure the pressure field in the Jezero crater on regular hourly basis starting in sol 15 after landing. The present study extends up to sol 460 encompassing the range of solar longitudes from Ls 13{\deg} - 241{\deg} (Martian Year (MY) 36). The data show the changing daily pressure cycle, the sol-to-sol seasonal evolution of the mean pressure field driven by the CO2 sublimation and deposition cycle at the poles, the characterization of up to six components of the atmospheric tides and their relationship to dust content in the atmosphere. They also show the presence of wave disturbances with periods 2-5 sols, exploring their baroclinic nature, short period oscillations (mainly at night-time) in the range 8-24 minutes that we interpret as internal gravity waves, transient pressure drops with duration 1-150 s produced by vortices, and rapid turbulent fluctuations. We also analyze the effects on pressure measurements produced by a regional dust storm over Jezero at Ls 155{\deg}.

The Mars Environmental Dynamics Analyzer instrument, on board NASA's Mars 2020 Perseverance rover, includes a number of sensors to characterize the Martian atmosphere. One of these sensors is the Radiation and Dust Sensor (RDS) that measures the solar irradiance at different wavelengths and geometries. We analyzed the RDS observations made during twilight for the period between sol 71 and 492 of the mission (Ls 39°–262°, Mars Year 36) to characterize the clouds over the Perseverance rover site. Using the ratio between the irradiance at zenith at 450 and 750 nm, we inferred that the main constituent of the detected high-altitude aerosol layers was ice from Ls = 39°–150° (cloudy period), and dust from Ls 150°–262°. A total of 161 twilights were analyzed in the cloudy period using a radiative transfer code and we found: (a) signatures of clouds/hazes in the signals in 58% of the twilights; (b) most of the clouds had altitudes between 40 and 50 km, suggesting water ice composition, and had particle sizes between 0.6 and 2 µm; (c) the cloud activity at sunrise is slightly higher that at sunset, likely due to the differences in temperature; (d) the time period with more cloud detections and with the greatest cloud opacities is during Ls 120°–150°; and (e) a notable decrease in the cloud activity around aphelion, along with lower cloud altitudes and opacities. This decrease in cloud activity indicates lower concentrations of water vapor or cloud condensation nuclei (dust) around this period in the Martian mesosphere.

The Mars Science Laboratory Curiosity rover has monitored the Martian environment in Gale crater since landing in 2012. This study reports the record of optical depth derived from visible and near-infrared images of the Sun. Aerosol optical depth, which is mostly due to dust but also includes ice, dominates the record, with gas optical depth too small to measure. The optical depth record includes the effects of regional dust storms and one planet-encircling dust event, showing the expected peaks during southern spring and summer and relatively lower and more stable optical depth in fall and winter. The measurements show that there is a seasonally varying diurnal change in dust load, with the optical depth peaking in the morning during southern spring and summer, correlated with thermotidal pressure changes. However, there was no systematic diurnal change during autumn and winter, except after one regional storm. There were indications that the dust was relatively enhanced at high altitudes during high-optical-depth periods and that high-altitude ice was significant during winter. The observations did not provide much information about particle size or composition, but they were consistent with a smaller particle size after aphelion (in southern winter). No scattering halos were seen in associated sky images, even when there was visual evidence of ice hazes or clouds, which suggests small or amorphous ice particles. Unexpectedly, the measurement campaign revealed that the cameras collected saltating sand in their sunshades 1.97 m above the surface. As a result, the measurement strategy had to be adjusted to avoid high-elevation imaging to avoid sand covering the optics.

The pressure sensors on Mars rover Perseverance measure the pressure field in the Jezero crater on regular hourly basis starting in sol 15 after landing. The present study extends up to sol 460 encompassing the range of solar longitudes from Ls ∼ 13°–241° (Martian Year (MY) 36). The data show the changing daily pressure cycle, the sol-to-sol seasonal evolution of the mean pressure field driven by the CO2 sublimation and deposition cycle at the poles, the characterization of up to six components of the atmospheric tides and their relationship to dust content in the atmosphere. They also show the presence of wave disturbances with periods 2–5 sols, exploring their baroclinic nature, short period oscillations (mainly at night-time) in the range 8–24 min that we interpret as internal gravity waves, transient pressure drops with duration ∼1–150 s produced by vortices, and rapid turbulent fluctuations. We also analyze the effects on pressure measurements produced by a regional dust storm over Jezero at Ls ∼ 155°.

The Mars Environmental Dynamics Analyzer instrument on Mars 2020 has five Atmospheric Temperature Sensors at two altitudes (0.84 and 1.45 m) plus a Thermal InfraRed Sensor that measures temperatures on the surface and at ∼40 m. We analyze the measurements from these sensors to describe the evolution of temperatures in Jezero up to mission sol 400 (solar longitude LS = 13°–203°). The diurnal thermal cycle is characterized by a daytime convective period and a nocturnal stable atmosphere with a variable thermal inversion. We find a linear relationship between the daytime temperature fluctuations and the vertical thermal gradient with temperature fluctuations that peak at noon with typical values of 2.5 K at 1.45 m. In the late afternoon (∼17:00 Local True Solar Time), the atmosphere becomes vertically isothermal with vanishing fluctuations. We observe very small seasonal changes in air temperatures during the period analyzed. This is related to small changes in solar irradiation and dust opacity. However, we find significant changes in surface temperatures that are related to the variety of thermal inertias of the terrains explored along the traverse of Perseverance. These changes strongly influence the vertical thermal gradient, breaking the nighttime thermal inversion over terrains of high thermal inertia. We explore possible detections of atmospheric tides on near-surface temperatures and we examine variations in temperatures over timescales of a few sols that could be indicative of atmospheric waves affecting near-surface temperatures. We also discuss temperatures during a regional dust storm at LS = 153°–156° that simultaneously warmed the near surface atmosphere while cooling the surface.

NASA’s Perseverance rover’s Mars Environmental Dynamics Analyzer is collecting data at Jezero crater, characterizing the physical processes in the lowest layer of the Martian atmosphere. Here we present measurements from the instrument’s first 250 sols of operation, revealing a spatially and temporally variable meteorology at Jezero. We find that temperature measurements at four heights capture the response of the atmospheric surface layer to multiple phenomena. We observe the transition from a stable night-time thermal inversion to a daytime, highly turbulent convective regime, with large vertical thermal gradients. Measurement of multiple daily optical depths suggests aerosol concentrations are higher in the morning than in the afternoon. Measured wind patterns are driven mainly by local topography, with a small contribution from regional winds. Daily and seasonal variability of relative humidity shows a complex hydrologic cycle. These observations suggest that changes in some local surface properties, such as surface albedo and thermal inertia, play an influential role. On a larger scale, surface pressure measurements show typical signatures of gravity waves and baroclinic eddies in a part of the seasonal cycle previously characterized as low wave activity. These observations, both combined and simultaneous, unveil the diversity of processes driving change on today’s Martian surface at Jezero crater.

Dust devils (convective vortices loaded with dust) are common at the surface of Mars, particularly at Jezero crater, the landing site of the Perseverance rover. They are indicators of atmospheric turbulence and are an important lifting mechanism for the Martian dust cycle. Improving our understanding of dust lifting and atmospheric transport is key for accurate simulation of the dust cycle and for the prediction of dust storms, in addition to being important for future space exploration as grain impacts are implicated in the degradation of hardware on the surface of Mars. Here we describe the sound of a Martian dust devil as recorded by the SuperCam instrument on the Perseverance rover. The dust devil encounter was also simultaneously imaged by the Perseverance rover's Navigation Camera and observed by several sensors in the Mars Environmental Dynamics Analyzer instrument. Combining these unique multi-sensorial data with modelling, we show that the dust devil was around 25m large, at least 118m tall, and passed directly over the rover travelling at approximately 5ms-1. Acoustic signals of grain impacts recorded during the vortex encounter provide quantitative information about the number density of particles in the vortex. The sound of a Martian dust devil was inaccessible until SuperCam microphone recordings. This chance dust devil encounter demonstrates the potential of acoustic data for resolving the rapid wind structure of the Martian atmosphere and for directly quantifying wind-blown grain fluxes on Mars.

Despite the importance of sand and dust to Mars geomorphology, weather, and exploration, the processes that move sand and that raise dust to maintain Mars' ubiquitous dust haze and to produce dust storms have not been well quantified in situ, with missions lacking either the necessary sensors or a sufficiently active aeolian environment. Perseverance rover's novel environmental sensors and Jezero crater's dusty environment remedy this. In Perseverance's first 216 sols, four convective vortices raised dust locally, while, on average, four passed the rover daily, over 25% of which were significantly dusty ("dust devils"). More rarely, dust lifting by nonvortex wind gusts was produced by daytime convection cells advected over the crater by strong regional daytime upslope winds, which also control aeolian surface features. One such event covered 10 times more area than the largest dust devil, suggesting that dust devils and wind gusts could raise equal amounts of dust under nonstorm conditions.

NASA's Mars 2020 (M2020) rover mission includes a suite of sensors to monitor current environmental conditions near the surface of Mars and to constrain bulk aerosol properties from changes in atmospheric radiation at the surface. The Mars Environmental Dynamics Analyzer (MEDA) consists of a set of meteorological sensors including wind sensor, a barometer, a relative humidity sensor, a set of 5 thermocouples to measure atmospheric temperature at ∼1.5 m and ∼0.5 m above the surface, a set of thermopiles to characterize the thermal IR brightness temperatures of the surface and the lower atmosphere. MEDA adds a radiation and dust sensor to monitor the optical atmospheric properties that can be used to infer bulk aerosol physical properties such as particle size distribution, non-sphericity, and concentration. The MEDA package and its scientific purpose are described in this document as well as how it responded to the calibration tests and how it helps prepare for the human exploration of Mars. A comparison is also presented to previous environmental monitoring payloads landed on Mars on the Viking, Pathfinder, Phoenix, MSL, and InSight spacecraft.

NASA’s Mars 2020 (M2020) rover mission includes a suite of sensors to monitor current environmental conditions near the surface of Mars and to constrain bulk aerosol properties from changes in atmospheric radiation at the surface. The Mars Environmental Dynamics Analyzer (MEDA) consists of a set of meteorological sensors including wind sensor, a barometer, a relative humidity sensor, a set of 5 thermocouples to measure atmospheric temperature at ∼1.5 m and ∼0.5 m above the surface, a set of thermopiles to characterize the thermal IR brightness temperatures of the surface and the lower atmosphere. MEDA adds a radiation and dust sensor to monitor the optical atmospheric properties that can be used to infer bulk aerosol physical properties such as particle size distribution, non-sphericity, and concentration. The MEDA package and its scientific purpose are described in this document as well as how it responded to the calibration tests and how it helps prepare for the human exploration of Mars. A comparison is also presented to previous environmental monitoring payloads landed on Mars on the Viking, Pathfinder, Phoenix, MSL, and InSight spacecraft.

The Mars Regional Atmospheric Modeling System (MRAMS) and a nested simulation of the Mars Weather Research and Forecasting model (MarsWRF) are used to predict the local meteorological conditions at the Mars 2020 Perseverance rover landing site inside Jezero crater (Mars). These predictions are complemented with the COmplutense and MIchigan MArs Radiative Transfer model (COMIMART) and with the local Single Column Model (SCM) to further refine predictions of radiative forcing and the water cycle respectively. The primary objective is to facilitate interpretation of the meteorological measurements to be obtained by the Mars Environmental Dynamics Analyzer (MEDA) aboard the rover, but also to provide predictions of the meteorological phenomena and seasonal changes that might impact operations, from both a risk perspective and from the perspective of being better prepared to make certain measurements. A full diurnal cycle at four different seasons (L 0 , 90 , 180 , and 270 ) is investigated. Air and ground temperatures, pressure, wind speed and direction, surface radiative fluxes and moisture data are modeled. The good agreement between observations and modeling in prior works [Pla-Garcia et al. in Icarus 280:103–113, 2016; Newman et al. in Icarus 291:203–231, 2017; Vicente-Retortillo et al. in Sci. Rep. 8(1):1–8, 2018; Savijärvi et al. in Icarus, 2020] provides confidence in utilizing these models results to predict the meteorological environment at Mars 2020 Perseverance rover landing site inside Jezero crater. The data returned by MEDA will determine the extent to which this confidence was justified.

Mars Science Laboratory Curiosity rover observations of the 2018/Mars year 34 global/planet-encircling dust storm represent the first in situ measurements of a global dust storm with dedicated meteorological sensors since the Viking Landers. The Mars Science Laboratory team planned and executed a science campaign lasting approximately 100 Martian sols to study the storm involving an enhanced cadence of environmental monitoring using the rover's meteorological sensors, cameras, and spectrometers. Mast Camera 880-nm optical depth reached 8.5, and Rover Environmental Monitoring Station measurements indicated a 97% reduction in incident total ultraviolet solar radiation at the surface, 30K reduction in diurnal range of air temperature, and an increase in the semidiurnal pressure tide amplitude to 40 Pa. No active dust-lifting sites were detected within Gale Crater, and global and local atmospheric dynamics were drastically altered during the storm. This work presents an overview of the mission's storm observations and initial results.

The Sample Analysis at Mars (SAM) instrument onboard the Mars Science Laboratory Curiosity rover measures the chemical composition of major atmospheric species (CO2, N2, 40Ar, O2, and CO) through a dedicated atmospheric inlet. We report here measurements of volume mixing ratios in Gale Crater using the SAM quadrupole mass spectrometer, obtained over a period of nearly 5 years (3 Mars years) from landing. The observation period spans the northern summer of MY 31 and solar longitude (LS) of 175° through spring of MY 34, LS = 12°. This work expands upon prior reports of the mixing ratios measured by SAM QMS in the first 105 sols of the mission. The SAM QMS atmospheric measurements were taken periodically, with a cumulative coverage of four or five experiments per season on Mars. Major observations include the seasonal cycle of CO2, N2, and Ar, which lags approximately 20¿40° of LS behind the pressure cycle driven by CO2 condensation and sublimation from the winter poles. This seasonal cycle indicates that transport occurs on faster timescales than mixing. The mixing ratio of O2 shows significant seasonal and interannual variability, suggesting an unknown atmospheric or surface process at work. The O2 measurements are compared to several parameters, including dust optical depth and trace CH4 measurements by Curiosity. We derive annual mean volume mixing ratios for the atmosphere in Gale Crater: CO2 = 0.951 (±0.003), N2 = 0.0259 (±0.0006), 40Ar = 0.0194 (±0.0004), O2 = 1.61 (±0.09) x 10-3, and CO = 5.8 (±0.8) x 10-4. ©2019. The Authors.

We analyze 10 years of Mars Express total electron content (TEC) data from the Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) instrument. We describe the spatial, seasonal, and solar cycle behavior of the Martian TEC. Due to orbit evolution, data come mainly from the evening, dusk terminator and postdusk nightside. The annual TEC profile shows a peak at Ls = 25–75° which is not related to the solar irradiance variation but instead coincides with an increase in the thermospheric density, possibly linked with variations in the surface pressure produced by atmospheric cycles such as the CO or water cycles. With the help of numerical modeling, we explore the contribution of the ion species to the TEC and the coupling between the thermosphere and ionosphere. These are the first observations which show that the TEC is a useful parameter, routinely measured by Mars Express, of the dynamics of the lower-upper atmospheric coupling and can be used as tracer for the behavior of the thermosphere.©2018. The Authors.

Variable levels of methane in the martian atmosphere have eluded explanation partly because the measurements are not repeatable in time or location.We report in situ measurements at Gale crater made over a 5-year period by the Tunable Laser Spectrometer on the Curiosity rover.The background levels of methane have a mean value 0.41 ± 0.16 parts per billion by volume (ppbv) (95% confidence interval) and exhibit a strong, repeatable seasonal variation (0.24 to 0.65 ppbv).This variation is greater than that predicted from either ultraviolet degradation of impact-delivered organics on the surface or from the annual surface pressure cycle.The large seasonal variation in the background and occurrences of higher temporary spikes (∼7 ppbv) are consistent with small localized sources of methane released from martian surface or subsurface reservoirs.

El estudio del entorno radiativo en la superficie marciana es fundamental para la comprensión y para una mejor caracterización de los procesos físicos de la atmósfera y el clima del planeta, así como para determinar el impacto biológico de la radiación ultravioleta. Estos dos objetivos son prioritarios en las misiones actuales y futuras a Marte debido a sus implicaciones en la preparación para la exploración humana del planeta. Debido a la importancia de la radiación solar, es necesario poder contar con modelos de transferencia radiativa precisos. Esta precisión es especialmente importante en el cálculo de las radiancias y de los flujos solares en la superficie, los cuales son cantidades fundamentales para caracterizar el entorno radiativo en la superficie y para maximizar el retorno científico de las misiones a Marte. Las simulaciones precisas de la radiación solar en la superficie marciana no sólo requieren modelos de transferencia radiativa detallados y validados, sino también un conocimiento exacto de las propiedades radiativas de los componentes atmosféricos, entre los que el polvo en suspensión es particularmente importante. La combinación de los resultados de los modelos y de las medidas de radiación solar desde la superficie marciana permiten la obtención de las propiedades del polvo en suspensión. El sensor de radiación ultravioleta (UVS) de REMS (Rover Environmental Monitoring Station), a bordo de la misión MSL (Mars Science Laboratory) ha estado midiendo la radiación solar en superficie por primera vez en seis bandas entre 200 y 380 nm. Estas medidas pueden proporcionar información sobre las propiedades y la variabilidad temporal del polvo en suspensión. El rango espectral de este sensor se verá ampliado en misiones futuras, tales como MetNet, que contará con un Sensor de Irradiancia Solar (MetSIS). Otras misiones futuras, tales como ExoMars 2020 y Mars 2020, también contarán con un RDS (Radiation and Dust Sensor)...

El estudio del entorno radiativo en la superficie marciana es fundamental para la comprensión y para una mejor caracterización de los procesos físicos de la atmósfera y el clima del planeta, así como para determinar el impacto biológico de la radiación ultravioleta. Estos dos objetivos son prioritarios en las misiones actuales y futuras a Marte debido a sus implicaciones en la preparación para la exploración humana del planeta. Debido a la importancia de la radiación solar, es necesario poder contar con modelos de transferencia radiativa precisos. Esta precisión es especialmente importante en el cálculo de las radiancias y de los flujos solares en la superficie, los cuales son cantidades fundamentales para caracterizar el entorno radiativo en la superficie y para maximizar el retorno científico de las misiones a Marte. Las simulaciones precisas de la radiación solar en la superficie marciana no sólo requieren modelos de transferencia radiativa detallados y validados, sino también un conocimiento exacto de las propiedades radiativas de los componentes atmosféricos, entre los que el polvo en suspensión es particularmente importante. La combinación de los resultados de los modelos y de las medidas de radiación solar desde la superficie marciana permiten la obtención de las propiedades del polvo en suspensión. El sensor de radiación ultravioleta (UVS) de REMS (Rover Environmental Monitoring Station), a bordo de la misión MSL (Mars Science Laboratory) ha estado midiendo la radiación solar en superficie por primera vez en seis bandas entre 200 y 380 nm. Estas medidas pueden proporcionar información sobre las propiedades y la variabilidad temporal del polvo en suspensión. El rango espectral de este sensor se verá ampliado en misiones futuras, tales como MetNet, que contará con un Sensor de Irradiancia Solar (MetSIS). Otras misiones futuras, tales como ExoMars 2020 y Mars 2020, también contarán con un RDS (Radiation and Dust Sensor)...

El estudio del entorno radiativo en la superficie marciana es fundamental para la comprensión y para una mejor caracterización de los procesos físicos de la atmósfera y el clima del planeta, así como para determinar el impacto biológico de la radiación ultravioleta. Estos dos objetivos son prioritarios en las misiones actuales y futuras a Marte debido a sus implicaciones en la preparación para la exploración humana del planeta. Debido a la importancia de la radiación solar, es necesario poder contar con modelos de transferencia radiativa precisos. Esta precisión es especialmente importante en el cálculo de las radiancias y de los flujos solares en la superficie, los cuales son cantidades fundamentales para caracterizar el entorno radiativo en la superficie y para maximizar el retorno científico de las misiones a Marte. Las simulaciones precisas de la radiación solar en la superficie marciana no sólo requieren modelos de transferencia radiativa detallados y validados, sino también un conocimiento exacto de las propiedades radiativas de los componentes atmosféricos, entre los que el polvo en suspensión es particularmente importante. La combinación de los resultados de los modelos y de las medidas de radiación solar desde la superficie marciana permiten la obtención de las propiedades del polvo en suspensión. El sensor de radiación ultravioleta (UVS) de REMS (Rover Environmental Monitoring Station), a bordo de la misión MSL (Mars Science Laboratory) ha estado midiendo la radiación solar en superficie por primera vez en seis bandas entre 200 y 380 nm. Estas medidas pueden proporcionar información sobre las propiedades y la variabilidad temporal del polvo en suspensión. El rango espectral de este sensor se verá ampliado en misiones futuras, tales como MetNet, que contará con un Sensor de Irradiancia Solar (MetSIS). Otras misiones futuras, tales como ExoMars 2020 y Mars 2020, también contarán con un RDS (Radiation and Dust Sensor)..., The study of the radiative environment at the Martian surface is paramount to understand and better characterize the physical processes of the atmosphere and the climate of the planet, as well as to determine the biological impact of ultraviolet radiation. These two objectives are a priority in current and future Mars missions due to their implications in the preparation for the human exploration of the planet. Due to the importance of solar radiation, accurate radiative transfer models are needed. Accuracy is particularly important for the calculation of the solar radiances and fluxes at the surface, which are key quantities to characterize the radiative environment at the surface and to maximize the scientific return of the missions to Mars. Accurate simulations of the solar radiation at the Martian surface require not only comprehensive and validated radiative transfer models, but also an accurate knowledge of the radiative properties of the atmospheric components, suspended dust being especially important. The combination of model results and solar radiation measurements from the Martian surface can allow the retrieval of the dust aerosol properties. The Ultraviolet Sensor (UVS) of the Rover Environmental Monitoring Station (REMS) on board the Mars Science Laboratory (MSL) mission has been measuring solar radiation at the surface of Mars for the first time in six bands between 200 and 380 nm. These measurements can provide information about the properties and temporal variability of the suspended dust. The spectral range of this sensor will be extended in future missions, such as MetNet, which will contain a Solar Irradiance Sensor (MetSIS). Other future missions, such as ExoMars 2020 and Mars 2020, will also carry a Radiation and Dust Sensor (RDS)...

El estudio del entorno radiativo en la superficie marciana es fundamental para la comprensión y para una mejor caracterización de los procesos físicos de la atmósfera y el clima del planeta, así como para determinar el impacto biológico de la radiación ultravioleta. Estos dos objetivos son prioritarios en las misiones actuales y futuras a Marte debido a sus implicaciones en la preparación para la exploración humana del planeta. Debido a la importancia de la radiación solar, es necesario poder contar con modelos de transferencia radiativa precisos. Esta precisión es especialmente importante en el cálculo de las radiancias y de los flujos solares en la superficie, los cuales son cantidades fundamentales para caracterizar el entorno radiativo en la superficie y para maximizar el retorno científico de las misiones a Marte. Las simulaciones precisas de la radiación solar en la superficie marciana no sólo requieren modelos de transferencia radiativa detallados y validados, sino también un conocimiento exacto de las propiedades radiativas de los componentes atmosféricos, entre los que el polvo en suspensión es particularmente importante. La combinación de los resultados de los modelos y de las medidas de radiación solar desde la superficie marciana permiten la obtención de las propiedades del polvo en suspensión. El sensor de radiación ultravioleta (UVS) de REMS (Rover Environmental Monitoring Station), a bordo de la misión MSL (Mars Science Laboratory) ha estado midiendo la radiación solar en superficie por primera vez en seis bandas entre 200 y 380 nm. Estas medidas pueden proporcionar información sobre las propiedades y la variabilidad temporal del polvo en suspensión. El rango espectral de este sensor se verá ampliado en misiones futuras, tales como MetNet, que contará con un Sensor de Irradiancia Solar (MetSIS). Otras misiones futuras, tales como ExoMars 2020 y Mars 2020, también contarán con un RDS (Radiation and Dust Sensor)..., The study of the radiative environment at the Martian surface is paramount to understand and better characterize the physical processes of the atmosphere and the climate of the planet, as well as to determine the biological impact of ultraviolet radiation. These two objectives are a priority in current and future Mars missions due to their implications in the preparation for the human exploration of the planet. Due to the importance of solar radiation, accurate radiative transfer models are needed. Accuracy is particularly important for the calculation of the solar radiances and fluxes at the surface, which are key quantities to characterize the radiative environment at the surface and to maximize the scientific return of the missions to Mars. Accurate simulations of the solar radiation at the Martian surface require not only comprehensive and validated radiative transfer models, but also an accurate knowledge of the radiative properties of the atmospheric components, suspended dust being especially important. The combination of model results and solar radiation measurements from the Martian surface can allow the retrieval of the dust aerosol properties. The Ultraviolet Sensor (UVS) of the Rover Environmental Monitoring Station (REMS) on board the Mars Science Laboratory (MSL) mission has been measuring solar radiation at the surface of Mars for the first time in six bands between 200 and 380 nm. These measurements can provide information about the properties and temporal variability of the suspended dust. The spectral range of this sensor will be extended in future missions, such as MetNet, which will contain a Solar Irradiance Sensor (MetSIS). Other future missions, such as ExoMars 2020 and Mars 2020, will also carry a Radiation and Dust Sensor (RDS)...