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The DTM (a) and the slope map (b) of the analysed area using HRSC topographic data. One of the steepest slopes (bright colour in the right inset) can be found along the main valley.
Source publication
This work analysis an 81 km long 1.85 km wide fluvial valley on Mars (at 2°55’ South and 111°53’ East) for the first time, located near to the so-called Palos carter and Tinto Vallis, called Tinto-B hereafter. The length of the valley is approximately 81 km, and the average width is ~1.85 km, depth ~250 m. The hypsometric curves were created in 5 d...
Contexts in source publication
Context 1
... is situated near to Palos crater and Tinto Vallis (Figure 1), thus, the analysed Vallis was named Tinto-B. This area includes several smaller valleys, which are located West from Tinto-B Vallis (see later the western part in Figure 2 inset 'a'). ...
Context 2
... hydrological analysis was made in ArcMap with ArcHydroTools (used version: 10.2) to identify post fluvial eroded, thus, poorly visible ancient tributaries. In this research, the authors used the Fill tool to auto-fill the possible depressions on the used DTM and Flow Direction and Flow Accumulation tools to determine the gullies and flows on the analysed area ( Figure 2). For crater identification the above-listed CTX image was used, where those features were counted as craters, which were at least 4-6 pixel diameter, showed an arc-shaped brighter and a darker features and they presented a circular shape together (minimum crater size: 20 metres). ...
Citations
... This work aims to apply the Earth-based model to Martian valleys, namely the Tinto-B valley [21], comparing it with the almost vegetation and soil-free Zafit basin in the Negev desert of Israel, from which the data on the reference precipitation event were collected. ...
... The second hypothesis posits that the valley is of volcanic origin [25] and that the surrounding valleys were formed by water released from the permafrost melted by volcanic activity. This hypothesis is corroborated by the results of the absolute age estimation based on crater statistics [26] in Tinto B [21]. The results suggest that the age of the study area corresponds to the period of the flood channels [27], which were common at the boundary of the Martian Hesperian and Amazonian periods. ...
... To address this limitation, the THEMIS TI [33,34] data were used to determine the different sediment size distributions of the Martian surface [35,36]. For Tinto B, the median sediment size from the entire watershed was 1 mm [21]. To ensure comparability of the results, this median sediment size was also employed for the terrestrial area of interest. ...
While fluvial features are plentiful on Mars and offer valuable insights into past surface conditions, the climatic conditions inferred from these valleys, like precipitation and surface runoff discharges, remain the subject of debate. Model-based estimations have already been applied to several Martian valleys, but exploration of the related numerical estimations has been limited. This work applies an improved precipitation-based, steady-state erosion/accumulation model to a Martian valley and compares it to a terrestrial Mars analogue dessert catchment area. The simulations are based on a previously observed precipitation event and estimate the fluvial-related hydrological parameters, like flow depth, velocity, and erosion/accumulation processes in two different but morphologically similar watersheds. Moderate differences were observed in the erosion/accumulation results (0.13/−0.06 kg/m²/s for Zafit (Earth) and 0.01/−0.007 for Tinto B (Mars)). The difference is probably related to the lower areal ratio of surface on Mars where the shield factor is enough to trigger sediment movement, while in the Zafit basin, there is a larger area of undulating surface. The model could be applied to the whole surface of Mars. Using grain size estimation from the global THEMIS dataset, the grain size value artificially increased above that observed, and decreased hypothetic target rock density tests demonstrated that the model works according to theoretical expectations and is useful for further development. The findings of this work indicate the necessity of further testing of similar models on Mars and a better general analysis of the background geomorphological understanding of surface evolution regarding slope angles.
... Our prior iteration of the Mars-specific SIMWE model employed a hypothetical precipitation value [78] that produced the ancient flow paths using the best available approach, providing a realistic simulation of the locations of former water flow tracks. However, we acknowledge that multiple processes could lead to the poor reconstruction of ancient flow paths on Mars, such as later topographic modification [29], or the newly acknowledged potential of Martian aeolian-fluvial interactions [79]. ...
... As a summary, this model aids in the identification of locations that might not be discernible through orbital optical imagery, such as concealed sedimentary formations and minor drainage pathways [78]. ...
Identifying surface sites with significant astrobiological potential on Mars requires a comprehensive understanding of past geological processes and conditions there, including the shallow subsurface region. Numerical modelling could distinguish between regions dominated by erosion and those characterized by sediment accumulation in ancient wet environments. The target area of Jezero Crater is relatively well explored and thus is an ideal site to evaluate model calculations; however, important works are still missing on expectations related to its shallow subsurface . In this work, the best available approaches were followed, and only surface morphology was considered (supposedly formed by the last fluvial episode). The shallow subsurface became an important target recently, and this model could provide new inputs in this area. Erosion–accumulation models are suitable for terrestrial surface features, but few have been applied to Mars. This work addresses this challenge using the SIMWE (SIMulated Water Erosion) model on the Jezero Crater delta, the landing site of the Perseverance rover. For calculations, the average grain size according to the THEMIS TI data was applied to the target area. The flow depth varied between 1.89 and 34.74 m (average of 12.66 m). The water-filled channel width ranged from 35.3 to 341.42 m. A flow velocity of 0.008–11.6 m/s, a maximum erosion rate of 5.98 g/m²/h, and a deposition 4.07 g/m²/h were estimated. These calculated values are close to the range of estimations from other authors assuming precipitation of 1–20 mm/h and discharges of 60–400 m³/s. The model was able to distinguish between erosion- and accumulation-dominated areas about 1 m above Jezero Crater’s delta that are not visible from above. This model helps to identify the accumulation-dominated areas with the finest grain size with good preservation capability for the shallow but invisible subsurface.
... There is an ongoing debate on how past Martian climate conditions can be reconstructed [5]; the most popular method is based on the evaluation of past water discharges in fluvial channels [6][7][8] associated with volumetric and temporal estimation methods of lacustrine environments [9]. However, related mineralogical and chemical investigations are also of key importance [10] and have not only paleoclimatic but also astrobiology implications: especially given that, in the case of carbonate minerals, the precipitation of carbonate in a liquid water environment is a key biosignature preservation mechanism [11]. ...
The presence of minerals formed under the occurrence of liquid water during the first billion years on Mars was a key discovery, but there is still a large number of open issues that make the study of these mineral deposits a main focus of remote sensing and laboratory studies. Moreover, even though there is extensive research related to the study of the spectral behavior of mixtures, we still lack a full understanding of the problem. The main goal of this work is the analysis of the detection limits of hydrated and carbonate phases within mixtures with basaltic-like fine regolith in the spectral region 1.0–5.5 µm (1818–10,000 cm−1). We selected two different basalt samples and mixed them with two carbonate phases: a dolomite and a calcite. Spectral features have been investigated isolating the main carbonate absorption features and overtones; deriving trends of spectral parameters such as band depth, band area, full-width-half-maximum; percentage and grain size variations. The results obtained in this work show how the presence of a basaltic component can strongly influence the appearance of the hydrated and carbonate features showing different trends and intensities depending on the grain size and percentage of the carbonate components.
O presente trabalho propõe realizar uma análise bibliométrica com trabalhos relacionados à erosão do solo e utilização de modelos hidrológicos, dando destaque ao modelo SIMWE e na sequência ranquear os mais relevantes por meio de método estatístico. Para a realização do trabalho, utilizou-se das bases Scopus e Web of Science para obter dados, que foram manipulados em ferramentas de um pacote de programação em linguagem R, o qual também permitiu a plotagem dos dados em gráficos e tabelas. Em termos de resultados, foram encontrados 373 trabalhos, com destaque para o maior número de produções na última década. Isso se deve aos avanços no manuseio de dados e a possibilidade de geração de modelos por meio de softwares, muitos deles de código aberto. Em relação à aplicação do modelo SIMWE, possui importante aplicação em áreas de vinhas no Mediterrâneo, com condições de solo e relevo suscetíveis a processos de erosão acelerada. O ranqueamento das publicações, utilizando o Methodi Ordinatio, permitiu conhecer as publicações mais relevantes da busca com base no ano de publicação, número de citações e fator de impacto da revista. A modelagem hidrológica tem se expandido bastante, permitindo a compreensão da dinâmica de processos e a geração de cenários.
