GEOLOGICAL MAPPING OF LUNAR CRATER LALANDE: TOPOGRAPHIC CONFIGURATION, MORPHOLOGY AND CRATERING PROCESS

Highland crater Lalande (4.45°&thinsp;S, 8.63°&thinsp;W; D&thinsp;=&thinsp;23.4&thinsp;km) is located on the PKT area of the lunar near side, southeast of Mare Insularum. It is a complex crater in Copernican era and has three distinguishing features: high silicic anomaly, highest Th abundance and special landforms on its floor. There are some low-relief bulges on the left of crater floor with regular circle or ellipse shapes. They are ~&thinsp;250 to 680&thinsp;m wide and ~&thinsp;30 to 91&thinsp;m high with maximum flank slopes >&thinsp;20°. There are two possible scenarios for the formation of these low-relief bulges which are impact melt products or young silicic volcanic eruptions. According to the absolute model ages of ejecta, melt ponds and hummocky floor, the ratio of diameter and depth, similar bugle features within other Copernican-aged craters and lack of volcanic source vents, we hypothesized that these low-relief bulges were most consistent with an origin of impact melts during the crater formation instead of small and young volcanic activities occurring on the crater floor. Based on Kaguya TC ortho-mosaic and DTM data produced by TC imagery in stereo, geological units and some linear features on the floor and wall of Lalande have been mapped. Eight geological units are organized by crater floor units: hummocky floor, central peak and low-relief bulges; and crater wall units: terraced walls, channeled and veneered walls, interior walls, mass wasting areas, blocky areas, and melt ponds. These geological units and linear features at Lalande provided us a chance to understand some details of the cratering process and elevation differences on the floor. We evaluated several possibilities to understand the potential causes for the observed elevation differences on the Lalande's floor. We proposed that late-stage wall collapse and subsidence due to melt cooling could be the possible causes of observed elevation differences on the floor.

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Geology of the Eminescu (H-09) quadrangle: Mapping status

10.5194/epsc2021-682 ◽

2021 ◽

Author(s):

Mayssa El Yazidi ◽

Gloria Tognon ◽

Valentina Galluzzi ◽

Lorenza Giacomini ◽

Matteo Massironi

Keyword(s):

Incidence Angle ◽

Central Peak ◽

Geological Mapping ◽

Geologic Mapping ◽

Linear Features ◽

Horizon 2020 ◽

The Status ◽

Global Mapping ◽

Dual Imaging ◽

Degradation Degree

Abstract The coordinated Mercury&#8217;s global mapping project (Galluzzi et al. (2021), aims at delivering quadrangle geological maps for the entire surface of Mercury by using the available basemaps derived from the NASA MESSENGER Mercury Dual Imaging Systems (MDIS) images. The NASA MESSENGER mission was able to cover the surface of Mercury with an average resolution of 200 m/px globally. This allows to produce a series of 1:3M regional geologic maps to be used in support to the ESA/JAXA BepiColombo mission. Here we present the status of the geologic mapping of the Eminescu (H-09) quadrangle, which covers the area between latitudes 22.5&#176;N, -22.5&#176;S and longitudes 72&#176;E, 144&#176;E. The selection of this quadrangle was based on its wealth of many interesting features (e.g., Beagle Rupes, hollow deposits on Eminescu crater, pyroclastic deposits at the margin of the Caloris basin) and on the color variability between the different terrain types that allows to reconstruct the geological history of H-09. Methods In this work, we used the available basemaps derived from the MESSENGER MDIS instrument images, such as the monochrome morphology image mosaics at high- and low-incidence angle (BDR, HIE, HIW and LOI) with a resolution of 166 m/px, together with the enhanced-color and 3-color global mosaics, having a resolution of 665 m/px. The chosen 1:3M output scale is achieved by mapping at an average scale of 1:400k, which is appropriate for the used basemaps. For the symbology, we applied, and in some cases revisited, the Federal Geographic Data Committee (FGDC) and the United Stated Geographic System (USGS) recommendations. The classification of the crater types was based on their diameter, degradation degree and superposition order. The crater's ejecta, central peak, and floor morphology (hummocky or smooth) were distinguished and mapped only for craters larger than 20 km, to avoid the saturation of map features. The terrain units were identified by means of morphology and crater-density, by distinguishing between smooth, intermediate and intercrater plains. We used different symbologies for geological contacts and linear features by distinguishing between certain and approximate contacts, or certain and uncertain/hidden structures, respectively. In particular, the linear features layer encompasses morphologies such as crater rims (up to 5 km in diameter), fault scarps, wrinkle ridges and volcanic vents. The variability in color and albedo was digitized within a surface features polygon layer (e.g., dark material, bright material, and hollow clusters). We did not consider details smaller than 4 km, nor linear features whose distance was smaller than this same threshold to avoid map readability issues. Results The mapping of H-09 is still in progress. The preliminary analysis shows an intriguing morphology related to endogenic and exogenic processes, where intensive tectonic and cratering structures constitute together the main geological events that provided the heterogeneity of terrains in the quadrangle. The tectonic events were probably driven by global cooling, however, we found both compressive and tensional tectonic features on the surface. Hollow clusters are spread all over the quadrangle in different sizes and locations (e.g., crater floors, central peaks). The Eminescu crater located in H-09, between latitudes 12.3&#176;N, 8.8&#176;N&#160; and longitudes 115.9&#176;E, 112.2&#176;E in H-09, is a relatively young crater on Mercury's surface and is characterized by extensive ejecta for one radius from the crater's rim and a recently hollowed central peak. These features and its enhanced color variability will probably require a higher-resolution study of this crater by integrating the geomorphological map with spectral data. This map will be the first geological product for this region with such a scale. Once the mapping is completed, we will be able to determine the absolute ages of the units to classify the terrains in chronological order and provide a complete geological and morphological analysis to understand the geological evolution of the quadrangle. Therefore, through the mapping of H-09 we aim at supporting the ESA/JAXA BepiColombo mission to Mercury by targeting all interesting features and contributing to the investigation and the understanding of Mercury. Keywords: Mercury (planet), Eminescu Quadrangle, Geological Mapping, MESSENGER, MDIS. Acknowledgements This research has been supported by European Union&#8217;s Horizon 2020 under grant agreement N&#176; 776276-PLANMAP. References Galluzzi et al. (2021), PGM Meeting 2021, LPI Contrib. No. 2610.

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Geological mapping of an interesting lunar site: Tsiolkovskiy crater

10.5194/egusphere-egu2020-733 ◽

2020 ◽

Author(s):

Gloria Tognon ◽

Riccardo Pozzobon ◽

Matteo Massironi

Keyword(s):

Central Peak ◽

Geological Mapping ◽

Crater Floor ◽

The European Union ◽

Horizon 2020 ◽

Geomorphological Mapping ◽

Lava Pile ◽

Definition Of ◽

Color Composite ◽

The Impact

Tsiolkovskiy is a 180 km diameter late Imbrian crater located at 20.4&#176; S, 129.1&#176; E on the far side of the Moon [Whitford-Stark & Hawke, 1982].Compared to the extensive mare deposits present of the lunar side facing the Earth, Tsiolkovskiy crater represents one of the few basaltic exposures on the far side [Pieters & Tompkins, 1999]. Along with its particularly dark and smooth crater floor, the impact crater is also characterized by a morphologically well-shaped central peak on which has been detected both olivine [Corley et al., 2018] and PAN [Ohtake et al., 2009; Lemelin et al., 2015].The area represents thus a potential scientific site of interest for a safe landing. The production of geological maps aiming at characterize Tsiolkovskiy crater will allow the definition of interesting locations for rover exploration.A geomorphological mapping of the crater has been performed using the ~100m/pixel LRO-WAC [Robinson et al., 2010] global mosaic along with the ~59m/pixel LRO-LOLA and Kaguya TC DEM merge which has a vertical resolution of 3-4m [Barker et al., 2016]. The mapping defined six units corresponding to the well-recognizable central peak and the texturally different smooth and hummocky materials constituting the crater floor units, and by scarps with slopes >40&#176;, isolated ponds of smooth material discernible from the rough material constituting the crater rim and constituting the crater walls units.The geomorphological mapping has then been coupled with a spectral characterization of Tsiolkovskiy crater performed on the basis of the ~200m/pixel Clementine UVVIS false color composite (Red 750/415nm; Green 750/1000nm; Blue 415/740nm) [Lucey et al., 2000]. The spectral mapping allowed to discriminate different units characterized by different origin and composition. In particular, the morphologically smooth crater floor unit is composed by fresher basalts and basaltic soils, the steep scarps and the central peak units are mostly composed by norites, troctolites and anorthosites, while the remaining smooth ponds, crater rim and the hummocky crater floor units are generally composed by mature highland soils.In order to define landing ellipses and broad traverses for a rover exploration of the site, the geological mapping is also been supported by an ongoing high-resolution mapping of a quarter of Tsiolkovskiy crater by means of a mosaic of ~0.5m/pixel LRO-NAC [Robinson et al., 2010] images here scaled to 3m/pixel.Finally, a radar investigation for the presence of deep structures will be performed to possibly detect lava pile emplacements and voids in the crater subsoil.AcknowledgmentsThis research was supported by the European Union&#8217;s Horizon 2020 under grant agreement No 776276-PLANMAP.ReferencesWhitford-Stark, J.L. & Hawke, B.R., XXXIII LPSC, pp. 861-862, 1982Barker, M.K. et al., Icarus, Vol. 273, pp. 346-355, 2016Pieters, C.M. & Tompkins, S., JGR, Vol. 104, pp. 21935-21949, 1999Corley, L.M. et al., Icarus, Vol. 300, pp. 287-304, 2018Ohtake, M. et al., Nature, Vol. 461, pp. 236-241, 2009Lemelin, M. et al., JGR: Planets, Vol. 120, pp. 869-8878, 2015Robinson, M.S. et al., Space Sci. Rev., Vol. 150, pp. 81&#8211;124, 2010Barker, M.K., et al., Icarus, Vol. 273, pp. 346-355, 2016Lucey, P.G. et al., JGR, Vol. 105, pp. 20377-20386, 2000

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Geology of Shantipur-Wami Taksar Areas of Gulmi-Baglung Districts, Western Nepal

Bulletin of the Department of Geology ◽

10.3126/bdg.v22i0.33412 ◽

2020 ◽

Vol 22 ◽

pp. 29-32

Author(s):

Sushant Sapkota ◽

Pashupati Gaire ◽

Kabi Raj Paudyal

Keyword(s):

Regional Scale ◽

Mineral Resources ◽

Geological Structure ◽

Geological Mapping ◽

The North ◽

Copper Mineralization ◽

Metallic Mineral ◽

Geological Map ◽

Map Scale ◽

Geological Units

The study area represents a small part of the Lesser Himalaya in western Nepal and lies about 346 km west from Kathmandu. It covers 250 km area representing some parts of Gulmi and Baglung districts. The area was selected for the present study on the impression from the previous geological map that has showed some metallic mineral resources like iron, copper and lead in the region. Similarly, studies reveal that there is very complicated geological structure which raised the interest for the study. Main objective of the study was to prepare a geological map of the area in a scale of 1:25,000 and study the possible mineral deposits. An extensive geological mapping was carried out in the field covering at one data within one centimetre of the map scale and large number of samples was collected for the petrographic as well as ore genesis studies. The rocks of the region were mapped under two geological units as the Nourpul Formation (older) and the Dhading Dolomite (younger). There are a series of folds in the area. From regional to micro-scale all folds are trending towards east-west. The Badi Gad Fault and the Harewa Khola Thrust are the regional scale thrust mapped in the area. The Badi Gad is considered as a strike-slip in nature. The Harewa Khola Thrust is probably an imbricate fault. It has propagated to the north which is out of sequence in nature. Some metallic minerals like copper and iron along with old working mines were observed during the study. Occurrences of copper and iron mineralization has been mapped and described. Present study revealed that copper mineralization is limited within the veins and boudinage forms as hydrothermal deposit while the iron is tabular and syngenetic in nature.

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Assessing Volcanic Hazard

10.1093/oxfordhb/9780190676889.013.32 ◽

2017 ◽

Author(s):

Joan Martí Molist

Keyword(s):

Hazard Assessment ◽

Volcanic Hazard ◽

Main Tool ◽

Volcanic Eruptions ◽

Historical Record ◽

Geological Mapping ◽

Volcanic System ◽

Future Behavior ◽

Geophysical Information ◽

Past Activity

Volcanoes represent complex geological systems capable of generating many dangerous phenomena. To evaluate and manage volcanic risk, we need first to assess volcanic hazard (i.e., identify past volcanic system behavior to infer future behavior. This requires acquisition of all relevant geological and geophysical information, such as stratigraphic studies, geological mapping, sedimentological studies, petrologic studies, and structural studies. All this information is then used to elaborate eruption scenarios and hazard maps. Stratigraphic studies represent the main tool for the reconstruction of past activity of volcanoes over time periods exceeding their historical record. This review presents a systematic approach to volcanic hazard assessment, paying special attention to reconstruction of past eruptive history. It reviews concepts and methods most commonly used in long- and short-term hazard assessment and analyzes how they help address the various serious consequences derived from the occurrence (and nonoccurrence in some crisis alerts) of volcanic eruptions and related phenomena.

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Predictive Geological Mapping from Geophysical Data Using Self-Organizing Maps: A Case Study from Baie Verte, NL, Canada

Geophysics ◽

10.1190/geo2020-0756.1 ◽

2021 ◽

pp. 1-55

Author(s):

Angela Carter-McAuslan ◽

Colin Farquharson

Keyword(s):

Gravity Data ◽

Geological Mapping ◽

Magnetic Data ◽

Self Organizing Maps ◽

Predictive Mapping ◽

Legacy Data ◽

Geological Units ◽

Radiometric Data ◽

Self Organizing

Self-organizing maps (SOMs) are a type of unsupervised artificial neural networks clustering tool. SOMs are used to cluster large multi-variate datasets. They can identify patterns and trends in the geophysical maps of an area and generate proxy geology maps, known as remote predictive mapping. We applied SOMs to magnetic, radiometric and gravity datasets compiled from multiple modern and legacy data sources over the Baie Verte Peninsula, Newfoundland, Canada. The regional and local geological maps available for this area and the knowledge from numerous geological studies allowed for assessing the accuracy of the SOM-based predictive mapping. Proxy geology maps generated by primary clustering directly from the SOMs and secondary clustering using a k-means approach reproduced many geological units identified by previous traditional geological mapping. Of the combinations of datasets tested, the combination of magnetic data, primary radiometric data and their ratios, and Bouguer gravity data gave the best results. We found that using reduced-to-the-pole residual intensity or analytic signal as the magnetic data were equally useful. The SOM process was unaffected by gaps in the coverage of some of the datasets. The SOM results could be used as input into k-means clustering as k-means clustering requires no gaps in the data. The subsequent k-means clustering resulted in more meaningful proxy geology maps than were created by the SOM alone. In regions where the geology is poorly known, these proxy maps can be useful in targeting where traditional, on-the-ground geological mapping would be most beneficial which can be especially useful in parts of the world where access is difficult and expensive.

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LANDSLIDES AND THE INCORRECT INTERPRETATION OF GEOLOGICAL STRUCTURE – EXAMPLES FROM THE SUDETY MOUNTAINS

Biuletyn Państwowego Instytutu Geologicznego ◽

10.5604/01.3001.0012.7708 ◽

2018 ◽

Vol 473 (473) ◽

pp. 27-48

Author(s):

Aleksander KOWALSKI

Keyword(s):

Geological Structure ◽

Geological Mapping ◽

Structural Elements ◽

Geomorphological Mapping ◽

The Past ◽

Bedding Planes ◽

Sw Poland ◽

Geological Units ◽

Lower Silesia

Despite the relatively large number of individual landslides recognized and described over the last several years from the Sudety (Sudetes) Mountains (Lower Silesia, SW Poland), most of the papers focused on the geomorphological characterisation of these forms. This paper presents the results of geological and geomorphological mapping of individual landslides, recognized within three geological units: the Wleń Graben (Northsudetic Synclinorium), the Łączna Elevation (Intrasudetic Synclinorium) and the Glinno Graben (Sowie Mountains Block). Particular attention has been paid to the role of the geological structure in the initiation and development of mass movements as well as the degree of transformation of the planar, structural elements (bedding planes, joints, faults) of the landslide bedrock. The results of geological mapping and geomorphometric analysis with a basis in Light Detection and Ranging (LiDAR) show that the structural measurements carried out in the past within previously unrecognized landslides were probably the main reason for incorrect interpretations of the geology of the areas investigated.

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The Cyborg Astrobiologist: matching of prior textures by image compression for geological mapping and novelty detection

International Journal of Astrobiology ◽

10.1017/s1473550413000372 ◽

2014 ◽

Vol 13 (3) ◽

pp. 191-202 ◽

Cited By ~ 2

Author(s):

P.C. McGuire ◽

A. Bonnici ◽

K.R. Bruner ◽

C. Gross ◽

J. Ormö ◽

...

Keyword(s):

Image Compression ◽

Novelty Detection ◽

Current System ◽

Geological Mapping ◽

Coal Bed ◽

Field Site ◽

Image Comparison ◽

Similarity Detection ◽

Geological Units ◽

Comparison Technique

AbstractWe describe an image-comparison technique of Heidemann and Ritter (2008a, b), which uses image compression, and is capable of: (i) detecting novel textures in a series of images, as well as of: (ii) alerting the user to the similarity of a new image to a previously observed texture. This image-comparison technique has been implemented and tested using our Astrobiology Phone-cam system, which employs Bluetooth communication to send images to a local laptop server in the field for the image-compression analysis. We tested the system in a field site displaying a heterogeneous suite of sandstones, limestones, mudstones and coal beds. Some of the rocks are partly covered with lichen. The image-matching procedure of this system performed very well with data obtained through our field test, grouping all images of yellow lichens together and grouping all images of a coal bed together, and giving 91% accuracy for similarity detection. Such similarity detection could be employed to make maps of different geological units. The novelty-detection performance of our system was also rather good (64% accuracy). Such novelty detection may become valuable in searching for new geological units, which could be of astrobiological interest. The current system is not directly intended for mapping and novelty detection of a second field site based on image-compression analysis of an image database from a first field site, although our current system could be further developed towards this end. Furthermore, the image-comparison technique is an unsupervised technique that is not capable of directly classifying an image as containing a particular geological feature; labelling of such geological features is donepost factoby human geologists associated with this study, for the purpose of analysing the system's performance. By providing more advanced capabilities for similarity detection and novelty detection, this image-compression technique could be useful in giving more scientific autonomy to robotic planetary rovers, and in assisting human astronauts in their geological exploration and assessment.

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Improving Ensemble Volcanic Ash Forecasts by Direct Insertion of Satellite Data and Ensemble Filtering

Atmosphere ◽

10.3390/atmos12091215 ◽

2021 ◽

Vol 12 (9) ◽

pp. 1215

Author(s):

Meelis J. Zidikheri ◽

Chris Lucas

Keyword(s):

Volcanic Ash ◽

Weather Prediction ◽

Source Parameters ◽

Volcanic Eruptions ◽

Forecast Skill ◽

Aviation Industry ◽

Transport Modelling ◽

Volcanic Source ◽

Mass Load ◽

Ensemble Filtering

Improved quantitative forecasts of volcanic ash are in great demand by the aviation industry to enable better risk management during disruptive volcanic eruption events. However, poor knowledge of volcanic source parameters and other dispersion and transport modelling uncertainties, such as those due to errors in numerical weather prediction fields, make this problem very challenging. Nonetheless, satellite-based algorithms that retrieve ash properties, such as mass load, effective radius, and cloud top height, combined with inverse modelling techniques, such as ensemble filtering, can significantly ameliorate these problems. The satellite-retrieved data can be used to better constrain the volcanic source parameters, but they can also be used to avoid the description of the volcanic source altogether by direct insertion into the forecasting model. In this study we investigate the utility of the direct insertion approach when employed within an ensemble filtering framework. Ensemble members are formed by initializing dispersion models with data from different timesteps, different values of cloud top height, thickness, and NWP ensemble members. This large ensemble is then filtered with respect to observations to produce a refined forecast. We apply this approach to 14 different eruption case studies in the tropical atmosphere. We demonstrate that the direct insertion of data improves model forecast skill, particularly when it is used in a hybrid ensemble in which some ensemble members are initialized from the volcanic source. Moreover, good forecast skill can be obtained even when detailed satellite retrievals are not available, which is frequently the case for volcanic eruptions in the tropics.

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Detailed age determinations for Tsiolkovskiy crater floor

10.5194/egusphere-egu21-10084 ◽

2021 ◽

Author(s):

Gloria Tognon ◽

Sabrina Ferrari ◽

Riccardo Pozzobon ◽

Matteo Massironi

Keyword(s):

Age Determination ◽

Total Surface Area ◽

Geological Mapping ◽

Crater Floor ◽

The European Union ◽

Frequency Distributions ◽

Horizon 2020 ◽

Color Ratio ◽

Crater Size ◽

Size Frequency

With respect to its counterpart, the lunar farside is characterized by few basaltic mare exposures. One of these, with a total surface area of approximately 12 000 km2, covers the floor of the ~200 km diameter Tsiolkovskiy crater (20.4&#176; S, 129.1&#176; E) [1].The crater size frequency distributions (CSFDs) calculated for this crater led to different results. The age determination performed on the mare infilling resulted in an Imbrian-Erathostenian age of about 3.2 Ga [2], while a 3.6 Ga Late Imbrian age was derived from areas scattered on top of a long run-out landslide generated from the western rim and its surroundings [3-4].The spectral map produced for Tsiolkovskiy crater [5-6], performed on the ~200 m/pixel Clementine UVVIS color ratio mosaic [7] (R: 750/415 nm; G: 750/1000 nm; B: 415/750 nm), and recently updated suggests for the crater floor the presence of three color units, characteristics of higher 415/750 nm ratio, higher 750/415 nm ratio and average 750/415 nm and 750/1000 nm ratios, defined by a different composition and/or age formation.In order to discriminate possible age differences ascribable to different eruptive events, on the basis of the spectral mapping we defined several areas for measuring the crater size-frequency distributions of the different color units on the crater floor. In addition, we calculated the age formation of Tsiolkovskiy crater itself by means of hummocky areas interpreted as impact melt identified in accordance to the geological mapping [5-6] performed on the ~100 m/pixel LRO-WAC [8] global mosaic.The CSFDs measurements have been performed on areas of at least 100 km2 using the CraterTools add-on [9] in the ArcGIS software on LRO-NAC [8] images with resolution ranging between 0.5 and 1.5 m/pixel. The exported data have then been plotted in the Craterstats2 software [10].The obtained results highlight that i) Tsiolkovskiy crater formed around 3.6 Ga, in agreement with [3], ii) three different age ranges are discernible and iii) these age ranges are correlated to each one of the three color units of the crater floor.This allows to reconstruct the evolution history of the crater and in particular of its crater floor, with particular focus also on its compositional variegation.&#160;AcknowledgmentsThis research was supported by the European Union&#8217;s Horizon 2020 under grant agreement No 776276-PLANMAP.References[1] Whitford-Stark, J.L. & Hawke, B.R., XXXIII LPSC, pp. 861-862, 1982&#160; [2] Pasckert, J.H. et al., Icarus, Vol. 257, pp. 336-354, 2015&#160; [3] Boyce, J.M. et al., XXXXVII LPSC, 2471, 2016&#160; [4] Boyce, J.M. et al., Icarus, Vol. 337, 2020&#160; [5] Tognon, G. et al., EGU, 733, 2020&#160; [6] Tognon, G. et al., EPSC, 581, 2020&#160; [7] Lucey, P.G. et al., JGR, Vol. 105, pp. 20377-20386, 2000&#160; [8] Robinson, M.S. et al., Space Sci. Rev., Vol. 150, pp. 81&#8211;124, 2010&#160; [9] Kneissl, M. et al., Plan. Space Sci., Vol. 59, pp. 1243-1254, 2011&#160; [10] Michael G.G. & Neukum, G., Earth and Plan. Sci. Letters, Vol. 294, pp. 223-229, 2010

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The geology of Yelcho Station: a new high-resolution geological map at northwestern Antarctic Peninsula

10.5194/egusphere-egu21-12707 ◽

2021 ◽

Author(s):

Wuidad Jara ◽

Joaquin Bastias ◽

Ricardo Jaña ◽

Marcelo Leppe

Keyword(s):

Antarctic Peninsula ◽

Satellite Images ◽

Geological Mapping ◽

Spectral Studies ◽

Future Studies ◽

Volcanic Deposits ◽

Northwestern Region ◽

Geological Map ◽

Geological Units ◽

The Antarctic

Yelcho Station is set on Doumer Island located in the southernmost section of Gerlache Strait between Anvers and Wienke Islands at the northwestern region of Antarctic Peninsula. This area is dominated by plutonic and volcanic deposits associated with the active margin developed during the Mesozoic and Cenozoic in the Antarctic Peninsula (e.g. Leat et al., 1995). Although Yelcho Station has been intensively visited since a few decades, the outcropping rocks have not been studied in detail. Furthermore, this location has hosted relevant contributions in the environmental and ecological sciences. We will present a detailed map (1:500) of the geological units outcropping in Yelcho Station based in fieldwork observations, which will be combined with drone and satellite images. Additionally, remote sensing spectral studies will be developed to support the geological mapping. This work will help to establish a geological baseline, which may serve for future studies in the area of Yelcho Station. This contribution will be a detailed geological study in the Antarctic Peninsula, which will also enhance our understanding of the geological units outcropping in Gerlache Strait. This material will also serve as an educational and outreach information for the polar community.Leat et al. (1995). Geological Magazine 132 (4), 399-412 (DOI: 10.1017/S0016756800021464).

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