Journal articles: 'MARS-3D'

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Loy, D. Gareth. "Mars in 3D." Computer Music Journal 37, no. 3 (September 2013): 101–3. http://dx.doi.org/10.1162/comj_r_00188.

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Kallio, E., H. Koskinen, S. Barabash, R. Lundin, O. Norberg, and J. G. Luhmann. "3D plasma observations near Mars." Geophysical Research Letters 20, no. 21 (November 5, 1993): 2339–42. http://dx.doi.org/10.1029/93gl02634.

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Courtland, Rachel. "Review: Mars 3D by Jim Bell." New Scientist 200, no. 2686 (December 2008): 47. http://dx.doi.org/10.1016/s0262-4079(08)63167-x.

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O'Neill, Sean. "3D print a home on Mars." New Scientist 226, no. 3023 (May 2015): 27. http://dx.doi.org/10.1016/s0262-4079(15)30462-0.

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Grace, Robert. "Habitats for Humanity - Potentially 3D Printed on Mars." Plastics Engineering 73, no. 8 (September 2017): 16. http://dx.doi.org/10.1002/j.1941-9635.2017.tb01773.x.

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Tao, Yu, Greg Michael, Jan-Peter Muller, Susan J. Conway, and Alfiah R. D. Putri. "Seamless 3D Image Mapping and Mosaicing of Valles Marineris on Mars Using Orbital HRSC Stereo and Panchromatic Images." Remote Sensing 13, no. 7 (April 3, 2021): 1385. http://dx.doi.org/10.3390/rs13071385.

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A seamless mosaic has been constructed including a 3D terrain model at 50 m grid-spacing and a corresponding terrain-corrected orthoimage at 12.5 m using a novel approach applied to ESA Mars Express High Resolution Stereo Camera orbital (HRSC) images of Mars. This method consists of blending and harmonising 3D models and normalising reflectance to a global albedo map. Eleven HRSC image sets were processed to Digital Terrain Models (DTM) based on an opensource stereo photogrammetric package called CASP-GO and merged with 71 published DTMs from the HRSC team. In order to achieve high quality and complete DTM coverage, a new method was developed to combine data derived from different stereo matching approaches to achieve a uniform outcome. This new approach was developed for high-accuracy data fusion of different DTMs at dissimilar grid-spacing and provenance which employs joint 3D and image co-registration, and B-spline fitting against the global Mars Orbiter Laser Altimeter (MOLA) standard reference. Each HRSC strip is normalised against a global albedo map to ensure that the very different lighting conditions could be corrected and resulting in a tiled set of seamless mosaics. The final 3D terrain model is compared against the MOLA height reference and the results shown of this intercomparison both in altitude and planum. Visualisation and access mechanisms to the final open access products are described.

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Domínguez-Pumar, Manuel, Lukasz Kowalski, Vicente Jiménez, Ivette Rodríguez, Manel Soria, Sandra Bermejo, and Joan Pons-Nin. "Analyzing the Performance of a Miniature 3D Wind Sensor for Mars." Sensors 20, no. 20 (October 20, 2020): 5912. http://dx.doi.org/10.3390/s20205912.

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This paper analyzes the behavior of a miniature 3D wind sensor designed for Mars atmosphere. The sensor is a spherical structure of 10 mm diameter divided in four sectors. By setting all the sectors to constant temperature, above that of the air, the 3D wind velocity vector can be measured. Two sets of experiments have been performed. First, an experimental campaign made under typical Mars conditions at the Aarhus Wind Tunnel Simulator is presented. The results demonstrate that both wind speed and angle can be efficiently measured, using a simple inverse algorithm. The effect of sudden wind changes is also analyzed and fast response times in the range of 0.7 s are obtained. The second set of experiments is focused on analyzing the performance of the sensor under extreme Martian wind conditions, reaching and going beyond the Dust Devil scale. To this purpose, both high-fidelity numerical simulations of fluid dynamics and heat transfer and experiments with the sensor have been performed. The results of the experiments, made for winds in the Reynolds number 1000–2000 range, which represent 65–130 m/s of wind speed under typical Mars conditions, further confirm the simulation predictions and show that it will be possible to successfully measure wind speed and direction even under these extreme regimes.

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Basdogan, Cagatay. "From 2D Images to 3D Tangible Models: Autostereoscopic and Haptic Visualization of Martian Rocks in Virtual Environments." Presence: Teleoperators and Virtual Environments 16, no. 1 (February 1, 2007): 1–15. http://dx.doi.org/10.1162/pres.16.1.1.

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A planetary rover acquires a large collection of images while exploring its surrounding environment. For example, 2D stereo images of the Martian surface captured by the lander and the Sojourner rover during the Mars Pathfinder mission in 1997 were transmitted to Earth for scientific analysis and navigation planning. Due to the limited memory and computational power of the Sojourner rover, most of the images were captured by the lander and then transmitted to Earth directly for processing. If these images were merged together at the rover site to reconstruct a 3D representation of the rover's environment using its on-board resources, more information could potentially be transmitted to Earth in a compact manner. However, construction of a 3D model from multiple views is a highly challenging task to accomplish even for the new generation rovers (Spirit and Opportunity) running on the Mars surface at the time this article was written. Moreover, low transmission rates and communication intervals between Earth and Mars make the transmission of any data more difficult. We propose a robust and computationally efficient method for progressive transmission of multi-resolution 3D models of Martian rocks and soil reconstructed from a series of stereo images. For visualization of these models on Earth, we have developed a new multimodal visualization setup that integrates vision and touch. Our scheme for 3D reconstruction of Martian rocks from 2D images for visualization on Earth involves four main steps: a) acquisition of scans: depth maps are generated from stereo images, b) integration of scans: the scans are correctly positioned and oriented with respect to each other and fused to construct a 3D volumetric representation of the rocks using an octree, c) transmission: the volumetric data is encoded and progressively transmitted to Earth, d) visualization: a surface model is reconstructed from the transmitted data on Earth and displayed to a user through a new autostereoscopic visualization table and a haptic device for providing touch feedback. To test the practical utility of our approach, we first captured a sequence of stereo images of a rock surface from various viewpoints in JPL MarsYard using a mobile cart and then performed a series of 3D reconstruction experiments. In this paper, we discuss the steps of our reconstruction process, our multimodal visualization system, and the tradeoffs that have to be made to transmit multiresolution 3D models to Earth in an efficient manner under the constraints of limited computational resources, low transmission rate, and communication interval between Earth and Mars.

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Coughlin, Natalie, Bradley Drake, Mikala Fjerstad, Easton Schuster, Tyler Waege, Adrian Weerakkody, and Todd Letcher. "Development and Mechanical Properties of Basalt Fiber-Reinforced Acrylonitrile Butadiene Styrene for In-Space Manufacturing Applications." Journal of Composites Science 3, no. 3 (September 5, 2019): 89. http://dx.doi.org/10.3390/jcs3030089.

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A new basalt fiber reinforced acrylonitrile butadiene styrene (ABS) filament has been developed for fused filament fabrication (FFF, 3D printing) to be used in Mars habitat construction. Building habitats on Mars will be expensive, especially if all material must be shipped from earth. However, if some materials can be used from Mars, costs will dramatically decrease. Basalt is easily mined from the surface of Mars. This study details the production process of the material, experimental results from mechanical testing, and preliminary X-ray shielding characteristics. The addition of chopped 3 mm basalt fibers to standard FFF material, ABS, increased strength and stiffness of the composite material. By adding 25% (by weight) basalt fiber to ABS, tensile strength improved nearly 40% by increasing from 36.55 MPa to 50.58 MPa, while Modulus of Elasticity increased about 120% from 2.15 GPa to 4.79 GPa. Flexural strength increased by about 20% from 56.94 MPa to 68.51 MPa, while Flexural Modulus increased by about 70% from 1.81 GPa to 3.05 GPa. While compression results did not see much strength improvements, the addition of fibers also did not decrease compressive strength. This is important when considering that basalt fibers provide radiation shielding and the cost of adding basalt fibers to construction materials on Mars will be negligible compared to the cost of shipping other materials from earth. In preliminary digital radiography testing, it was shown that 77% of X-rays were shielded with 25% basalt fiber added (as compared to neat ABS). In small-scale 3D printing applications, the 25% fiber ratio seems to be the highest ratio that provides reliable FFF printing.

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Basak, Arnab, and Dibyendu Nandy. "Modelling the imposed magnetospheres of Mars-like exoplanets: star–planet interactions and atmospheric losses." Monthly Notices of the Royal Astronomical Society 502, no. 3 (January 28, 2021): 3569–81. http://dx.doi.org/10.1093/mnras/stab225.

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ABSTRACT Based on 3D compressible magnetohydrodynamic simulations, we explore the interactions between the magnetized wind from a solar-like star and a Mars-like planet – with a gravitionally stratified atmosphere – that is either non-magnetized or hosts a weak intrinsic dipolar field. The primary mechanism for the induction of a magnetosphere around a non-magnetized conducting planet is the pile-up of stellar magnetic fields in the day-side region. The magnetopause stand-off distance decreases as the strength of the planetary dipole field is lowered and saturates to a minimum value for the case of a planet with no magnetic field. Global features such as bow shock, magnetosheath, magnetotail, and strong current sheets are observed in the imposed magnetosphere. We explore variations in atmospheric mass loss rates for different stellar wind strengths to understand the impact of stellar magnetic activity and plasma winds – and their evolution – on (exo)planetary habitability. In order to simulate a case analogous to the present-day Mars, a planet without atmosphere is considered. Our simulations are found to be in good agreement with observational data from Mars Global Surveyor and Mars Atmosphere and Volatile EvolutioN missions and is expected to complement observations from the Emirates (Hope) Mars Mission, China's Tianwen-1 and NASA's Mars 2020 Perseverance mission.

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Tao, Yu, Sylvain Douté, Jan-Peter Muller, Susan J. Conway, Nicolas Thomas, and Gabriele Cremonese. "Ultra-High-Resolution 1 m/pixel CaSSIS DTM Using Super-Resolution Restoration and Shape-from-Shading: Demonstration over Oxia Planum on Mars." Remote Sensing 13, no. 11 (June 3, 2021): 2185. http://dx.doi.org/10.3390/rs13112185.

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We introduce a novel ultra-high-resolution Digital Terrain Model (DTM) processing system using a combination of photogrammetric 3D reconstruction, image co-registration, image super-resolution restoration, shape-from-shading DTM refinement, and 3D co-alignment methods. Technical details of the method are described, and results are demonstrated using a 4 m/pixel Trace Gas Orbiter Colour and Stereo Surface Imaging System (CaSSIS) panchromatic image and an overlapping 6 m/pixel Mars Reconnaissance Orbiter Context Camera (CTX) stereo pair to produce a 1 m/pixel CaSSIS Super-Resolution Restoration (SRR) DTM for different areas over Oxia Planum on Mars—the future ESA ExoMars 2022 Rosalind Franklin rover’s landing site. Quantitative assessments are made using profile measurements and the counting of resolvable craters, in comparison with the publicly available 1 m/pixel High-Resolution Imaging Experiment (HiRISE) DTM. These assessments demonstrate that the final resultant 1 m/pixel CaSSIS DTM from the proposed processing system has achieved comparable and sometimes more detailed 3D reconstruction compared to the overlapping HiRISE DTM.

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Foss, Frederick J., Nathaniel E. Putzig, Bruce A. Campbell, and Roger J. Phillips. "3D imaging of Mars' polar ice caps using orbital radar data." Leading Edge 36, no. 1 (January 2017): 43–57. http://dx.doi.org/10.1190/tle36010043.1.

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Troemner, Matthew, Elham Ramyar, Jonathan Meehan, Benton Johnson, Nima Goudarzi, and Gianluca Cusatis. "A 3D-Printing Centered Approach to Mars Habitat Architecture and Fabrication." Journal of Aerospace Engineering 35, no. 1 (January 2022): 04021109. http://dx.doi.org/10.1061/(asce)as.1943-5525.0001359.

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Wang, Ying, Xuan Feng, Haoqiu Zhou, Zejun Dong, Wenjing Liang, Cewen Xue, and Xiaotian Li. "Water Ice Detection Research in Utopia Planitia Based on Simulation of Mars Rover Full-Polarimetric Subsurface Penetrating Radar." Remote Sensing 13, no. 14 (July 8, 2021): 2685. http://dx.doi.org/10.3390/rs13142685.

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The probe of China’s first Mars exploration mission, Tianwen-1, has been successfully launched. It will carry out scientific exploration on the topography, soil characteristics, water ice, climate, ionosphere, and physical fields of Mars. Different from other rovers landing on the moon and Mars, the Zhurong rover is equipped with a full polarimetric subsurface penetrating radar (FP-SPR) system for the first time. The radar’s mission is to depict the shallow subsurface structure of Mars and search for possible water ice. Therefore, in this paper, a 3D realistic structure model is established and numerically simulated based on the possible subsurface structure of Utopia Planitia (the landing area). Influencing factors such as topographical fluctuations, rocks, water ice, and the variation of dielectric constant of different layers are added to the model. The analysis of the acquired FP-SPR data set shows that the two-dimensional principal component analysis (2D-PCA) method can extract effective reflected signals from the radar data with noise interference and improve the data quality. These clearly imaged targets may be water ice blocks, so the application of 2D-PCA to FP-SPR data increases the imaging quality of suspected water ice targets. The results of this paper are the basis for future processing of the measured FP-SPR data on Mars, which will help to identify more details of subsurface structures.

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Tao, Yu, Siting Xiong, Susan J. Conway, Jan-Peter Muller, Anthony Guimpier, Peter Fawdon, Nicolas Thomas, and Gabriele Cremonese. "Rapid Single Image-Based DTM Estimation from ExoMars TGO CaSSIS Images Using Generative Adversarial U-Nets." Remote Sensing 13, no. 15 (July 22, 2021): 2877. http://dx.doi.org/10.3390/rs13152877.

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The lack of adequate stereo coverage and where available, lengthy processing time, various artefacts, and unsatisfactory quality and complexity of automating the selection of the best set of processing parameters, have long been big barriers for large-area planetary 3D mapping. In this paper, we propose a deep learning-based solution, called MADNet (Multi-scale generative Adversarial u-net with Dense convolutional and up-projection blocks), that avoids or resolves all of the above issues. We demonstrate the wide applicability of this technique with the ExoMars Trace Gas Orbiter Colour and Stereo Surface Imaging System (CaSSIS) 4.6 m/pixel images on Mars. Only a single input image and a coarse global 3D reference are required, without knowing any camera models or imaging parameters, to produce high-quality and high-resolution full-strip Digital Terrain Models (DTMs) in a few seconds. In this paper, we discuss technical details of the MADNet system and provide detailed comparisons and assessments of the results. The resultant MADNet 8 m/pixel CaSSIS DTMs are qualitatively very similar to the 1 m/pixel HiRISE DTMs. The resultant MADNet CaSSIS DTMs display excellent agreement with nested Mars Reconnaissance Orbiter Context Camera (CTX), Mars Express’s High-Resolution Stereo Camera (HRSC), and Mars Orbiter Laser Altimeter (MOLA) DTMs at large-scale, and meanwhile, show fairly good correlation with the High-Resolution Imaging Science Experiment (HiRISE) DTMs for fine-scale details. In addition, we show how MADNet outperforms traditional photogrammetric methods, both on speed and quality, for other datasets like HRSC, CTX, and HiRISE, without any parameter tuning or re-training of the model. We demonstrate the results for Oxia Planum (the landing site of the European Space Agency’s Rosalind Franklin ExoMars rover 2023) and a couple of sites of high scientific interest.

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Liu, Yifan, Andrew F. Nagy, Clinton P. T. Groth, Darren L. DeZeeuw, Tamas I. Gombosi, and Kenneth G. Powell. "3D multi-fluid MHD studies of the solar wind interaction with Mars." Geophysical Research Letters 26, no. 17 (September 1, 1999): 2689–92. http://dx.doi.org/10.1029/1999gl900584.

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Seo, Gwang Hyeok, Hong Hyun Son, and Sung Joong Kim. "Numerical analysis of RBHT reflood experiments using MARS 1D and 3D modules." Journal of Nuclear Science and Technology 52, no. 1 (July 10, 2014): 70–84. http://dx.doi.org/10.1080/00223131.2014.932722.

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Herrero-Gil, Andrea, Javier Ruiz, and Ignacio Romeo. "3D modeling of planetary lobate scarps: The case of Ogygis Rupes, Mars." Earth and Planetary Science Letters 532 (February 2020): 116004. http://dx.doi.org/10.1016/j.epsl.2019.116004.

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Tao, Yu, Jan-Peter Muller, Susan J. Conway, and Siting Xiong. "Large Area High-Resolution 3D Mapping of Oxia Planum: The Landing Site for the ExoMars Rosalind Franklin Rover." Remote Sensing 13, no. 16 (August 18, 2021): 3270. http://dx.doi.org/10.3390/rs13163270.

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We demonstrate an end-to-end application of the in-house deep learning-based surface modelling system, called MADNet, to produce three large area 3D mapping products from single images taken from the ESA Mars Express’s High Resolution Stereo Camera (HRSC), the NASA Mars Reconnaissance Orbiter’s Context Camera (CTX), and the High Resolution Imaging Science Experiment (HiRISE) imaging data over the ExoMars 2022 Rosalind Franklin rover’s landing site at Oxia Planum on Mars. MADNet takes a single orbital optical image as input, provides pixelwise height predictions, and uses a separate coarse Digital Terrain Model (DTM) as reference, to produce a DTM product from the given input image. Initially, we demonstrate the resultant 25 m/pixel HRSC DTM mosaic covering an area of 197 km × 182 km, providing fine-scale details to the 50 m/pixel HRSC MC-11 level-5 DTM mosaic. Secondly, we demonstrate the resultant 12 m/pixel CTX MADNet DTM mosaic covering a 114 km × 117 km area, showing much more detail in comparison to photogrammetric DTMs produced using the open source in-house developed CASP-GO system. Finally, we demonstrate the resultant 50 cm/pixel HiRISE MADNet DTM mosaic, produced for the first time, covering a 74.3 km × 86.3 km area of the 3-sigma landing ellipse and partially the ExoMars team’s geological characterisation area. The resultant MADNet HiRISE DTM mosaic shows fine-scale details superior to existing Planetary Data System (PDS) HiRISE DTMs and covers a larger area that is considered difficult for existing photogrammetry and photoclinometry pipelines to achieve, especially given the current limitations of stereo HiRISE coverage. All of the resultant DTM mosaics are co-aligned with each other, and ultimately with the Mars Global Surveyor’s Mars Orbiter Laser Altimeter (MOLA) DTM, providing high spatial and vertical congruence. In this paper, technical details are presented, issues that arose are discussed, along with a visual evaluation and quantitative assessments of the resultant DTM mosaic products.

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Chen, Zeyu, Bo Wu, and Wai Chung Liu. "Mars3DNet: CNN-Based High-Resolution 3D Reconstruction of the Martian Surface from Single Images." Remote Sensing 13, no. 5 (February 24, 2021): 839. http://dx.doi.org/10.3390/rs13050839.

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Three-dimensional (3D) surface models, e.g., digital elevation models (DEMs), are important for planetary exploration missions and scientific research. Current DEMs of the Martian surface are mainly generated by laser altimetry or photogrammetry, which have respective limitations. Laser altimetry cannot produce high-resolution DEMs; photogrammetry requires stereo images, but high-resolution stereo images of Mars are rare. An alternative is the convolutional neural network (CNN) technique, which implicitly learns features by assigning corresponding inputs and outputs. In recent years, CNNs have exhibited promising performance in the 3D reconstruction of close-range scenes. In this paper, we present a CNN-based algorithm that is capable of generating DEMs from single images; the DEMs have the same resolutions as the input images. An existing low-resolution DEM is used to provide global information. Synthetic and real data, including context camera (CTX) images and DEMs from stereo High-Resolution Imaging Science Experiment (HiRISE) images, are used as training data. The performance of the proposed method is evaluated using single CTX images of representative landforms on Mars, and the generated DEMs are compared with those obtained from stereo HiRISE images. The experimental results show promising performance of the proposed method. The topographic details are well reconstructed, and the geometric accuracies achieve root-mean-square error (RMSE) values ranging from 2.1 m to 12.2 m (approximately 0.5 to 2 pixels in the image space). The experimental results show that the proposed CNN-based method has great potential for 3D surface reconstruction in planetary applications.

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Wong, Julielynn Y. "On-Site 3D Printing of Functional Custom Mallet Splints for Mars Analogue Crewmembers." Aerospace Medicine and Human Performance 86, no. 10 (October 1, 2015): 911–14. http://dx.doi.org/10.3357/amhp.4259.2015.

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Wong, Julielynn Y., and Andreas C. Pfahnl. "3D Printed Surgical Instruments Evaluated by a Simulated Crew of a Mars Mission." Aerospace Medicine and Human Performance 87, no. 9 (September 1, 2016): 806–10. http://dx.doi.org/10.3357/amhp.4281.2016.

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Boesswetter, A., H. Lammer, Y. Kulikov, U. Motschmann, and S. Simon. "Non-thermal water loss of the early Mars: 3D multi-ion hybrid simulations." Planetary and Space Science 58, no. 14-15 (December 2010): 2031–43. http://dx.doi.org/10.1016/j.pss.2010.10.003.

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Bauske, R., A. F. Nagy, D. L. DeZeeuw, T. I. Gombosi, and K. G. Powell. "3D multiscale mass loaded MHD simulations of the solar wind interaction with Mars." Advances in Space Research 26, no. 10 (January 2000): 1571–75. http://dx.doi.org/10.1016/s0273-1177(00)00105-8.

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Kading, Benjamin, and Jeremy Straub. "Utilizing in-situ resources and 3D printing structures for a manned Mars mission." Acta Astronautica 107 (February 2015): 317–26. http://dx.doi.org/10.1016/j.actaastro.2014.11.036.

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Sidiropoulos, Panagiotis, and Jan-Peter Muller. "BATCH CO-REGISTRATION OF MARS HIGH-RESOLUTION IMAGES TO HRSC MC11-E MOSAIC." ISPRS - International Archives of the Photogrammetry, Remote Sensing and Spatial Information Sciences XLI-B4 (June 14, 2016): 491–95. http://dx.doi.org/10.5194/isprs-archives-xli-b4-491-2016.

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Four NASA missions over the last forty years with onboard instruments for high-resolution orbital imaging have achieved both global coverage (with 6m CTX, 20m THEMIS-VIS and >8m Viking Orbiter cameras) as well as imaging with very high resolution in specific regions of interest (e.g. 25cm HiRISE and ≈1.5-12m MOC-NA cameras). Overall, this set of cameras have acquired more than 400,000 high-quality images of Mars with resolution between 25cm/pixel and 100m/pixel (Sidiropoulos and Muller, 2015). On the other hand, ESA has sent the only high-resolution stereo photogrammetric camera around Mars, HRSC onboard the Mars Express spacecraft, which has been mapping the Martian surface since 2004 with a resolution of 12.5 m/pixel (Jaumann et al., 2015). Initially the raw images are combined through an elaborate photogrammetric process to get (single-strip) 3D products (i.e. digital terrain models (DTMs) and derived orthorectified images (ORIs)). However, recently the processing chain has changed, and the single-strip product release was temporarily halted to be replaced by the production and release of mosaics of Mars quadrangles. The first product of this kind is the mosaic for the East part of quadrangle MC11 (i.e. the MC11-E mosaic), a product with 12.5 metres per pixel resolution in the panchromatic image and 50 metres per pixel resolution in the corresponding DTM (Gwinner et al., 2015). <br><br> Such a product provides an excellent basemap to co-register and orthorectify all NASA high-resolution (≤100m/pixel) orbital images. The need for this co-registration to HRSC comes from their poor areo-referencing, which often leads to large deviations (reaching up to several kilometres) between the area they are supposed to image and the area they are actually imaging. After co-registration, all products are projected onto an common 3D coordinate system, which allows an examination of dynamic features of Mars through the changes that happen on its surface. In this work, we present the results of the batch coregistration of all NASA high-resolution orbiter images of MC11-E, i.e. almost 8,000 images in total. This task was conducted with an in-house pipeline which was modified in order to handle the different parameters of the mosaic in comparison to single-strip HRSC products and to process the large input data volumes within a realistic time. An outline of the processing pipeline is given, along with examples of co-registered images and statistics of the co-registration performance. We demonstrate how such a time series representation of the surface will open up new areas for exploration and understanding of the Martian surface.

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Baik, H., and J. Kim. "THE DEVELOPMENT OF 3D SUB-SURFACE MAPPING SCHEME AND ITS APPLICATION TO MARTIAN LOBATE DEBRIS APRONS." ISPRS - International Archives of the Photogrammetry, Remote Sensing and Spatial Information Sciences XLII-3/W1 (July 25, 2017): 1–5. http://dx.doi.org/10.5194/isprs-archives-xlii-3-w1-1-2017.

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The Shallow Subsurface Radar (SHARAD), a sounding radar equipped on the Mars Reconnaissance Orbiter (MRO), has produced highly valuable information about the Martian subsurface. In particular, the complicated substructures of Mars such as polar deposit, pedestal crater and the other geomorphic features involving possible subsurface ice body has been successfully investigated by SHARAD. In this study, we established a 3D subsurface mapping strategy employing the multiple SHARAD profiles. A number of interpretation components of SHARAD signals were integrated into a subsurface mapping scheme using radargram information and topographic data, then applied over a few mid latitude Lobate Debris Aprons (LDAs). From the identified subsurface layers of LDA, and the GIS data base incorporating the other interpretation outcomes, we are expecting to trace the origin of LDAs. Also, the subsurface mapping scheme developed in this study will be further applied to other interesting Martian geological features such as inter crater structures, aeolian deposits and fluvial sediments. To achieve higher precision sub-surface mapping, the clutter simulation employing the high resolution topographic data and the upgraded clustering algorithms assuming multiple sub-surface layers will be also developed.

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Morgan, G. A., B. A. Campbell, L. M. Carter, J. J. Plaut, and R. J. Phillips. "3D Reconstruction of the Source and Scale of Buried Young Flood Channels on Mars." Science 340, no. 6132 (March 7, 2013): 607–10. http://dx.doi.org/10.1126/science.1234787.

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Turbet, Martin, Francois Forget, James W. Head, and Robin Wordsworth. "3D modelling of the climatic impact of outflow channel formation events on early Mars." Icarus 288 (May 2017): 10–36. http://dx.doi.org/10.1016/j.icarus.2017.01.024.

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Lenoir, Benjamin, Donald Banfield, and David A. Caughey. "Accommodation Study for an Anemometer on a Martian Lander." Journal of Atmospheric and Oceanic Technology 28, no. 2 (February 1, 2011): 210–18. http://dx.doi.org/10.1175/2010jtecha1490.1.

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Abstract Measuring the wind velocity and its turbulent fluctuations near the surface of Mars is an important component of the future exploration of Mars, not only to minimize risk in landing, but also to understand some of the most important fundamental processes that dominate Mars’ behavior today. Previous missions have included instrumentation to measure 2D mean winds, but a more sophisticated instrument has been designed that allows for fast, precise 3D measurements of the wind and its turbulent properties. These richer observations raise the question of how best to place such an instrument on a future Martian lander to minimize the flow distortions imposed by the lander, and how to correct for the perturbations that cannot be avoided. To carry out this research, computational fluid dynamic simulations in three dimensions were performed using Fluent, a commercially available software. The first step was to model the conditions at the surface of Mars and, more particularly, the quantities describing the flow in the boundary layer. Using these models, simulations were conducted with two simple shapes for the lander and with eight turbulence conditions representing neutral stability flows in the Martian boundary layer. The results are believed to be generally robust for neutral stability cases because the simulations exhibited little variability as a function of the turbulence conditions. This allowed criteria to be established that would optimize the placement of an anemometer in close proximity to a Martian lander under these conditions. The optimal position that has been derived is an elevation of 55° with a minimum distance from the lander of 0.8 times the characteristic size of the lander.

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Sidiropoulos, Panagiotis, and Jan-Peter Muller. "BATCH CO-REGISTRATION OF MARS HIGH-RESOLUTION IMAGES TO HRSC MC11-E MOSAIC." ISPRS - International Archives of the Photogrammetry, Remote Sensing and Spatial Information Sciences XLI-B4 (June 14, 2016): 491–95. http://dx.doi.org/10.5194/isprsarchives-xli-b4-491-2016.

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Four NASA missions over the last forty years with onboard instruments for high-resolution orbital imaging have achieved both global coverage (with 6m CTX, 20m THEMIS-VIS and >8m Viking Orbiter cameras) as well as imaging with very high resolution in specific regions of interest (e.g. 25cm HiRISE and ≈1.5-12m MOC-NA cameras). Overall, this set of cameras have acquired more than 400,000 high-quality images of Mars with resolution between 25cm/pixel and 100m/pixel (Sidiropoulos and Muller, 2015). On the other hand, ESA has sent the only high-resolution stereo photogrammetric camera around Mars, HRSC onboard the Mars Express spacecraft, which has been mapping the Martian surface since 2004 with a resolution of 12.5 m/pixel (Jaumann et al., 2015). Initially the raw images are combined through an elaborate photogrammetric process to get (single-strip) 3D products (i.e. digital terrain models (DTMs) and derived orthorectified images (ORIs)). However, recently the processing chain has changed, and the single-strip product release was temporarily halted to be replaced by the production and release of mosaics of Mars quadrangles. The first product of this kind is the mosaic for the East part of quadrangle MC11 (i.e. the MC11-E mosaic), a product with 12.5 metres per pixel resolution in the panchromatic image and 50 metres per pixel resolution in the corresponding DTM (Gwinner et al., 2015). <br><br> Such a product provides an excellent basemap to co-register and orthorectify all NASA high-resolution (≤100m/pixel) orbital images. The need for this co-registration to HRSC comes from their poor areo-referencing, which often leads to large deviations (reaching up to several kilometres) between the area they are supposed to image and the area they are actually imaging. After co-registration, all products are projected onto an common 3D coordinate system, which allows an examination of dynamic features of Mars through the changes that happen on its surface. In this work, we present the results of the batch coregistration of all NASA high-resolution orbiter images of MC11-E, i.e. almost 8,000 images in total. This task was conducted with an in-house pipeline which was modified in order to handle the different parameters of the mosaic in comparison to single-strip HRSC products and to process the large input data volumes within a realistic time. An outline of the processing pipeline is given, along with examples of co-registered images and statistics of the co-registration performance. We demonstrate how such a time series representation of the surface will open up new areas for exploration and understanding of the Martian surface.

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Li, Jianing, Shiliang Zhang, and Tiejun Huang. "Multi-Scale 3D Convolution Network for Video Based Person Re-Identification." Proceedings of the AAAI Conference on Artificial Intelligence 33 (July 17, 2019): 8618–25. http://dx.doi.org/10.1609/aaai.v33i01.33018618.

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This paper proposes a two-stream convolution network to extract spatial and temporal cues for video based person ReIdentification (ReID). A temporal stream in this network is constructed by inserting several Multi-scale 3D (M3D) convolution layers into a 2D CNN network. The resulting M3D convolution network introduces a fraction of parameters into the 2D CNN, but gains the ability of multi-scale temporal feature learning. With this compact architecture, M3D convolution network is also more efficient and easier to optimize than existing 3D convolution networks. The temporal stream further involves Residual Attention Layers (RAL) to refine the temporal features. By jointly learning spatial-temporal attention masks in a residual manner, RAL identifies the discriminative spatial regions and temporal cues. The other stream in our network is implemented with a 2D CNN for spatial feature extraction. The spatial and temporal features from two streams are finally fused for the video based person ReID. Evaluations on three widely used benchmarks datasets, i.e.,MARS, PRID2011, and iLIDS-VID demonstrate the substantial advantages of our method over existing 3D convolution networks and state-of-art methods.

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Boivin, A., P. Lai, C. Samson, E. Cloutis, S. Holladay, and F. A. Monteiro Santos. "Electromagnetic induction sounding and 3D laser imaging in support of a Mars methane analogue mission." Planetary and Space Science 82-83 (July 2013): 27–33. http://dx.doi.org/10.1016/j.pss.2013.03.005.

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Kuzmanova, Teodora, Nick Higgett, Mark Sims, Eric Tatham, and Jim Clemmet. "3D technology as an effective tool for reflection simulation: The Beagle 2 lander on Mars." Virtual Creativity 8, no. 2 (December 1, 2018): 159–78. http://dx.doi.org/10.1386/vcr.8.2.159_1.

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Di, Kaichang, Zongyu Yue, Zhaoqin Liu, and Shuliang Wang. "Automated rock detection and shape analysis from mars rover imagery and 3D point cloud data." Journal of Earth Science 24, no. 1 (February 2013): 125–35. http://dx.doi.org/10.1007/s12583-013-0316-3.

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Muller, J. P., Y. Tao, A. R. D. Putri, and S. J. Conway. "3D MULTI-RESOLUTION MAPPING OF MARS USING CASP-GO ON HRSC, CRISM, CTX AND HIRISE." International Archives of the Photogrammetry, Remote Sensing and Spatial Information Sciences XLIII-B3-2021 (June 29, 2021): 667–71. http://dx.doi.org/10.5194/isprs-archives-xliii-b3-2021-667-2021.

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Abstract. Automated large-scale retrieval of stereo photogrammetric DTMs of Mars fall into three categories: use of COTS software such as BAE-SOCET®; private software such as the DLR-VICAR software suite and open source solutions such as the NASA Ames Stereo Pipeline (ASP). We describe here a novel open source system developed on the back of ASP known as CASP-GO (Tao et al., 2018) which has automated and extended ASP to be able to be applied to all modern single-pass or repeat-pass stereo photogrammetric datasets from 21st century systems such as HRSC, CTX and HiRISE, CASP-GO also includes an automated co-registration system which employs HRSC (itself linked to MOLA) as the base-map upon which all other DTMs are co-registered. We show an example here of this automated co-registration system applied to multi-resolution stacks including CRISM images. Several thousand multi-resolution 3D products, Digital Terrain Models (DTMs) and their corresponding orthorectified images (ORIs) have been generated and used in a wide variety of scientific studies, a few examples of which are shown here. Finally, a new method distributing these products providing long-term archiving and ease of access using DOIs is shown employing the ESA-PSA Guest Storage Facility and their corresponding display within the iMars webGIS system.

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Lazure, Pascal, and Franck Dumas. "An external–internal mode coupling for a 3D hydrodynamical model for applications at regional scale (MARS)." Advances in Water Resources 31, no. 2 (February 2008): 233–50. http://dx.doi.org/10.1016/j.advwatres.2007.06.010.

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Widyaningsih, Maura, and Wina Wulandari. "Edukasi Tata Surya Menggunakan Teknologi Augmented Reality." Jurnal Sains Komputer dan Teknologi Informasi 2, no. 1 (November 4, 2019): 29–39. http://dx.doi.org/10.33084/jsakti.v2i1.1161.

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Augmented Reality (AR) adalah teknologi yang menggabungkan objek dunia virtual atau dunia maya dengan dunia nyata. Teknologi ini pada umumnya dikembangkan pada PC dekstop seiring kemajuan teknologi banyak aplikasi yang mengadopsi teknologi ini kedalam sebuah aplikasi smartphone. Penerapan teknologi ini dapat membantu memfasilitasi dalam pembelajaran dengan menampilkan objek 3D dan animasi yang diharapkan membuat lebih memahami materi mengenai tata surya. Media AR ini juga merupakan alat bantu ajar untuk melengkapi metode pembelajaran yang sudah ada sebelumnya agar lebih menunjang program pembelajaran dalam membantu penyampaian materi tentang tata surya. Dalam membangun aplikasi AR menggunakan Unity 3D dan Vuforia untuk membangun aplikasi AR Tata Surya dari tahap awal sampai tahap akhir pembuatan aplikasi, yang mana beberapa tahap tersebut terdiri dari: concept, design, material collecting, assembly, testing, dan distribution. Karakter planet yang dibangun dalam aplikasi ada 9 planet terdiri dari Matahari, Merkurius, Venus, Bumi, Mars, Yupiter, Saturnus, Uranus, Neptunus. Aplikasi tata surya memiliki 2 marker yaitu marker planet dan marker tata surya sebagai penanda untuk menampilkan objek 3D. Aplikasi Augmented Reality ini mendukung pembelajaran pengenalan tata surya berbasis Android, minimal versi 5. Karakter dan navigasi menggunakan layar sentuh untuk memunculkan obyek planet dan penjelasannya

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Cubo-Mateo, Nieves, Sandra Podhajsky, Daniela Knickmann, Klaus Slenzka, Tommaso Ghidini, and Michael Gelinsky. "Can 3D bioprinting be a key for exploratory missions and human settlements on the Moon and Mars?" Biofabrication 12, no. 4 (September 25, 2020): 043001. http://dx.doi.org/10.1088/1758-5090/abb53a.

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Ansan, V., and N. Mangold. "3D morphometry of valley networks on Mars from HRSC/MEX DEMs: Implications for climatic evolution through time." Journal of Geophysical Research: Planets 118, no. 9 (September 2013): 1873–94. http://dx.doi.org/10.1002/jgre.20117.

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Jackson, B. V., J. A. Boyer, P. P. Hick, A. Buffington, M. M. Bisi, and D. H. Crider. "Analysis of Solar Wind Events Using Interplanetary Scintillation Remote Sensing 3D Reconstructions and Their Comparison at Mars." Solar Physics 241, no. 2 (April 2007): 385–96. http://dx.doi.org/10.1007/s11207-007-0276-9.

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42

Kao, Szu-Pyng, Yao-Chung Chen, Fang-Shii Ning, and Yuh-Min Tu. "An LS-MARS method for modeling regional 3D ionospheric electron density based on GPS data and IRI." Advances in Space Research 55, no. 9 (May 2015): 2256–67. http://dx.doi.org/10.1016/j.asr.2015.02.006.

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43

Tao, Y., J. P. Muller, K. Willner, J. Morley, J. Sprinks, C. Traxler, and G. Paar. "3D Data Products and Web-GIS for Mars Rover Mission for Seamless Visualisation from Orbit to Ground-level." ISPRS - International Archives of the Photogrammetry, Remote Sensing and Spatial Information Sciences XL-4 (April 23, 2014): 249–56. http://dx.doi.org/10.5194/isprsarchives-xl-4-249-2014.

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This paper presents a wide range of research and processing results in the area of multi-resolution orbital data co-registration, multiresolution ground 3D reconstruction, and orbit-to-ground data fusion, achieved within the EU-FP7 PRoVisG and PRoViDE project. We focus on three NASA rover missions, MER-A, MER-B, and MSL, to provide examples of automated methods for producing coregistered, multi-resolution 3D products. We highlight the mis-registration discovered between current HiRISE to HRSC datasets, CTX to HRSC and HiRISE to CTX co- results, wide baseline stereo reconstruction results of rover imagery, ground-to-orbit coregistration, i.e. reconstructed wide baseline ground ORI and HiRISE ORI co-registration, and extensive exploitation of the coregistered datasets in visualisation and interactive web-GIS.

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Gupta, Vanshika, Sharad Kumar Gupta, and Jungrack Kim. "Automated Discontinuity Detection and Reconstruction in Subsurface Environment of Mars Using Deep Learning: A Case Study of SHARAD Observation." Applied Sciences 10, no. 7 (March 27, 2020): 2279. http://dx.doi.org/10.3390/app10072279.

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Machine learning (ML) algorithmic developments and improvements in Earth and planetary science are expected to bring enormous benefits for areas such as geospatial database construction, automated geological feature reconstruction, and surface dating. In this study, we aim to develop a deep learning (DL) approach to reconstruct the subsurface discontinuities in the subsurface environment of Mars employing the echoes of the Shallow Subsurface Radar (SHARAD), a sounding radar equipped on the Mars Reconnaissance Orbiter (MRO). Although SHARAD has produced highly valuable information about the Martian subsurface, the interpretation of the radar echo of SHARAD is a challenging task considering the vast stocks of datasets and the noisy signal. Therefore, we introduced a 3D subsurface mapping strategy consisting of radar echo pre-processors and a DL algorithm to automatically detect subsurface discontinuities. The developed components the of DL algorithm were synthesized into a subsurface mapping scheme and applied over a few target areas such as mid-latitude lobate debris aprons (LDAs), polar deposits and shallow icy bodies around the Phoenix landing site. The outcomes of the subsurface discontinuity detection scheme were rigorously validated by computing several quality metrics such as accuracy, recall, Jaccard index, etc. In the context of undergoing development and its output, we expect to automatically trace the shapes of Martian subsurface icy structures with further improvements in the DL algorithm.

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Balme, Matt, Ellen Robson, Rob Barnes, Frances Butcher, Peter Fawdon, Ben Huber, Thomas Ortner, et al. "Surface-based 3D measurements of small aeolian bedforms on Mars and implications for estimating ExoMars rover traversability hazards." Planetary and Space Science 153 (April 2018): 39–53. http://dx.doi.org/10.1016/j.pss.2017.12.008.

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Atienza, Maria-Teresa, Lukasz Kowalski, Sergi Gorreta, Vicente Jiménez, Luis M. Castañer, and Manuel Domínguez-Pumar. "Sliding mode analysis applied to improve the dynamical response of a spherical 3D wind sensor for Mars atmosphere." Sensors and Actuators A: Physical 267 (November 2017): 342–50. http://dx.doi.org/10.1016/j.sna.2017.09.044.

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Tveito, Torbjørn, Juha Vierinen, Björn Gustavsson, and Viswanathan Lakshmi Narayanan. "Planetary radar science case for EISCAT 3D." Annales Geophysicae 39, no. 3 (May 12, 2021): 427–38. http://dx.doi.org/10.5194/angeo-39-427-2021.

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Abstract. Ground-based inverse synthetic aperture radar is a tool that can provide insights into the early history and formative processes of planetary bodies in the inner solar system. This information is gathered by measuring the scattering matrix of the target body, providing composite information about the physical structure and chemical makeup of its surface and subsurface down to the penetration depth of the radio wave. This work describes the technical capabilities of the upcoming 233 MHz European Incoherent Scatter Scientific Association (EISCAT) 3D radar facility for measuring planetary surfaces. Estimates of the achievable signal-to-noise ratios for terrestrial target bodies are provided. While Venus and Mars can possibly be detected, only the Moon is found to have sufficient signal-to-noise ratio to allow high-resolution mapping to be performed. The performance of the EISCAT 3D antenna layout is evaluated for interferometric range–Doppler disambiguation, and it is found to be well suited for this task, providing up to 20 dB of separation between Doppler northern and southern hemispheres in our case study. The low frequency used by EISCAT 3D is more affected by the ionosphere than higher-frequency radars. The magnitude of the Doppler broadening due to ionospheric propagation effects associated with traveling ionospheric disturbances has been estimated. The effect is found to be significant but not severe enough to prevent high-resolution imaging. A survey of lunar observing opportunities between 2022 and 2040 is evaluated by investigating the path of the sub-radar point when the Moon is above the local radar horizon. During this time, a good variety of look directions and Doppler equator directions are found, with observations opportunities available for approximately 10 d every lunar month. EISCAT 3D will be able to provide new, high-quality polarimetric scattering maps of the nearside of the Moon with the previously unused wavelength of 1.3 m, which provides a good compromise between radio wave penetration depth and Doppler resolution.

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Xue, Long, Rong Rong Zhang, Wei Zong, Jia Feng Song, and Meng Zou. "Bionic Design for Mars Sampling Scoop Inspired by Himalayan Marmot Claw." Applied Bionics and Biomechanics 2016 (2016): 1–9. http://dx.doi.org/10.1155/2016/5713683.

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Cave animals are often adapted to digging and life underground, with claw toes similar in structure and function to a sampling scoop. In this paper, the clawed toes of the Himalayan marmot were selected as a biological prototype for bionic research. Based on geometric parameter optimization of the clawed toes, a bionic sampling scoop for use on Mars was designed. Using a 3D laser scanner, the point cloud data of the second front claw toe was acquired. Parametric equations and contour curves for the claw were then built with cubic polynomial fitting. We obtained 18 characteristic curve equations for the internal and external contours of the claw. A bionic sampling scoop was designed according to the structural parameters of Curiosity’s sampling shovel and the contours of the Himalayan marmot’s claw. Verifying test results showed that when the penetration angle was 45° and the sampling speed was 0.33 r/min, the bionic sampling scoops’ resistance torque was 49.6% less than that of the prototype sampling scoop. When the penetration angle was 60° and the sampling speed was 0.22 r/min, the resistance torque of the bionic sampling scoop was 28.8% lower than that of the prototype sampling scoop.

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Wu, Han, Wai-Fan Wong, Zhaohui Yang, Peter B. Wills, Jorge L. Lopez, Yingping Li, Bastian Blonk, Ben Hewett, and Albena Mateeva. "Dual-well 3D vertical seismic profile enabled by distributed acoustic sensing in deepwater Gulf of Mexico." Interpretation 3, no. 3 (August 1, 2015): SW11—SW25. http://dx.doi.org/10.1190/int-2014-0248.1.

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We have acquired and processed 3D vertical seismic profile (VSP) data recorded simultaneously in two wells using distributed acoustic sensing (DAS) during the acquisition of the 2012 Mars 4D ocean-bottom seismic survey in the deepwater Gulf of Mexico. The objectives of the project were to assess the quality of DAS data recorded in fiber-optic cables from the surface to the total depth, to demonstrate the efficacy of the DAS VSP technology in a deepwater environment, to derisk the use of the technology for future water injection or production monitoring without intervention, and to exploit the velocity information that 3D VSP data provide for evaluating and updating the velocity model. We evaluated the advantages of DAS VSP to reduce costs and intrusiveness, and we determined that high-quality images can be obtained from relatively noisy raw 3D DAS VSP data, as evidenced by the well 1 image, probably the best 3D VSP image we have ever seen. Our results also revealed that the direct arrival traveltimes can be used to assess the quality of an existing velocity model and to invert for an improved velocity model. We identified issues with the DAS acquisition and the processing steps to mitigate them and to handle problems specific to DAS VSP data. We described the steps for conditioning the data before migration, reverse time migration, and postmigration processing to reduce noise artifacts. We outlined a novel first-break picking procedure that works even in the absence of a strong first arrival and a velocity diagnosis method to assess and validate velocity models and velocity updates. Finally, we determined potential applications to 4D monitoring of fluid movement around producer or injector wells, identification of active salt movements, and more accurate imaging and monitoring of complex structures around the wells.

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Gastineau, Renaldo, Susan J. Conway, Andreas Johnsson, Jana Eichel, Nicolas Mangold, Peter M. Grindrod, and Tatiana Izquierdo. "Small-scale lobate hillslope features on Mars: A comparative 3D morphological study with terrestrial solifluction lobes and zebra stripe lobes." Icarus 342 (May 2020): 113606. http://dx.doi.org/10.1016/j.icarus.2019.113606.

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Journal articles on the topic 'MARS-3D'

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