Polygonal Impact Craters in the Thaumasia Minor, Mars: Role of Pre-existing Faults in Their Formation
- 16 Downloads
Terrestrial planets, dwarf planets and moons (natural satellites) in the solar system have undergone meteoric impacts since their formation. The craters formed due to such impacts may show various geometric shapes. Formation of impact craters that are polygonal in shape is controlled by the presence of pre-existing tectonic features in the area of impact. Thaumasia Minor, the easternmost part of Thaumasia Planum of Mars, has ~ E–W-trending grabens and ~ N–S-trending wrinkle ridges, similar to the rest of Thaumasia Planum. The massive weight of the Tharsis Montes, lying to the northwest of Thaumasia, is considered as the primary cause for the extensional and compressional fractures developed in multiple temporal phases throughout the geological history of Mars. Five such polygonal impact craters in the southern Thaumasia Minor were compared with the visible expressions of tectonic planes in the region. The straight segments of the craters are also used as a proxy to reveal the presence and possible orientations of buried weak planes in the region.
KeywordsPolygonal impact crater Wrinkle ridge Graben Pre-existing faults Fault reactivation
A. Kundu, N. Dasgupta and D. Dasgupta acknowledge a research Grant (DOS Sanction Order No.: No. B.19013/10/2016-Sec.2) under MOM-AO program of the Space Science Program Office, Indian Space Research Organisation.
- Anderson, R. C., Dohm, J. M., Golombek, M. P., Haldemann, A. F., Franklin, B. J., Tanaka, K. L., et al. (2001). Primary centers and secondary concentrations of tectonic activity through time in the western hemisphere of Mars. Journal of Geophysical Research: Planets, 106(E9), 20563–20585.CrossRefGoogle Scholar
- Andrews-Hanna, J. C. (2012). The formation of Valles Marineris: 2. Stress focusing along the buried dichotomy boundary. Journal of Geophysical Research, Planets, 117(E4).Google Scholar
- Arya, A. S., Sarkar, S. S., Srinivas, A. R., Moorthi, S. M., Patel, V. D., Singh, R. B., et al. (2015). Mars Colour Camera: The payload characterization/calibration and data analysis from Earth imaging phase. Current Science, 00113891, 109(6).Google Scholar
- Baker, V. R., Maruyama, S., & Dohm, J. M. (2007). Tharsis super plume and the geological evolution of early Mars. In Super plumes: Beyond plate tectonics (pp. 507–522). Dordrecht: Springer.Google Scholar
- Cole, H. M., & Andrews-Hanna, J. C. (2017). The anatomy of a wrinkle ridge revealed in the wall of Melas Chasma, Mars. Journal of Geophysical Research: Planets, 122(5), 889–900.Google Scholar
- Epard, J. L., & Groshong, R. H., Jr. (1993). Excess area and depth to detachment. AAPG Bulletin, 77(8), 1291–1302.Google Scholar
- Garvin, J. B., Sakimoto, S. E. H., & Frawley, J. J. (2003). Craters on Mars: Global geometric properties from gridded MOLA topography (abstract #3277). In 6th International conference on Mars. Google Scholar
- Jaumann, R., Neukum, G., Behnke, T., Duxbury, T. C., Eichentopf, K., Flohrer, J., et al. (2007). The high-resolution stereo camera (HRSC) experiment on Mars Express: Instrument aspects and experiment conduct from interplanetary cruise through the nominal mission. Planetary and Space Science, 55(7–8), 928–952.CrossRefGoogle Scholar
- Kring, D. A., & Cohen, B. A. (2002). Cataclysmic bombardment throughout the inner solar system 3.9–4.0 Ga. Journal of Geophysical Research, Planets, 107(E2).Google Scholar
- Malin, M. C., Bell, J. F., Cantor, B. A., Caplinger, M. A., Calvin, W. M., Clancy, R. T., et al. (2007). Context camera investigation on board the Mars Reconnaissance Orbiter. Journal of Geophysical Research, Planets, 112(E5).Google Scholar
- Montgomery, D. R., Som, S. M., Jackson, M. P., Schreiber, B. C., Gillespie, A. R., & Adams, J. B. (2009). Continental-scale salt tectonics on Mars and the origin of Valles Marineris and associated outflow channels. Geological Society of America Bulletin, 121(1–2), 117–133.Google Scholar
- Öhman, T., Aittola, M., Kostama, V. P., & Raitala, J. (2005). The preliminary analysis of polygonal impact craters within greater Hellas region, Mars. In Impact tectonics (pp. 131–160). Berlin: Springer.Google Scholar
- Peterson, G., Johnson, C., Byrne, P. K., Phillips, R. J., & Neumann, G. A. (2016), February. Depth of faulting in Mercury’s northern Hemisphere from Lobate Scarp Morphology. In AGU Fall Meeting Abstracts. Google Scholar
- Pike R. (1980). Control of crater morphology by gravity and target type: Mars, Earth, Moon. In Proceedings, 11th lunar and planetary science conference (pp. 2159–2189).Google Scholar
- Schultz, P. H. (1976). Moon morphology. Austin: University of Texas Press.Google Scholar
- Tanaka, K. L., Skinner Jr, J. A., Dohm, J. M., Irwin, III, R. P., Kolb, E. J., Fortezzo, C. M., Platz, T., Michael, G. G., & Hare, T. M. (2014). Geologic map of Mars. U.S. Geol. Surv. Sci. Invest. Map, 3292, scale 1:20,000,000. https://doi.org/10.3133/sim3292.
- Williams, N. R., Shirzaei, M., Bell III, J. F., & Watters, T. R. (2015). December. Inverse modelling of wrinkle ridge structures on the Moon and Mars. In AGU Fall Meeting Abstracts. Google Scholar