Abstract
In the present research, we carried out detailed chronological and compositional analyses along with detailed spectral analysis of three unnamed craters on the surface of Mars. Knowledge on chronology/age analysis and compositional analysis of Mars’ surface is essential for future manned and unmanned missions. The study area is near the landing site of previous landed missions, which could be used for future landing. The area is interesting to be studied because of its high elevation in the northeastern side and low elevation in the southern side, consisting of three major geological boundaries, i.e., Hesperian, Noachian, and Amazonian, which are further subdivided into fourteen units. Chronological investigations were carried out using the active machine learning approach and Craterstats 2.0 software, which revealed the age plot of 3.09 ± 0.04 Ga for Amazonian, 3.63 ± 0.0 Ga for Hesperian, and 3.73 ± 0.0 Ga for Noachian geological units, stating that N(1) craters’ density corresponds to the early Amazonian, early Hesperian, and late Noachian/early Hesperian periods according to the established crater density boundaries, respectively. Compact Reconnaissance Imaging Spectrometer for Mars (CRISM)-derived browse products are used for the compositional study of the surface characteristics of Mars. A spectral investigation was performed on an unnamed crater belonging to the Amazonian period, which showed to be majorly composed of oxides as the primary mineral, indicating the spectra of hematite, boehmite, and akaganeite. A Hesperian unit-unnamed crater shows the signature of monohydrated sulfates, melilite, illite, and kaolinite minerals in the region. For the unnamed crater 3, which belongs to the Noachian period, it has diagnostic absorptions of clay minerals in their extracted spectra, indicating the sign of long-term water–rock interactions in the period. Derived chronology results and compositional studies of craters help in better understanding the geological formation units of Mars’ surface.
Highlights
Mars is smaller than Earth, it has the same terrestrial land area
The geology of the study area is composed of three major geological units, i.e., Hesperian, Noachian, and Amazonian units, which have been further subdivided into fourteen geological units such as Ahi (Amazonian and Hesperian impact unit), AHv (Amazonian and Hesperian volcanic unit), Av (Amazonian volcanic unit), HNt (Hesperian and Noachian transition unit), eAb (Early Amazonian basin unit), eHt (Early Hesperian transition unit), eHv (Early Hesperian volcanic unit), eNh (Early Noachian highland unit), IHI (Late Hesperian lowland unit), IHt (Late Hesperian transition unit), INh (Late Noachian highland unit), mAI (Middle Amazonian low-land unit), MNh (Middle Noachian highland unit), and mNhm (Middle Noachian highland massif unit)
To study the age of the major geological units, crater-size frequency data were derived using a novel active machine learning approach, in which the planetary imagery (CTX and Viking 2 image) and Mars Orbiter Laser Altimeter (MOLA) DEM are used for collecting training samples with more automation and better performance
Summary
Mars is smaller than Earth, it has the same terrestrial land area. In its early history, Mars was characterized by high rates of fluvial and geological activity, which includes impact cratering, weathering, erosion, and valley formation (Carr and Head, 2010). We used a CRISM data-derived RGB color composite map and spectral investigation of three unnamed craters belonging to the Amazonian, Hesperian, and Noachian units. We end with a conclusion of study area chronological age analysis using crater size frequency distribution and compositional diversity of craters, which belong to major geological units on Mars’ surface. The MRO’s CRISM has been gathering visible and shortwave infrared-reflectance profiles (0.4–3.9 μm) as far as 2006 (Murchie et al, 2007) Such electromagnetic information on materials has advanced our understanding about the surface of Mars, enabling to determine the identity and analysis of the geological process which have created iron- and manganese-rich facies, evaporites, and hydrated deposits of minerals
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Free) 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
