Date of Award
12-2025
Document Type
Thesis
Degree Name
Master of Science (MS)
Degree Statement
Master of Science in Geophysics
Department
Department of Geosciences
Committee Chair
Herrick, Robert
Committee Member
Neish, Catherine
Committee Member
Meyer, Franz
Table of Contents
Chapter 1: Introduction
1.1 Background
1.1.1 Crater formation
1.1.3 Mars
1.1.4 Previous studies
1.2 Motivation for this study
Chapter 2: Methods
2.1 Data sets
2.1.1 HiRISE and CTX
2.1.2 MOLA
2.1.3 Robbins and Hynek Crater Database
2.1.4 Tanaka et al. geologic map
2.2 Crater selection
2.3 ISIS processing
2.3.1 CTX image preparation
2.3.2 Creating ancillary files for SOCET SET
2.4 DEM generation
2.4.1 Stereophotogrammetry
2.4.2 ASP DEM generation
2.4.3 SOCET SET DEM generation
2.5 DEM and orthophoto analysis
Chapter 3: Results
3.1 Overview of craters
3.1.1 Utopia Planitia Region
3.1.2 Chryse Planitia Region
3.1.3 Alba Mons Region
3.1.4 Terra Sirenum Region
3.2 Morphological comparisons
3.2.1 Crater rims
3.2.2 Slumps and terraces
3.2.3 Complex crater central structures
Chapter 4: Discussion
4.1 Morphological variation by geologic unit
4.2 Implications for excavation and modification
4.3 Washboarding error removal
Chapter 5: Conclusions.
Abstract
Impact craters on Mars have a wide range of morphologies, and the relationship between the mechanics of their formation and their eventual morphologies is still not completely understood. By examining craters within a narrow diameter range, impact energies are constrained to similar values - enabling focused investigation of target properties and their influence on crater excavation and modification. There is a transition from simple bowl-shaped depressions to complex craters with terraced walls and central floor structures with increasing crater diameter. We analyzed target influences on morphology by examining eleven well-preserved craters of varying morphologies in the 7 to 9 km diameter simple-to-complex transition range on Mars. These craters occur in four geologically diverse regions: Utopia Planitia, Chryse Planitia, Alba Mons, and Terra Sirenum. High-resolution Context Camera (CTX) imagery was used to generate topography of these craters via stereophotogrammetry. Crater rim, wall, and interior differences were studied in detail using High Resolution Imaging Science Experiment (HiRISE) and CTX imagery. Morphometric properties such as depth, diameter, and rim height were measured using GIS software. We found associations between target geology and crater morphology, and evidence that variations in target strength affect the style and amount of crater wall collapse. Wall slumping and terracing alone could not account for the depth reduction observed in several high-rimmed craters; rebound of the crater floor and/or excavation of a different transient cavity shape must be responsible.
Recommended Citation
Dorn, Lindsey, "Examination of differences of similar-sized Martian craters at the simple-complex transition as revealed by high-resolution imaging and stereo-derived topography" (2025). Geosciences. 335.
https://scholarworks.alaska.edu/uaf_grad_geosci/335