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Windows of Mars: Impact Craters Along the Martian Dichotomy as Markers for Planetary Evolution

Persson, Frida LU (2026) In Dissertations in Geology at Lund University GEOL02 20261
Department of Earth and Environmental Sciences (MGeo)
Abstract
When an impact excavates and modifies the Martian surface, by bringing deeper lying material to the surface, it opens a window into past geology. Trying to understand surface properties on Mars and how target material behaves during impact requires a multi-view approach. Previous research has focused mainly on ejecta emplacement and morphologies as a proxy for surface properties. However, interior morphological structures, such as central uplifts and terraces of complex craters might hold important information about the target material as well. With the use of JMARS and HiRISE imaging, such structures have been analysed in this work. The focus area lies around the Martian dichotomy, a crustal boundary separating old, heavily cratered... (More)
When an impact excavates and modifies the Martian surface, by bringing deeper lying material to the surface, it opens a window into past geology. Trying to understand surface properties on Mars and how target material behaves during impact requires a multi-view approach. Previous research has focused mainly on ejecta emplacement and morphologies as a proxy for surface properties. However, interior morphological structures, such as central uplifts and terraces of complex craters might hold important information about the target material as well. With the use of JMARS and HiRISE imaging, such structures have been analysed in this work. The focus area lies around the Martian dichotomy, a crustal boundary separating old, heavily cratered highlands in the south from smooth lowlands composed of younger deposits in the north. The area of interest ranges from approximately 58°N to 4°N and 58°E to 40°E but future studies may further investigate the same area and other areas with similar characteristics. Three impact craters have been chosen for investigation: (1) the Quenisset crater, located in the Southern highlands, (2) the Moreux crater along the Martian dichotomy and (3) an unnamed crater in the Northern lowlands. All craters show structures and features formed by water, highlighting the importance of understanding how water-rich material behaves during impact. Another marker for surface properties is the size difference of craters which might reveal what the target material is made off as it varies between e.g. sedimentary deposits and crystalline bedrock. (Less)
Abstract (Swedish)
När ett nedslag gräver upp och modifierar Mars yta, genom att medföra material från djupare delar till ytan, öppnar det fönster ner till äldre geologi. Att försöka förstå ytegenskaper på Mars och hur källmaterialet beter sig vid ett nedslag kräver en metod från flera perspektiv. Tidigare forskning har främst fokuserat på ejecta och ejektamorfologi som en indikator på ytegenskaper. Däremot kan även inre morfologiska strukturer, såsom centrala upphöjningar och terrasser i komplexa kratrar bära på viktig information om källmaterialet. Med hjälp av JMARS och HiRISE-bilder, kan sådana strukturer bli analyserade i detta arbete. Fokusområdet ligger runt den marsianska dikotomin, en gräns som separerar gammalt högland täckt av kratrar i söder,... (More)
När ett nedslag gräver upp och modifierar Mars yta, genom att medföra material från djupare delar till ytan, öppnar det fönster ner till äldre geologi. Att försöka förstå ytegenskaper på Mars och hur källmaterialet beter sig vid ett nedslag kräver en metod från flera perspektiv. Tidigare forskning har främst fokuserat på ejecta och ejektamorfologi som en indikator på ytegenskaper. Däremot kan även inre morfologiska strukturer, såsom centrala upphöjningar och terrasser i komplexa kratrar bära på viktig information om källmaterialet. Med hjälp av JMARS och HiRISE-bilder, kan sådana strukturer bli analyserade i detta arbete. Fokusområdet ligger runt den marsianska dikotomin, en gräns som separerar gammalt högland täckt av kratrar i söder, från ett jämnare lågland bestående av yngre avlagringar, i norr. Området av intresse sträcker sig ungefär från 58°N to 4°N and 58°E to 40°E men framtida studier borde vidare undersöka samma område och områden med liknande karaktäristik. Tre impaktkratrar har blivit valda att undersöka: (1) Quenisset, lokaliserad i södra höglandet, (2) Moreux vid marsianska dikotomin, och (3) en namnlös krater i norra låglandet. Alla kratrar visar strukturer och särdrag format av vatten, vilket understryker vikten av att förstå hur vattenrika material beter sig vid nedslag. En annan markör för ytegenskaper är storlekskillnaden mellan kratrarna som kan avslöja vad källmaterialet består av, då det skiljer sig mellan till exempel sedimentära avlagringar och kristallin berggrund (Less)
Popular Abstract
Our neighbouring red planet is quite unique in terms of its surface and has always been of great research interest. In early Martian history there was flowing water on the surface and Mars was, like Earth, geologically active. However, as time went on, the water seemed to disappear, and the geological processes seemed to stop. So how can we then know what Mars looked like in the past and why is it important?
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author
Persson, Frida LU
supervisor
organization
course
GEOL02 20261
year
type
M2 - Bachelor Degree
subject
keywords
Martian dichotomy, Surface properties, Impact cratering, Crater morphology
publication/series
Dissertations in Geology at Lund University
report number
731
language
English
id
9234118
date added to LUP
2026-06-25 12:41:58
date last changed
2026-06-25 12:41:58
@misc{9234118,
  abstract     = {{When an impact excavates and modifies the Martian surface, by bringing deeper lying material to the surface, it opens a window into past geology. Trying to understand surface properties on Mars and how target material behaves during impact requires a multi-view approach. Previous research has focused mainly on ejecta emplacement and morphologies as a proxy for surface properties. However, interior morphological structures, such as central uplifts and terraces of complex craters might hold important information about the target material as well. With the use of JMARS and HiRISE imaging, such structures have been analysed in this work. The focus area lies around the Martian dichotomy, a crustal boundary separating old, heavily cratered highlands in the south from smooth lowlands composed of younger deposits in the north. The area of interest ranges from approximately 58°N to 4°N and 58°E to 40°E but future studies may further investigate the same area and other areas with similar characteristics. Three impact craters have been chosen for investigation: (1) the Quenisset crater, located in the Southern highlands, (2) the Moreux crater along the Martian dichotomy and (3) an unnamed crater in the Northern lowlands. All craters show structures and features formed by water, highlighting the importance of understanding how water-rich material behaves during impact. Another marker for surface properties is the size difference of craters which might reveal what the target material is made off as it varies between e.g. sedimentary deposits and crystalline bedrock.}},
  author       = {{Persson, Frida}},
  language     = {{eng}},
  note         = {{Student Paper}},
  series       = {{Dissertations in Geology at Lund University}},
  title        = {{Windows of Mars: Impact Craters Along the Martian Dichotomy as Markers for Planetary Evolution}},
  year         = {{2026}},
}