Since graduating from my masters I, have been working for a mining company in West Africa. I have had some great times meeting amazing people as well as seeing some amazing geology, at night, during in the dry season, I would get some awe-inspiring views of the rest of the universe.
My photo of Venus and the Milkyway take from Liberia in 2016
From an early age I was always fascinated with dinosaurs and volcanoes, so I tried to find out more about them, a terrible memory for names meant that the dinosaurs fell by the wayside, but my interest in volcanoes grew into wanting to understand how the Earth worked and slowly I turned into a geologist.
A rocky shoreline on Titan ESA/NASA/JPL/University of Arizona
At the same time, the rest of the universe has been there from staring at shooting stars to the Galileo mission, it’s photos of Jupiter and the moons were part of my childhood. In 2005 the photos Huygens probe touchdown on Titan opened my eyes to how surprisingly familiar alien worlds can be (maybe that says something about British seaside holidays).
So after 6 years as a geologist on Earth, I realised one planet was not enough, it’s time for a change of course. I have just started PhD at the Open University where I will be researching Mercury using Nasa’s MESSENGER data to make geological maps of part of the planet, contributing to our knowledge of the smallest planet in the solar system. During the coming weeks, I hope to publish some more specific blogs on Mercury as well as the more general planetary geology and from time to time I’ll post updates on my progress.
My new planet of study Mercury as taken by MESSENGER (JPL)
For the smallest of the planets, Mercury is a surprisingly active place with a complex internal structure and magnetic field, however, it’s tectonics is dominated by its size.
Smaller bodies lose heat a lot faster than bigger bodies, due to a higher ratio of surface area to volume, this means that Mercury has cooled relatively rapidly. As the planet cooled it has shrunk. Estimates for this contraction of its radius range from ~2 – 7 km over its lifetime, whilst this is only 0.2% of its total radius, this equates to its diameter shrinking 44 km at its equator.
Mercury’s surface is a single tectonic plate, it doesn’t have the subduction and rifting zones which can accommodate strain. As the planet has cooled and contracted the crust at the surface has become compressed as the larger diameter crust is pulled in to fit into a smaller area. Rocks when under compression buckle and eventually break and form faults. In the case of Mercury, shallow angle faults known as thrust faults are created. As one part of the crust rides over another it forms cliffs (called “Rupes”) which can be 100’s of km long and several hundred meters high.
Carnegie Rupes, 2 km high wall running diagonally across the image created by a thrust fault (NASA/Johns Hopkins University Applied Physis Laboratory/Carnegie Institution of Washington)
Where multiple faults interact they can produce complex structures. The Great Valley is 1000 km long valley formed from thrust faults which make up either side and has been bent downwards in the middle.
The Great Valley (in Blue) close to Rembrandt basin on Mercury, (Nasa/JHUAPL/CIW/DLR/SI)
Smaller scale scarps have also been identified, whilst smaller (10’s of km long and 10’s of meters high) they are often found cutting across small impact craters and smooth younger planes which means that these features are less than 50 million years old and suggests that Mercury is still tectonically active now.
Smaller scarpes from recent tectonic activity, (NASA/JHUAPL/ Carnegie Institution of Washington/Smithsonian Institution
Whilst there are other features such as some structures on its surface which are linked to thicker patches of crust probably linked to mantle structures Mercury is dominated by the side effects of being a small cooling planet which is still slowly shrinking.