The modern surface of Mars has widespread substantial deposits of sand-sized sediments that form significant sand dune fields of various typologies and scales (Bridges et al. 2012). With wind forces being the only contemporary (and ancient) driving parameter in moving and altering dunefields and sediment processes across the surface of Mars, understanding the dynamics of surface atmospheric boundary layers in contact with the underlying sediment surface is paramount in any examination of the landform dynamics.
Most research efforts to date have focussed on Mars atmospheric circulation at very large scales, with Global Climate Models (GCMs) (e.g., Leovy and Mintz, 1969; Haberle et al., 1993; Hourdin et al., 1995; Richardson et al., 2002) being the primary guidance. The temporal and spatial scales these models are operating at are good first principles in understanding atmospheric-surface interactions – however, they are much too coarse when we are trying to understand how surface landforms such as dunes are (or have been) moulded into the forms we see them in today.
Understanding aeolian (wind-blown) processes must be approached at a spatial scale of much less than the length of a dune to properly assess dune evolution patterns. Mesoscale climate models (e.g., Rafkin et al., 2001; Toigo and Richardson, 2002; Tyler et al., 2002; Richardson et al., 2007; Spiga and Forget, 2009) have reduced the resolution gap considerably, but their utility chiefly lies at the dunefield scale or larger. However, mesoscale modelling does capture relatively short-timescale wind flow pattern variability due to complex interactions between the atmosphere and regional topography and surface properties. Such variations are believed to be hugely important for localised modifications in dunefields and for the longer term dynamics of the dunes’ migration patterns.
Recent efforts (Jackson et al. 2015) have employed 3-D microscale (<5m resolution) computational fluid dynamics modelling to investigate atmospheric surface interactions and dune surface changes. Mars atmospheric/aeolian model validation can take many forms, but in the context of sand dunes, it typically involves analysing orbital imagery of the dunes and their surroundings to find relevant morphological changes and clues. Additionally, the Curiosity rover has recently passed through a small dunefield in Gale crater (Mars), providing invaluable in situ imagery and meteorological data. Several state-of-the-art numerical atmospheric modelling tools will be used, including a Mars GCM, a regional Mars mesoscale climate model, and a computational fluid dynamics model (OpenFOAM). Geospatial and geomorphic analysis of relevant spacecraft imagery and other observational data will be used to constrain and validate the modelling results.
Overall to combine macro- to meso- to micro-scale airflow modelling for a significantly more realistic approach to modelling the meter-scale fluid dynamics involved in the time-evolution of aeolian features (such as dunes) on Mars.
*Run the global climate model using contemporary Mars parameters, archiving its output for use as the initial state and boundary conditions for mesoscale modelling runs
*Select key sites to apply the integrated modelling approach at, favouring locations with exceptional orbital and/or in situ observational data coverage
*Access and analyse digital terrain models of the Martian surface, integrating them into mesoscale and microscale airflow model runs
*Merge mesoscale climate modelling with CFD microscale simulations through initial state and boundary conditions
*Validate the model results using geomorphic analysis of imagery and in situ datasets
Bridges, N.T., Bourke, M.C., Geissler, P.E., Banks, M.E., Colon, C., Diniega, S., Golombek, M.P., Hansen, C.J., Mattson, S., McEwen, A.S., Mellon, M.T., Stantzos, N., and Thomson, B.J., 2012. Planet-wide sand motion on Mars, Geology, 40(1), 31-34.
Haberle, R.M., Pollack, J.B., Barnes, J.R., Zurek, R.W., Leovy, C.B., Murphy, J.R., Lee, H., and Schaeffer, J., 1993. Mars atmospheric dynamics as simulated by the NASA Ames General Circulation Model, 1. The zonal mean circulation. Journal of Geophysical Research, 98, 3093-3123.
Hourdin, F. and Forget, F., 1995. The sensitivity of the Martian surface pressure and atmospheric mass budget to various parameters: A comparison between numerical simulations and Viking observations. Journal of Geophysical Research, 100 (E3), 5501-5523, doi:10.1029/94JE03079.
Jackson, D.W.T., Bourke, M.C., and Smyth, T.A.G., 2015. The dune effect on sand-transporting winds on Mars. Nature Communications, 6:8796.
Leovy, C. and Mintz, Y., 1969. Numerical simulation of the atmospheric circulation and climate of Mars. Journal of Atmospheric Science, 26 (6), 1167-1190.
Rafkin, S.C.R., Haberle, R.M., and Michaels, T.I., 2001. The Mars Regional Atmospheric Modeling System: Model description and selected simulations. Icarus, 151, doi:10.1006/icar.2001.6605.
Richardson, M.I., Wilson, R.J., and Rodin, A.V., 2002. Water ice clouds in the Martian atmosphere: General circulation model experiments with a simple cloud scheme. Journal of Geophysical Research, 107 (E9), doi:10.1029/2001JE001804.
Richardson, M.I., Toigo, A.D., and Newman, C.E., 2007. PlanetWRF: A general purpose, local to global numerical model for planetary atmospheric and climate dynamics. Journal of Geophysical Research, 112 (E9), doi:10.1029/2006JE002825.
Spiga, A. and Forget, F., 2009. A new model to simulate the Martian mesoscale and microscale atmospheric circulation: Validation and first results. Journal of Geophysical Research, 114 (E2), doi:10.1029/2008JE003242.
Toigo, A.D. and Richardson, M.I., 2002. A mesoscale model for the Martian atmosphere, Journal of Geophysical Research, 107 (E7), doi:10.1029/2000JE001489.
Tyler, D., Barnes, J.R., and Haberle, R.M., 2002. Simulation of surface meteorology at the Pathfinder and VL1 sites using a Mars mesoscale model. Journal of Geophysical Research, 107 (E4), doi:10.1029/2001JE001618.
If the University receives a large number of applicants for the project, the following desirable criteria may be applied to shortlist applicants for interview.
Vice Chancellors Research Scholarships (VCRS)
The scholarships will cover tuition fees and a maintenance award of £14,777 per annum for three years (subject to satisfactory academic performance). Applications are invited from UK, European Union and overseas students.
The scholarship will cover tuition fees at the Home rate and a maintenance allowance of £ 14,777 per annum for three years. EU applicants will only be eligible for the fees component of the studentship (no maintenance award is provided). For Non EU nationals the candidate must be "settled" in the UK.
Completing the MRes provided me with a lot of different skills, particularly in research methods and lab skills.
Michelle Clements Clements - MRes - Life and Health SciencesWatch Video
I would highly recommend Ulster University as you get so much support. Coleraine is a beautiful town and the people are so friendly. It was a really positive experience.
Carin Cornwall - PhD Environmental SciencesWatch Video
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