Dome Dune

  • Eric J. R. Parteli
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Circular to elliptical, relatively flat mounds often without external slip faces.



On Mars, they are 40–100 m across and <30 m high with 100–1,000 m spacing (De Hon 2006).


They may form when wind velocities are low (Pye and Tsoar 1990 and references therein). Dome dunes may transform into other dune forms. Computer modeling (Parteli et al. 2009) suggests that dome dunes may form if the wind oscillates between two prevailing directions with a period shorter than 0.01 % of the dune’s turnover time, which is the time needed for the dune to cover a distance equal to its own size.

Domes may also be dunes smaller than the critical size for a barchan development where slip faces and horns are not able to evolve (Parteli 2007).

On Mars, dome dunes are smaller (<100 m across) than adjacent barchans (>100 m) (De Hon 2006; Fig. 1). The occurrence of dome dunes in Chasma Boreale in the northern polar region of Mars might be...


Carbon Dioxide Geographical Information Wind Velocity Polar Region Sand Dune 
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© Springer Science+Business Media New York 2014

Authors and Affiliations

  1. 1.Institute for Multiscale SimulationUniversity of Erlangen-NurembergErlangenGermany