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).
- De Hon RA (2006) Transitional dune forms on Mars. Lunar Planet Sci Conf XXXVII, abstract #1361, Houston. http://elib.uni-stuttgart.de/opus/volltexte/2007/2964/
- Parteli EJR (2007) Sand dunes on Mars and on Earth. Dissertation. Institut für Computerphysik der Universität StuttgartGoogle Scholar
- Schatz V, Tsoar H, Edgett K, Parteli EJR, Herrmann HJ (2006) Evidence for indurated sand dunes in the Martian north polar region. J Geophys Res Planet 111. doi:10.1029/2005JE002514Google Scholar
- Tirsch D (2008) Dark dunes on Mars. Dissertation, Freie Universität Berlin. http://www.diss.fu-berlin.de/diss/receive/FUDISS_thesis_000000008848