SHARAD Radar investigations into the initiation of spiral troughs on Planum Boreum, Mars

Recent evidence demonstrates that the prominent spiral troughs of the North Polar Layered Deposits (NPLD) on Mars are not young features, having persisted and evolved during accumulation of more than 500 meters of ice [Smith and Holt, Nature, 2010]. Because of the rich stratigraphy in the NPLD, determining the processes controlling trough formation and evolution is an important step in understanding the history of ice and climate on Mars. Multiple periods of trough initiation are observed in radar data collected by the Shallow Radar (SHARAD) instrument on Mars Reconnaissance Orbiter; however, the mechanism behind trough initiation is still a mystery. Discrete radar reflectors can be associated with the onset of spiral troughs because of their stratigraphic relationships: below the reflectors the troughs do not exist, and above the troughs begin to take shape. To address the question of trough formation we have mapped these reflectors, which are assumed to represent isochrones, in more than 400 SHARAD observations throughout the NPLD. Taken together these represent the surfaces where troughs initiated, i.e. surfaces that lie directly below the first appearance of troughs. When observation geometries are favorable, we find that the onset of each trough rests on a change in slope usually at the base of a buried erosional scarp. The underlying layers end abruptly at the scarps rather than diminish or pinch out with distance, suggesting that the NPLD underwent cap-wide erosion predating trough formation. This surface morphology provides the initial conditions needed to form troughs from the combination of deposition and katabatic winds affected by surface slope. Radar observations indicate that the troughs initiated and evolved with approximately the same wavelength as can be measured today. Thus proposed hypotheses of small bedforms growing into larger wavelength structures is not supported. Locally, the unconformable contact between younger, trough-related material and older eroded surfaces is exposed at the surface. Neither the younger nor older exposed layers show small-scale bedforms, supporting this conclusion. At least two initiation surfaces can be observed in the radar data within the uppermost 500 m of the NPLD. Alternating periods of erosion and deposition are predicted to result from large changes in obliquity and insolation at the Martian north pole [Laskar et al., Nature, 2004], suggesting that trough initiation may be related to orbital forcing.