D.J. Applebee | Geology Reports

USGS1993

Geologic map of science study area 8, Apollinaris Patera region of Mars

Volcanoes are among the most imposing and geologically interesting features on Mars. Nearly 60 percent of the planet’s surface is covered by volcanic rocks dating from the Early Noachian to Late Amazonian Epochs (Tanaka and others, 1988). This map of the volcano Apollinaris Patera and surrounding area is one of a series of large-scale (1:500,000) geologic maps initiated by the National Aeronautics and Space Administration to investigate areas of particular scientific interest. The areas selected for mapping contain candidate landing sites for future sample-return missions to Mars (fig. 1). The map area is considered to be of special scientific interest for several reason: (1) it includes the prominent volcano Apollinaris Patera, a type of volcanic edifice unusual on Mars in that it is not associated with significant faulting and is partly surrounded by a basal scarp similar to that of its much larger counterpart at the base of Olympus Mons; (2) it is located in a major transition zone between ancient highlands to the south and much of the younger lowland plains to the north; (3) rocks have different origins and a ide range of ages occurring in the area; and (4) erosional processes associated with fluvial, volcanic, and eolian activity have shaped the terrain. The map area’s potential as a landing site is increased by its extensive, relatively smooth areas at low elevation (0 to 1 km), which would permit access by an automated vehicle and atmospheric breaking by a landing craft.

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USGS1991

Geologic maps of science study area 3, Olympus Rupes, Mars

This map is one in a series of 1:500,000 -scale geologic maps initiated by the National Aeronautics and Space Administration to investigate areas of particular scientific interest on Mars. Olympus Mons is the largest known volcanic construct in the Solar System; it is more than 600 km across and more than 27 km above datum (fig, 1, sheet 1). The volcano and the great scarp that bounds it have been the subject of much scientific controversy. Although i t has been possible to generate an empirical model that closely resembles Olympus Mons (fig. 2, sheet 1), the dynamics of scarp formation are still unproven . The scarp area is thus a logical selection as a scientific study area. It has also been designated as a candidate site for a proposed lander/rover/sample-return mission to Mars (fig. 1, sheet 2) not only because the site may provide information about the origins of the scarp and the evolution of Olympus Mons, but also because the rocks of widely diverse ages may be studied from the samples collected from talus at the base of the scarp.

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