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What New Can LRO Tell Us About Lunar Thermal Evolution, Interior Structure and Dynamics?

Introduction: Lunar surface features imaged from space can provide important new constraints on lunar structure and dynamics over the history of the Moon. While the surface of the Moon is dominated by impact craters and basins, tectonic landforms attest to basin localized stresses and global crustal contraction resulting from slow cooling of the lunar interior (see [1] and references therein). In addition, seismometers em-placed during the Apollo era recorded numerous moonquakes (see [2, 3] and references therein). While the maximum recorded body wave magnitude is around 5, it is conceivable that surface features associated with known moonquakes may be identified. Wrinkle ridges, graben and lobate scarps: As shown in the Figure 1, tectonic landforms are mostly concentrated in the mare on the lunar nearside. The wrinkle ridges and graben appear to associated mostly with emplacement and subsidence of mare basalts, while the lobate scarps, although few in number, are less clearly associated with the maria and may express global tectonic stresses. Lunar wrinkle ridges are complex structures involving thrust faults and folds resulting from compres-sional stresses in the maria. They are found in mare basalts and consist of a broad arch and a superimposed narrow ridge. While sinuous rilles in the maria are believed to be volcanic in origin, linear and arcuate rilles are graben, resulting from extensional tectonics. The wrinkle ridges and graben appear to result from basin-localized compressional and extensional tecton-ics associated with subsidence and flexure. Unlike the wrinkle ridges and graben, the lobate scarps are not directly associated with the mare basins and may have origins similar to those for parallel land-forms on Mercury and Mars. Lunar lobate scarps are generally asymmetic and are often lobate and segmented. With lengths of only a few tens of kilometers and maximum relief of only a few tens of meters, they are generally significantly smaller than their counterparts on Mercury and Mars. Lunar lobate scarps appear to be the result of shallow thrust faults, and are sometimes associated with wrinkle ridges, although they are found predominantly in the lunar highlands. The compressional stresses that formed the lobate scarps may have resulted from thermal stresses due to global cooling. If this model is correct, the spatial distribution and scale of the scarps may have important