Velocity structure and properties of the lunar crust |
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| Authors: | M N Toks?z F Press K Anderson A Dainty G Latham M Ewing J Dorman D Lammlein Y Nakamura G Sutton F Duennebier |
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| Institution: | (1) Dept. of Earth and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, Mass., USA;(2) Lamont-Doherty Geological Observatory, Palisades, New York, USA;(3) University of Hawaii, Honolulu, Hawaii, USA |
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| Abstract: | Lunar seismic data from three Apollo seismometers are interpreted to determine the structure of the Moon's interior to a depth of about 100 km. The travel times and amplitudes ofP arrivals from Saturn IV B and LM impacts are interpreted in terms of a compressional velocity profile. The most outstanding feature of the model is that, in the Fra Mauro region of Oceanus Procellarum, the Moon has a 65 km thick layered crust. Other features of the model are: (i) rapid increase of velocity near the surface due to pressure effects on dry rocks, (ii) a discontinuity at a depth of about 25 km, (iii) near constant velocity (6.8 km/s) between 25 and 65 km deep, (iv) a major discontinuity at 65 km marking the base of the lunar crust, and (v) very high velocity (about 9 km/s) in the lunar mantle below the crust. Velocities in the upper layer of the crust match those of lunar basalts while those in the lower layer fall in the range of terrestrial gabbroic and anorthositic rocks.Lamant-Doherty Geological Observatory Contribution No. 1768. |
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