STRUCm MODEL OF THE IMBRIUM BASIN, R. A. De Hon, Department of Geosciences, Northeast Louisiana University, Monroe, LA 71209 A long history of geologic observation and speculation has not produced a fully comprehensive and acceptable model for the origin of the Imbrim Basin (1-4). Wkile an impact origin for the basin is generally accepted, controversy still exists concerning the detailed internal structure and the origin of some of the most prominent features. An isopach map of the mare basalt within the basin provides improved understanding of the location and configuration of the salient buried topography. However, a map, based entirely on estimates of basalt thickness at partially buried craters (5), is not fully satisfactory due to the small number of clustered data points. The data provide restrictions to possible basin configurations. Inclusion of less quantitative, but nevertheless real-, data limits allows construction of an improved model of the internal structure of the basin. As with any major circular basin, the depth of the basin precludes pre- servation of a significant population of buried craters due to the low cra- ter density and inherent depth of burial, The isopach mp constructed for involves interpretation of sparse crater data and correlation of non-numerical thickness indicators to establish trends and overall thick- ness distributions. Data and observations which restrict the model consist of the following: 1) basalt thickness derived from buried craters; 2) loca- tion of the mare contact with terra materials; 3) crest line of the encir- cling outer mountain ring; and 4) location of massifs and mare ridges marking the location of the inner basin ring. The isopach map (Fig. 1) is characterized by a central thick lens of basalt surrounded by a discontinuous ring of moderately thick basalt. The isopach map is subtracted from a 12th degree harmonic model of surface topo- graphy (Fig. 2). The paleomorphologic map exhibits a deep central basin surrounded by an uneven shelf. An inner raised ring concentric to the outer basin rim separates the deep basin from the shelf. The outer ring of the Imbrium Basin is approximately 1350 km in dia- meter (less in the region). The inner ring is approximately 700 km in diameter. The southeastern rim crest (Montes Apeminus) averages 9700 m in elevation. The surrounding surface outside the basin averages 6000 m in elevation. The total thickness of the mare basalt in the central basin can not be measured directly, but it is probably in the range of 1500- 2000 m thick (8). Hence, the i.nner basin floor my be estimated at 3200 m. Thus the total relief of the basin before burial is on the order of 6500 rn. The resulting topographic model of the original Imbrim Basin is that of a two-ringed basin. The outer ring is composed of high standing terra of Montes Carpatus, , Montes Caucasus, Montes Alpes, and rugged terra north and northeast of the basin. The inner ring is marked by the mare ridge trend and isolated massifs such as Montes Spitzbergensis, Nons Pico, and PiIons La Hire.

0 Lunar and Planetary Institute Provided by the NASA Astrophysics Data System STRUCTURAL MODEL OF THE lTvlBRIUM BASIN

De Hon, R. A.

The outer ring of the basin is offset between the Montes Alpes and Montes Caucasus. This offset is presently interpreted as a tear fault (7). Presumedly the offset is caused by an uneven roll-back of the rim flap during excavation of the crater. Similarly, incomplete excavation results in remnant material of the Apennine Bench which rises above the basalt fill on the floor of the basin shelf.

The rim of the IrriPrium Basin is broken and discontinuous. The 260 km diameter Iridum Basin is superposed on the northwest Jmbrium shelf. The Iridum rim overlaps both the inner and outer rings of the lmbrium Basin. Large discontinuities in the Imbrium outer ring mark the locations of inter- action between Imbrium excavation and pre-existing basins. In the east, a small gap between the Montes Apenninus and Montes Caucasus is formed where the Imbrium Basin impinges on the Serenitatis Basin. In the south, a break between the Montes Apenninus and Montes Carpatus marks the infringement of the Imbrium Basin on the older Stadius-Aestuum Basin. The largest break in the Imbrium rim occurs in the southwest where a full one-fifth of the rim is apparently submerged beneath mare basalts. Isopach mpping reveals a here- tofore unrecognized basin 600 km in diameter centered just beyond the nomi- nal basin rim in this locality.

In a strict sense the model is independent of the basin fomtion mech- anism. However, the model does not require faulting along the Apenninus Front to form the outer ring, and it is consistant with an impact origin for the basin and outer ring (9 and 10). It is reasonable that the recon- structed basin configuration is an equilibrium form resulting from isostatic adjustment prior to emplacement of the mare basalts.

References (1) Gilbert, G. K. (1893) Philos. Soc. Washington k11. , 12, 241-292. (2) Baldwin, R. B. (1949) in The Face of the , Univ. of Chicago Press. (3) Hartm, W. K. and ~uzer,G. P. (1962) Ariz. Univ. Lunar and Planetary Lab. ~orm.,1, 13,- 51166. (4) Spurr, J. E. (1945) in Geology Applied to Selenology, Science Press. (5) De Hon, R. A. (1974)-oc. Lunar Sci. Conf'. V, 244-259. (6) Bills, B. G. and Ferrari, A. J. (1977) Icarus, 82, 244-259. (7) McCauley et al. (1979) Icarus, in press. (8) Thurber, C. H. and Solomon, S. C. (1978) Proc. Lunar and Planetary Sci. Conf. IX, in press. (9) Wilhelms, D. E. et al. (1977) -in Impact and Explosion Cratering, Pergamon Press, 539-562. - (10) Hodges, C. A. and Wilhelms, D. E. (1978) Icarus, 34, 294-323.

0 Lunar and Planetary Institute Provided by the NASA Astrophysics Data System STRUCTURAL MODEL OF THE IMBRIUM BASIN De Hon, R. A.

Figure 1. Isopach map of Mare Imbrium basalt. Isopach interval is 0.5 km. Crosses mark the location of measured basalt thickness. Diagonal lines indicate region of unknown values.

Figure 2. Paleotopography of the 1mbriu.m Basin. Contour inter- val is 0.5 km. Datum is 1730 km radius vector. Dots mark crests of inferred rings. Dashed lines are "tear faultst'in rim flap.

0 Lunar and Planetary Institute Provided by the NASA Astrophysics Data System