Mare volcanism in the lunar farside Moscoviense region: Implication for lateral variation in magma production of the Moon

Abstract

Accurate estimates of the duration and volume of extrusive volcanism of the Moon are essential for understanding the lunar thermal evolution. Here, using new high‐resolution images obtained by the SELENE Terrain Camera, we determined the thicknesses and ages of basalts in Mare Moscoviense, one of the most prominent mare deposits on the farside. Mare volcanism in Mare Moscoviense was active for at least ∼1.5 Ga following the formation of the Moscoviense basin. Mare basalts are estimated to be at least 600 m thick, corresponding to a total volume of 9,500–16,000 km3. The long duration and large volume of extrusive volcanism are plausibly attributed to the thinner crust of the Moscoviense basin relative to those of other farside basins. From a comparison with mare volume within a same‐sized nearside basin, we concluded that a magma production in the farside mantle was 3–10 times less than that of the nearside.

The variety of lithologies in the Yamato-86032 lunar meteorite: Implications for formation processes of the lunar crust

“…Basaltic volcanism in the vicinity of the PKT is generally much younger (Hiesinger et al, 2000). We note that Morota et al (2009) reported mare volcanism on the lunar farside, consistent with the presence of mare basalt clasts in Y-86032 assuming its farside origin, but such volcanism is apt to pre-date that in the vicinity of the PKT. Thus, Y-86032 is most likely derived from outside of the PKT, and probably from a considerable distance from the PKT.…”

Timing and duration of mare volcanism in the central region of the northern farside of the Moon

“…Our results indicated that the mare deposits in the region formed from 3.7 to 2.7 Gyr ago. From model ages for all mare deposits in the region investigated by both our study and previous studies Morota et al, 2009), we found that mare volcanism in this region began at least as early as 3.9 Gyr ago, and continued until ∼2.6 Gyr ago. The comparison of model ages in the region and the SPA basin indicates the simultaneity of the mare volcanism in these regions.…”

“…1). Previous dating of four mare units in Mare Moscoviense using TC image data Morota et al, 2009) revealed that Fig. 9.…”

“…9. Histograms of the model ages of mare deposits in the central region of the northern farside (A), including Lacus Luxuriae, Buys-Ballot, Campbell, Kohlschütter (this study), and those in Mare Moscoviense Morota et al, 2009), within the SPA basin (B), including Poincaré, Ingenii, Antoniadi, Chrétien, Jules Verne, Aitken, Apollo, Von Karman, Von Karman M, Leibnitz, Rumford, Maksutov, and Nishina , and on the nearside (C), including those in Mare Imbrium, Serenitatis, Humorum, Tranquillitatis, Humboldtinum (Hiesinger et al, 2000), Oceanus Procellarum, Mare Nubium, Cognitum, Insularum (Hiesinger et al, 2003), and Mare Fecunditatis (Hiesinger et al, 2006). the lava flows were formed from 3.9 to 2.6 Gyr ago.…”

Science Summary of Kaguya Mission

“…The maximum thickness of lunar crust is found in the Dirichlet-Jackson crater rim of the farside, where the highest altitude was evidently identified by the LALT. The minimum thickness is estimated to be under Mare Moscoviense of the farside, where an almost 0-m thickness of crust was recorded under lava basalt of 600 m thickness 22) . Mantle uplift occurred after formation of the impact basin.…”