Impact-Induced Convection and Melt Production in the Lunar Mantle: Source of Mare Basalt

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1 Impact-Induced Convection and Melt Production in the Lunar Mantle: Source of Mare Basalt A. Ghods (Institute for Advanced Studies in Basic Sciences, Zanjan, Iran) J. Arkani-Hamed (McGill University, Montreal, Canada) 1

2 Full Moon as seen from Apollo 11 2

3 3

4 Lunar Basalt Lunar basalt covers about 17% of lunar surfaces, mostly inside impact basins. It is the product of partial melting in the upper km of the Moon. There is a distinct delay between impact basin formation (3.9-4 Ga) and basaltic volcanism that largely occurred Myr after the impacts, maximum flooding was at around 3.6 Ga. 4

5 Lunar Mascons Mascons are associated with intermediate size ( km diameter) impact basins. South Pole Aitken basin (~2500 km diameter) and craters <100 km in diameter have no mascons. Mascons have been mechanically supported for the last about 3.5 Gy. Masoncs require more mass than associated with the estimated mare fillings. 5

6 Current Mascon formation Theories Passive: Partial melting occurred in the deep interior due to global heating of the Moon, and impact basins were favorable low lands for basalt to pond. a. Mascons in the farside, Moskoviense, Mendeleev, Sharonov, Korolev b. Lack of mascons not associated with basins c. Delay in mare flows relative to the formation of the basins d. Lack of mascon associated with South Pole Aitken Basin 6

7 Current Mascon formation Theories Active: Large impacts that produced the basins induced partial melting in the upper mantle of the Moon and resulted in volcanic flow that flooded the basins. a. Depth of partial melting (previous versions) b. Lack of mascon associated with South Pole Aitken Basin 7

8 Impact-Induced Melting Near surface melting (projectile and target) Depressurized melting (upper mantle) Adiabatic melting (Impact-induced convection) 8

9 The Main goal Investigate mantle convection induced by an impact to explain: volcanism within Myr after the formation of a basin enough partial melting in the interior to explain the observed volcanic flow. Strong lithosphere to support mascons 9

10 Effects of Physical parameters We use numerical models to investigate the effects of the following parameters on the melt produced in the lunar interior by the impact-induced mantle convection: 1. Temperature-dependent mantle viscosity 2. Possible KREEP layer beneath the crust 3. Impact size 4. Melt migration in the partially molten region 10

11 Two Stages of Thermal Evolution Pre-impact models (4.5-4 Ga): To provide starting temperature, composition, and melt depletion region in the mantle prior to the impact event at 4 Gyr ago. Post-impact models (after 4 Ga): To determine the amount of melt produced by the impact-induced mantle convection 11

12 The initial temperature and boundary conditions for pre-impact models 12

13 The initial Conditions 1. Pre-impact model: The initial temperature follows the solidus temperature of peridotite, plus a small perturbation to initiate convection The initial velocity is zero 2. Post-impact model: The initial temperature is the spherically symmetric temperature of the pre-impact model plus the impactinduced temperature perturbations modified to account for the isostatic rebound of the mantle The initial velocity is zero 13

14 Description of the Numerical Model (1) Two-Phase flow convection in a cylindrical coordinate Each phase is incompressible, but the entire medium is compressible (Compaction & decompaction processes) Thermal, chemical, and melt retention buoyancy forces Temperature-dependent Viscosity & thermal conductivity Dry peridotite mantle Melt migrates in the partially molten regions 14

15 Description of the Numerical Model (2) The crust and mantle have radioactive heat sources. Thermal conductivity and heat generation of the crust are modified to take into account the effects of ejecta blanket and also the removal of the basin materials. A KREEP layer of 20 km directly beneath the crust 15

16 Laterally averaged temperature profiles in Pre-impact models at 4 Ga (impermeable) 16

17 Effects of mantle viscosity contrast on the melt production (impermeable) 17

18 Rate of melt production in the η=1000 post-impact model (impermeable) 18

19 Impact-induced depressurized melting 19

20 Mantle plume induced by an Imbrium-size impact (impermeable) (4000, 3390, 2790, 2180 Ma) 20

21 Effects of the KREEP layer on melt production (KREEP, T, D at 2180 Ma) 21

22 Effects of melt migration on melt production 22

23 Effect of impact size on melt production (impermeable) 23

24 Why lunar mascons have been supported? 24

25 Conclusions Large impacts produce strong mantle convection and large volumes of melt. The larger is the impact, the shorter is the delay between the impact and the volcanism Decreasing the deep mantle viscosity decreases the melt volume in the post-impact period 25

26 Conclusions Melt migration reduces the time elapsed between start and climax of melt production. The KREEP layer has minor effects on the melt production. The cold and rigid lithosphere beneath the Imbrium-size basins becomes thick enough to support mascons, but that beneath SPA basin remains thin, it cannot support mascon 26

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