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Moon's Greatest Hits Since 2000

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Moon's Greatest Hits Since 2000 Moon’s Greatest Hits Since 2000 Misions to the Moon Mission Launch Date End Date Clementine 25 Jan. 1994 5 May 1994 Lunar Propsector 7 Jan. 1998 31 July 1999 SMART-1 27 Sept. 2003 3 Sept. 2006 Kaguya (SELENE) 14 Sept. 2007 10 June 2009 Chang’e 1 24 Oct. 2009 1 Mar. 2010 Channdrayaan-1 22 Oct. 2008 31 Aug. 2009 LRO 17 June 2009 STILL ACTIVE LCROSS 17 June 2009 9 Oct. 2009 ARTEMIS 20 July 2009* STILL ACTIVE Chang’e 2 1 Oct. 2010 April 2012 GRAIL 10 Sept. 2011 17 Dec. 2011 LADEE 6 Sept. 2013 17 Apr. 2014 Chang’e 3 1 Dec. 2013 STILL ACTIVE * Actual launch date = 17 Feb. 2007 as part of THEMIS mission. Date represents start of operations once three satellites arrived at the Moon Non-Representivity of Apollo Sites Lunar Terranes [Jolliff et al. (2000) JGR 105, 4197] • Apollo sites close to terrane boundaries. • Samples contain PKT signature. • Apollo sample collection is not representative of the lunar compositional diversity. Giguere et al. (2000) MaPS 35, 193 Lunar Topography Kaguya (SELENE) Chang’e-1 LRO (LOLA) Hi-Resolution Lunar Gravity GRAIL Gravity map, updating the Kaguya and Chang’E-1 gravity maps. Kaguya: Namiki et al., (2009) Science 323, 900- 905. Free Air Chang’e-1: Yan et al. (2010) Advances in Space Bouger Research 46, 50-57. GRAIL: Zuber et al. (2013) Science 339, 668-672. Chang’E-1 Microwave Emission Day Night Daytime (upper panel) and nighttime (lower panel) maps of the 3 GHz channel, for −60° latitude 60° and −180° longitude 180°. Bright/dark show high/low values; in the daytime the maximum and minimum values of are 9 K and −10 K, respectively, while in the nighttime panel they are 7 K and −10 K. Chan et al. (2010) EPSL 295, 287-291. Global Neutron Maps 1˚ x 1˚ of fast neutron flux (in counts per second) from the lunar surface measured by LEND SHEN-N detector. Litvak et al. (2012) J. Geophys. Res. 117 E00H22, doi:10.1029/2011JE003949 Reinterpretation of the Apollo Seismic Data Thinning of the nearside crust! Toksoz et al. (1972) Science 176, 1012-1016; (1974) Rev. Geophys. Space Phys. 12, 539-567): 60-65 km Khan & Mosegaard (2002) JGR 107, doi:10.1029/2001JE001658: 45 km Lognonné et al. (2003) Earth Planet. Sci. Lett. 211, 27-44: 30 km Chenet et al. (2006) Earth Planet. Sci. Lett. 243, 1-14: 31-38 km Wieczorek et al. (2013) Science 339, 671-675: 34-43 km Detection of the Lunar Core? Weber et al. (2011) Science 331, 309-312 Evidence for a Liquid Lunar Core – Laser Ranging Lunar rotation displays a strong source of dissipation which is compatible with a fluid core. Dissipation results suggest core radius of 352-374 km (20% of the lunar radius. Williams et al. (2001) J. Geophys. Research 106, 27933–27968. Williams et al. (2006) Advances in Space Research 37, 67-71. Rediscovery of Lunokhod 1 and Lunar Laser Ranging LROC NAC images used to locate the lander and the rover. Lander identified by albedo anomaly and spacecraft identification. Rover located by(following the tracks. Murphy et al. (2011) Laser ranging to the lost Lunokhod 1 reflector. Icarus 211, 1103-1108 Recent Volcanic Activity “Recent” volcanic eruptions ~ 1 Ga. Recent fumarolic eruptions; ~10 Ma? Ina depression in Lacus Felicitatis Schultz et al. (2006) Nature, v. 444, p. 184- Recent Volcanic Activity Aristarchus North Sosigenes Maclear-1 “IMPs” (Irregular Mare Patches) <100 Ga. The irregular mare patches exhibit sharp, metre-scale morphology with relatively few superposed impact craters larger than ten metres in diameter. Crater distributions from the three largest Unnamed Unnamed Unnamed irregular mare patches imply ages Manilus-1 younger than 100 million years, based on chronology models of the lunar surface Unnamed Unnamed Braden S.E. et al. (2014) Nature Geoscience, v. 7, p. 787-791. Unnamed Unnamed Carrel-1 Images = 450 m across New Lunar Lithologies Rock Types not represented in the sample collection. Pure Anorthosite: Kaguya (SELENE) New Lunar Lithologies Rock Types not represented in the sample collection. Olivine, Orthopyroxene, and Mg-Spinel-rich lithologies (OOS) Chandrayaan-: M3 Pieters et al. (2011) JGR, 116, E00G08; Pieters et al. (2014) American Min. 99, 1895-1910 Surface Volatiles on the Moon Volatile Deposits: Chandrayaan-1 (M3), LRO Pieters et al. (2009) Science 326, 568-572 Hydrogen Deposits: LRO Mitrofanov et al. (2010) Science 330, 483-486 Cabeus Crater OH/H2O 3µm adsorption Surface Volatiles on the Moon LCROSS Impact into Cabeus Crater Colaprete et al. (2010) Science 330, 463-468. Schultz et al. (2010) Science 330, 468- 472. Surface Temperatures Paige et al. (2010) Science 330, 479-482. Bandfield et al. (2011) J. Geophys. Res. 116, E00H02, doi:10.1029/2011JE003866. Bandfield et al. (2014) Icarus 231, 221-231. PSRs are the coldest place in the Solar System. Ice Permafrost Around PSRs Neutron Suppression Regions (NSRs)are found in both permanently shadowed and illuminated areas, and they are not coincident with Permanently Shadowed Regions (PSRs). Mitrofanov et al. (2012) J. Geophys. Res. 117 E00H27, doi:10.1029/2011JE003956. Radar Detection of Water-Ice Spudis et al. (2013) J. Geophys. Res. 118, 2016-2029. Fa & Cai (2013) J. Geophys. Res. 118, 1582- 1608. Spudis et al. (2010) Geophys. Res. Lett. 37, L06204, doi:10.1029/2009GL042259 High CPR inside and outside is consistent with blocks; High CPR inside only is consistent with water-ice. LRO/LAMP Evidence of Surface Water Frost in Lunar Polar Craters LAMP’s nightside Lyman- α maps of the lunar poles show lower albedos (dark blue) in the Permanently Shaded Regions (PSRs), which is consistent with higher porosity surfaces in these regions. Comparisons of star- illuminated surfaces at FUV wavelengths with a diagnostic water spectral signature (shortward and longward of 160 nm) indicate that PSRs such as Haworth crater (inset) are best explained by 1- 2% abundances of water frost right at the surface. LAMP provides the first indications of surface water frost in permanently shadowed polar craters Gladstone et al., “Far-Ultraviolet Reflectance Properties of the Moon’s Permanently Shadowed Regions,” J. Geophys. Res., 117, E00H04, doi:10.1029/2011JE003913, 2012. LRO LAMP detects H2O on lunar dayside Hendrix et al., "The Lunar Far-UV Albedo: Indicator of Hydrated Materials and Space Weathering," J. Geophys. Res., 117, E12001, doi:10.1029/2012JE004252, 2012 • LRO LAMP makes measurements of the surface of the moon at far- ultraviolet wavelengths morning afternoon • Small amounts of water are detected across the surface of the more hydration moon • The H2O abundances are strongly correlated with surface temperature: - there’s more early in the day less hydration and late in the day, when the surface is cooler - there’s more at higher • The H2O is likely formed when solar wind latitudes, which receive less protons (H+) interact with surface molecules sunlight and are cooler containing oxygen - at warmer temperatures the • LAMP also detects H2O in permanently H2O “percolates” out of the soil shadowed polar regions Lunar Endogenous Volatiles McCubbin et al. (2010) Proc. OH content of phosphates Nat. Acad. Sci. 107, 11223-11228. 14053,16 Water in Mare Basalt Sources: 2-5 ppm Liu et al. (2010) LPSC 41 Boyce et al. (2010) Nature 466, 466-469 14053,241 Lunar Endogenous Volatiles Saal et al. (2008 Water in the Glass Parent Nature 454, 192-195) Magma: 260-745 ppm H2O Apollo 15 Green Glass (VLT) Cl F Hauri et al. (2011) Science 333, 213-215 Melt Inclusions in Olivine S Lunar Endogenous Volatiles (Chandrayaan-1 M3 data) COMPTON BELKOVICH VOLCANIC COMPLEX Bhattacharya et al. (2013) Curr. Sci. 105(5), 685-691 Enhanced hydration at CBVC could have originated from the episodic events of eruption and effusion involving silicic magma. Chandrayaan-M3 Bhattacharya et al. (2015) CRATER THEOPHILUS Icarus 260, 167–173 High-resolution spectral and spatial data analyses of crater Theophilus revealed the presence of OH-bearing Exposures on its central peak in association with olivine- , spinel- and crystalline plagioclase- bearing lithologies. Lunar Endogenous Volatiles Hejiu Hui, Anne H. Peslier, Youxue Zhang, and Clive R. Neal (2013) Water in lunar anorthosites and evidence for a wet early Moon. Nature GeoscienceLetters 6, 177-180 • FTIR analysis of Ferroan Anorthosites, samples of the primary lunar crust, show they contain significant amounts of water. • Results indicate the plagioclase contained ~6 ppm H2O. • These data allow an estimate of the initial water content of the lunar magma ocean to have been ~320 ppm. • Water in the final residuum (urKREEP) could have been 1.4 wt%. Lunar Endogenous Volatiles Yang Chen, Youxue Zhang, Yang Liu, Yunbin Guan, John Eiler, Edward M. Stolper (2015) Water, fluorine, and sulfur concentrations in the lunar mantle. Earth & Planetary Science Letters 427, 37-46 • Analysis of volatiles in melt inclusions in 74220, 15421, 10020, 12008, 15016. • Results by Hauri et al. (2011) for 74220 are not anomalous. • Approximate constancy of volatile depletion in the Moon relative to the Earth explained by assuming that both acquired volatiles from a similar source or by a similar mechanism, but the earth was more efficient in acquiring the volatiles. • The H2O, F and S concentrations in the primitive lunar mantle source to be similar to or slightly lower than those in terrestrial MORB mantle. Anhydrous Moon The Cl isotope composition of Apollo basalts & glasses have a range of isotopic values 25 times the range for Earth. Explained by volatilization of metal halides during eruption of a basalt containing H concentrations ~104 to 105 lower than those of Earth, implying that the lunar interior is essentially anhydrous. Sharp et al. (2010) Science 329, 1050-1053.
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