SMART-1 mission to the Moon: Status, first results and goals

Foing, B. H.; Racca, Giuseppe D.; Marini, Andrea; Evrard, E; Stagnaro, L.; Almeida, Miguel; Koschny, D.; Frew, David J.; Zender, Joe; Heather, James P.; Grandé, M.; Huovelin, J.; Keller, H. U.; Nathues, A.; Josset, J. L.; Mälkki, Anssi; Schmidt, W.; Noci, G.; Birkl, Reinhard; Iess, L.; Sodnik, Zoran; McManamon, Paul

doi:10.1016/j.asr.2005.12.016

Cited by 87 publications

(31 citation statements)

References 21 publications

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“…New data from the Lunar Reconnaissance Orbiter (LRO) mission, related NASA missions such as the Gravity Recovery and Interior Laboratory (GRAIL) mission , and international missions to the Moon (SMART 1, Foing et al, 2006; Kaguya, Kato et al, 2008;Chandrayaan-1, Goswami and Annadurai, 2009;Chang'e, Li et al, 2015), enable our analysis of the generation, ascent and eruption of magma and the description and interpretation of emplacement processes and the geologic record presented here. Building on the theoretical framework of the generation, ascent and eruption of magma ) derived from analysis of: 1) new data on lunar crustal thickness and structure from the GRAIL mission , and 2) new data on the production of volatiles during magma ascent and eruption (Wilson and Head, 2003a;Rutherford and Papale, 2009;Saal et al, 2008;Hauri et al, 2011Hauri et al, , 2015Wetzel et al, 2015), we use data from LRO on the global topography of the Moon from new altimetry (Figure 1b) (Lunar Orbiter Laser Altimeter, LOLA; Zuber et al, 2010;Smith et al, 2010), and detailed characterization of lunar volcanic features and deposits using new imaging data (Lunar Reconnaissance Orbiter Camera, LROC; Robinson et al, 2010), altimetry data (LOLA; Zuber et al, 2010;Smith et al, 2010), and spectral reflectance data (Moon Mineralogy Mapper, M3; Pieters et al, A C C E P T E D M A N U S C R I P T 7 2009).…”

Section: Introductionmentioning

confidence: 98%

Generation, ascent and eruption of magma on the Moon: New insights into source depths, magma supply, intrusions and effusive/explosive eruptions (Part 2: Predicted emplacement processes and observations)

Head

Wilson

2017

Icarus

186

197

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1 Highlights  Mare basalt eruption process predictions are compared to observed features/deposits.  Single dike event magma volume predicted to be 10 2 -10 3 km 3 ; dikes 40-100 m by 60-100 km. Shallower-source dikes continuous from source to surface; deeper dikes detach from source. Dikes reaching surface form wide range of predicted/observed effusive/explosive eruption types. Intrusion is favored in thicker farside crust; extrusion is favored on thin nearside crust. AbstractWe utilize a theoretical analysis of the generation, ascent, intrusion and eruption of basaltic magma on the Moon to develop new insights into magma source depths, supply processes, transport and emplacement mechanisms via dike intrusions, and effusive and explosive eruptions. We make predictions about the intrusion and eruption processes and compare these with the range of observed styles of mare volcanism, and related features and deposits. Density contrasts between the bulk mantle and regions with a greater abundance of heat sources will cause larger heated regions to rise as buoyant melt-rich diapirs that generate partial melts that can undergo collection into magma source regions; diapirs rise to the base of the anorthositic crustal density trap (when the crust is thicker than the elastic lithosphere) or, later in history, to the base of the lithospheric rheological trap (when the thickening lithosphere exceeds the thickness of the crust). Residual diapiric buoyancy, and continued production and arrival of diapiric material, enhances melt volume and overpressurizes the source regions, producing sufficient stress to cause brittle deformation of the elastic part of the overlying lithosphere; a magma-filled crack initiates and propagates toward the surface as a convex upward, blade-shaped dike. The volume of magma released in a single event is likely to lie in the range 10 2 km 3 to 10 3 km 3 , corresponding to dikes with widths of 40-100 m and both vertical and horizontal extents of 60-100 km, favoring eruption on the lunar nearside. Shallower magma sources produce dikes that are continuous from the source region to the surface, but deeper sources will propagate dikes that detach from the source region and ascend as discrete penny-shaped structures. As the Moon cools with time, the lithosphere thickens, source regions become less abundant, and rheological traps become increasingly deep; the state of stress in the lithosphere becomes increasingly contractional, inhibiting dike emplacement and surface eruptions.In contrast to small dike volumes and low propagation velocities in terrestrial environments, lunar dike propagation velocities are typically sufficiently high that shallow sill formation is not favored; local low-density breccia zones beneath impact crater floors, however, may cause lateral magma migration to form laccoliths (e.g., Vitello Crater) and sills (e.g., Humboldt Crater) in floor-fractured craters. Dikes emplaced into the shallow crust may stall and produce crater chains due to active andpassive gas venting (e.g., Men...

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Section: Introductionmentioning

confidence: 98%

Generation, ascent and eruption of magma on the Moon: New insights into source depths, magma supply, intrusions and effusive/explosive eruptions (Part 2: Predicted emplacement processes and observations)

Head

Wilson

2017

Icarus

186

197

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“…After the 1990s, three spacecraft, Clementine (Nozette et al 1994), Lunar Prospector (Binder 1998), and SMART-1 (Foing et al 2006) orbited the Moon. Three-dimensional low-energy electron measurements by Lunar Prospector revealed the lunar plasma environment, including plasma interactions with crustal magnetic fields, surface charging, and wake structure Halekas et al 2001Halekas et al , 2002Halekas et al , 2005Halekas et al , 2008Halekas et al , 2009aHalekas et al , 2009b Besides the three orbiters, observations by the Wind spacecraft during its Moon fly-by showed features of the lunar wake (Ogilvie et al 1996).…”

Section: Introductionmentioning

confidence: 99%

In-flight Performance and Initial Results of Plasma Energy Angle and Composition Experiment (PACE) on SELENE (Kaguya)

et al. 2010

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MAP-PACE (MAgnetic field and Plasma experiment-Plasma energy Angle and Composition Experiment) on SELENE (Kaguya) has completed its ∼1.5-year observation of low-energy charged particles around the Moon. MAP-PACE consists of 4 sensors: ESA (Electron Spectrum Analyzer)-S1, ESA-S2, IMA (Ion Mass Analyzer), and IEA (Ion Energy Analyzer). ESA-S1 and S2 measured the distribution function of low-energy electrons in the energy range 6 eV-9 keV and 9 eV-16 keV, respectively. IMA and IEA measured the distribution function of low-energy ions in the energy ranges 7 eV/q-28 keV/q and 7 eV/q-29 keV/q. All the sensors performed quite well as expected from the laboratory experiment carried out before launch. Since each sensor has a hemispherical field of view, two electron sensors and two ion sensors installed on the spacecraft panels opposite each other could cover the full 3-dimensional phase space of low-energy electrons and ions. One of the ion sensors IMA is an energy mass spectrometer. IMA measured mass-specific ion energy spectra that have never before been obtained at a 100 km altitude polar orbit around the Moon. The newly observed data show characteristic ion populations around the Moon. Besides the solar wind, MAP-PACE-IMA found four clearly distinguishable ion populations on the dayside of the Moon: (1) Solar wind protons backscattered at the lunar surface, (2) Solar wind protons reflected by magnetic anomalies on the lunar surface, (3) Reflected/backscattered protons picked-up by the solar wind, and (4) Ions originating from the lunar surface/lunar exosphere.

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“…This technology was to be tested by ESA through the first Small Mission for Advanced Research in Technology (SMART-1) to the Moon. This mission, launched in 2003 and very successfully implemented, used SEP for transfer to lunar orbit and concluded in 2006 when the spacecraft was crashed into the Moon, following a successful technological and scientific programme (Foing et al 2006). …”

Section: Concepts Of a Mercury Orbiter Mission In Europementioning

confidence: 98%