Unique, Antique Vesta - Lunar And Planetary Institute (LPI)
Unique, Antique VestaAsteroid Vesta, 510 kmin diameter. PHOTOCREDIT : NASAHarry Y. McSween1, Maria Cristina De Sanctis2,Thomas H. Prettyman3, and the Dawn Science Team1811-5209/14/0010-039 2.50MDOI: 10.2113/gselements.10.1.39Modeling of Vesta’s gravity andshape reveals its dense heart—an iron metal core 220 kmacross (Russell et al. 2012). Thecatastrophic Rheasilvia impactshould likely have destroyed Vesta,but its metallic skeleton may haveaided the asteroid’s survival. Theeffects of Rheasilvia, though, arehard to miss. A girdle of ridges andtroughs that encircles the equator(Buczkowski et al. 2012) is thoughtKEYWORDS : Vesta, asteroid, HED meteorites, differentiation, impactto be a result of seismic reverberations from the core, and a thickblanket of ejecta extends outwardVESTA—OUTSIDE AND INfrom the basin to cover the southern half of the asteroidAsteroid Vesta, once called the smallest terrestrial planet(Schenk et al. 2012).(Keil 2002), is a leftover planetary building block. It wasrecently imaged, analyzed, and mapped from orbit by theDawn spacecraft mission (described in Box 1).BOX 1THE DAWN MISSIONVesta has an average diameter of 510 km and a meanArtist’sdensity of 3456 kg/m3 (Russell et al. 2012). Although thedepiction ofbody is massive enough to have assumed a spherical shape,the Dawnit is conspicuously out of round, a consequence of a hugespacecraftin orbitimpact basin (FIG. 1) near its south pole (Schenk et al.around Vesta.2012). This basin, called Rheasilvia4, has a diameter almostR EPRODUCEDequal to that of Vesta. Rheasilvia is superimposed on anCOURTESY OFolder crater, Veneneia. The combined impacts excavatedNASAdeeply enough to expose the Vestan mantle (Jutzi et al.2013; McSween et al. 2013). The Rheasilvia event launcheda host of multikilometer-sized bodies that are still orbitallylinked to Vesta—the Vesta family, or “Vestoids” (Binzel andXu 1993). Dislodged samples of the Vestoids have migratedThe Dawn spacecraft (Russell and Raymond 2011) was launched ininto nearby resonances—“escape hatches” from which theySeptember 2007 and traveled for nearly four years to reach its firstwere perturbed into Earth-crossing orbits to eventuallyobjective, 4 Vesta. The spacecraft is powered by solar panels with anbecome meteorites. 20 m wingspan, and thrust is provided by a novel ion propulsionsystem that expels xenon ions. After a slow but steady acceleration,Vesta is covered with a regolith of impact-comminutedDawn now holds the records for the greatest velocity increase andigneous rocks and pocked with hundreds of craters.the longest powered flight. Once in Vestan orbit, the spacecraft spentHowever, no lava flows or other volcanic constructs aremore than a year mapping the asteroid from altitudes of 2735, 685,recognizable (Jaumann et al. 2012). Steep slopes are everyand 210 km.where on Vesta, complicating our understanding of itsDawn carries three kinds of instruments: dual Framing Cameras forgeomorphology.geologic imagery and navigation, provided by the German Max PlanckInstitute for Solar System Studies; a Visible and Infrared Spectrometer(VIR) for mineral identification and mapping, provided by the ItalianNational Institute for Astrophysics; and a Gamma Ray and NeutronDetector (GRaND) for geochemical analysis and mapping, operated1 Department of Earth and Planetary Sciencesby the U.S. Planetary Science Institute. In addition, a gravity experiUniversity of Tennessee, Knoxville, TN 37996-1410, USAment, carried out using radio tracking of the spacecraft’s orbit withE-mail: mcsween@utk.edudetailed topographic mapping, provided constraints on Vesta’s interior2 Istituto di Astrofisica e Planetologia Spazialistructure and on its mean density.ost asteroids are collisional rubble from eons past, and few of themhave survived intact. Vesta, the second most massive asteroid, isthe only differentiated, rocky body in this category. This asteroidprovides a unique view of the kinds of planetesimals that accreted to formthe terrestrial planets. We know more about this asteroid than any other,thanks to its recently completed exploration by the orbiting Dawn spacecraftand studies of the 1000 meteorites derived from it. The synergy providedby in situ analyses and samples has allowed an unparalleled understandingof Vesta’s mineralogy, petrology, geochemistry, and geochronology.Istituto Nazionale de Astrofisica, Rome, ItalyUpon completion of its exploration of Vesta in October 2012, Dawndeparted Vesta’s gravitational grasp and set sail on a three-yearjourney to 1 Ceres, the largest asteroid.3 Planetary Science Institute, Tucson, AZ 85719, USA4 The names of Vestan features follow a Roman naming convention;Rheasilvia is named after the mother of Rome’s founders, Romulusand Remus.E LEMENTS , V OL . 10,PP.39–4439F EBRUARY 2014
VESTA SAMPLES—HED METEORITESPerspective view of the topography of Vesta’s southpole region, showing the huge Rheasilvia impactbasin. Elevations, relative to the average Vesta surface, are indicatedby coloration and demonstrate that this basin significantly affectsthe asteroid’s overall shape. This view was compiled by the DawnScience Team from Framing Camera images.FIGURE 1Four decades ago, McCord et al. (1970) identified Vesta asthe likely parent body for the igneous howardite-eucritediogenite (“HED”) meteorites, based on their spectralsimilarities. Eucrites are comprised of plagioclase pluspyroxene and are commonly subdivided into fi ne-grainedvolcanic (basaltic eucrite) and coarse-grained plutonic(cumulate gabbroic eucrite) varieties (FIG. 2). Diogenites areultramafic rocks formed through accumulation of crystals oforthopyroxene (pyroxenite) or orthopyroxene plus olivine(harzburgite) (FIG. 2). One mostly olivine cumulate (dunite)obviously linked to diogenites has also been described. Mosteucrites and diogenites are breccias and represent regolithmaterials. These breccias can be monomict (containingclasts of a single lithology) or polymict (containing clasts ofboth basaltic and cumulate eucrite, or of multiple diogeniteunits). If both eucrite and diogenite clasts are present, themeteorite is a howardite. There is a continuum betweenpolymict eucrites, howardites, and polymict diogenites,making the distinction somewhat arbitrary. The co-occurrence of these different rock types within breccias supportsthe idea that they formed on a common parent body. Theoxygen isotope compositions of most HEDs also lie on thesame 16O–17O–18O mass-fractionation line (Greenwood etal. 2005), taken as a geochemical fingerprint of their parentasteroid. Descriptions of the petrology and geochemistry ofthese meteorites abound, and are most recently reviewedby McSween et al. (2011).The crystallization ages of basaltic eucrites, determined fromradiogenic isotopes ( 87Rb– 87Sr, 147Sm–143Nd, 207Pb–206Pb),are 4.5 billion years (numerous references in McSweenet al. 2011). The measured ages of plutonic diogenitesand cumulate eucrites tend to be slightly younger, likelyreflecting slower cooling through the isotope blockingtemperatures. The decay products of short-lived radionuclides (26Al, 53Mn, 182Hf) are also found in HED meteorites,further confi rming their ancient ages and the rapid differentiation of their parent body.pyroxenes and plagioclase; and (right) diogenite, composed oforthopyroxene and, locally, olivine. Scale bars are 2.5 mm.Photomicrographs (crossed polars) of (left) basalticeucrite, composed of ferroan pyroxenes andplagioclase; (center) cumulate eucrite, composed of magnesianFIGURE 2E LEMENTS40F EBRUARY 2014
Despite the association of eucrites and diogenites inbreccias, the petrogenetic relationships between them arenot well understood. An early model explaining eucrites aspartial melts and diogenites as solid residues (Stolper 1977)has mostly been supplanted by magma-ocean models thatexplain diogenites as cumulates and eucrites as residualliquids (e.g. Righter and Drake 1997; Greenwood et al.2005; Mandler and Elkins-Tanton 2013). Asteroid-widemelting is suggested by rapid heating through decay of 26Al.However, models indicate highly efficient melt removalfrom asteroid mantles, so that only a few percent of magmamight be present at any particular time, possibly preventingformation of a magma ocean (Wilson and Keil 2012). Fora body the size of Vesta, eruptions directly to the surfacevia dikes would be mechanically difficult; instead, largemagma chambers would likely form in the subsurface,and flows could erupt episodically from these chambers(Wilson and Keil 2012; Mandler and Elkins-Tanton 2013).The varied trace element patterns in diogenites are consistent with their derivation from separate magma chambers(Shearer et al. 1997; Mittlefehldt et al. 2012), and geochemical trends in basaltic eucrites may require multiple magmasand complex processes within the crust (Barrat et al. 2007).occurred). Mixing of eucrite with diogenite, or vice versa, isapparently common at this scale on Vesta, pulling spectratowards the center of the plot.Vesta’s global weight ratio of Fe/Si and Fe/O, determinedby GRaND (Prettyman et al. 2012), also identifies HED-likecompositions (FIG. 4). In this diagram, howardite anddiogenite provide the best match for Vesta data. Othermeteorite types mostly plot outside the Vesta data ovals.VESTA’S COMPOSITIONAS MEASURED BY DAWNComparing the reflectance spectra of Vesta, as measuredby a visible–infrared spectrometer (VIR) (De Sanctis etal. 2012a), with the spectra of HEDs provides a means ofidentifying surface lithologies. FIGURE 3 shows a plot of thecenter positions of the 1 μm and 2 μm absorption bands(henceforth called BI and BII) in well-characterized HEDmeteorites measured in the laboratory; these bands varywith pyroxene composition and abundance. The boxes inFIGURE 3 serve as a spectral classification, and a contoured,global cloud of Vestan spectral pixels measured by Dawn’sVIR spectrometer is also shown. The greatest concentration of Vestan pixels corresponds to howardite or cumulateeucrite. Howardite, representing the regolith, is the morelikely interpretation. The eucrite and diogenite boxes inFIGURE 3 are not completely populated by Vesta data. Thispresumably reflects the large spatial resolution of VIRdata ( 700 m/pixel at the altitude where global mappingGRaND element ratios for Vesta compared to thecompositions of HED meteorites. The 1σ and 2σ ovalsindicate standard deviations of the mean for GRaND's Vesta data.DATA FROM PRETTYMAN ET AL. (2012)FIGURE 4A VIR global map (De Sanctis et al. 2012a), using theclassification in FIGURE 3, distinguishes areas dominatedby howardite, eucrite, and diogenite (FIG. 5). Eucrite mostlyoccurs in heavily cratered, ancient crust near the equator,and diogenite is concentrated in the southern hemisphere.A global map of GRaND-measured variations in neutronabsorption (Prettyman et al. 2012), which relate to thedifferent element abundances in eucrites and diogenites,is illustrated in FIGURE 6. Although the spatial footprint ofGRaND is large ( 300 km), these data confi rm the distributions of HED lithologies determined by VIR spectra.VIR and GRaND maps of Vesta’s south pole regiondemonstrate that diogenite is exposed on the floor of theRheasilvia basin and is a major component of its ejectablanket (McSween et al. 2013). The estimated depth ofexcavation of Rheasilvia is at least twice the crustal thickness, so diogenite is interpreted as mantle rock. Althoughthe occurrence of diogenite is at about the right depth( 20 km) for some magma-ocean models, its lateral extentis not known, so excavated plutons are possible.The measured depletions of siderophile (metal-loving) traceelements (Righter and Drake 1997) and paleomagneticindications of a former magnetic dynamo (Fu et al. 2012)in eucrites are evidence for a metal core in the HED parentasteroid. Compositional models of the interior of the HEDparent body, constructed from the meteorite compositions,predict a metallic core with a mass fraction of 15–20%(Righter and Drake 1997). This compares favorably withthe 18% mass fraction of Vesta’s core determined by Dawn(Russell et al. 2012).BI versus BII band center positions for spectra of HEDmeteorites, and a cloud of Vesta data measured byvisible-light–infrared (VIR) spectroscopy. The boxes are defi ned bywell-characterized HEDs, each having at least 30 spectralmeasurements.FIGURE 3E LEMENTS41F EBRUARY 2014
homogenized composition (Warren et al. 2009) was notborne out, as FIGURES 5 and 6 show that the proportions ofeucrite and diogenite in howardite terranes vary considerably. Although a few exotic components have been foundin howardites, such as potassium-rich glasses suggested torepresent a highly fractionated component analogous tolunar KREEP (Barrat et al. 2009), none has been detectedat Dawn mapping scales.VESTA’S CHRONOLOGYAND IMPACT HISTORYThe ages of Vesta’s surface units, derived from the densityof craters, are 3 to 4 billion years (Marchi et al. 2012). Theseare minimum ages, because the surface has become effectively saturated with craters, so that new craters destroyolder ones. The 4.5-billion-year crystallization ages ofeucrites, and especially the former presence of short-livedradionuclides, reveal that Vesta melted and differentiatedearlier, within the first several million years of Solar Systemhistory. However, somewhat younger ages for diogenitesand cumulate eucrites indicate a protracted cooling historylasting perhaps 50 million years.Another surprise was GRaND’s discovery of hydrogen inthe regolith (Prettyman et al. 2012). Broad regions of thesurface contain 400 μg/g H (FIG. 7), an abundance thatcannot be explained by solar wind implantation, as onthe Moon. The hydrogen-rich regions have low albedo andexhibit a 2.8 μm absorption in VIR spectra, which is attributable to OH in phyllosilicate minerals (De Sanctis et al.2012b). In hindsight, this discovery should not have beena surprise. Howardites commonly contain foreign clastsof carbonaceous chondrite meteorites (FIG. 7), which arelargely composed of OH-bearing serpentine and clays.Laboratory spectra of eucrites mixed with a few percentcarbonaceous chondrite (which would give bulk hydrogencontents like those measured by GRaND) provide an excellent match with the spectra of these dark regions (Reddyet al. 2012).Like other bodies in the Solar System, Vesta was struckby careening, massive bolides in the period from 4.1 to3.5 billion years ago. This period of high impactor flux,sometimes called the “late heavy bombardment,” is thoughtto have resulted from gravitational stirring of the asteroidbelt when the giant planets migrated inward or outwardto their present orbital positions. This bombardment isrevealed by a number of peaks among the 40Ar– 39Ar agesof eucrite breccias, and these peaks represent a series ofage-resetting events.Rheasilvia, the most prominent feature on Vesta, is 1.0billion years old as determined from crater counting andtherefore is considerably younger than the rest of the asteroid’s surface (Marchi et al. 2012). This age is consistentwith the ages of the Vestoids, the orbits of which wouldhave been scrambled if they had been launched from Vestamuch earlier.Solar irradiation and micrometeorite bombardment havealtered the spectrum of lunar soil—a process called spaceweathering. The spectral changes result from the production of nanoscale iron metal particles, which subdueabsorption bands and modify the continuum slope. OnVesta, space weathering takes a different form. Althoughthe albedo of the Vestan surface exposed by recent impactschanges over time, its spectrum does not show the characteristics of nanophase iron (Pieters et al. 2012), and thismineral is virtually absent from howardites. Vesta’s locationso far from the Sun, where impact velocities are lower, andpossible shielding of cosmic rays by its remnant magneticfield (Fu et al. 2012) may account for this difference insoil mineralogy.VESTA’S SURPRISING SOILAlthough howardite covers most of Vesta’s surface, it is notthe most abundant type of HED meteorite. The Rheasilviaimpact excavated much more material from the deepcrust and mantle than from the veneer of regolith on thesurface. A prediction that the regolith might have a globallydotted lines represent the limits of the Rheasilvia and Veneneiaimpact basins, respectively.Global map of the distribution of terrains dominatedby eucrite, diogenite, and howardite on Vesta, basedon VIR spectra from De Sanctis et al. (2012a). The dashed andFIGURE 5E LEMENTS42F EBRUARY 2014
Global map of the relativevariations of thermalneutron absorption measured byGRaND, confirming the identificationand distribution of lithologies based onVIR spectra. Regions with low (blue) orhigh (red) absorption contain morediogenite or basaltic eucrite, respectively. The Rheasilvia boundary is shownby the white line. GRaND data aresuperimposed on a shaded relief mapprovided by R. Gaskell.FIGURE 6GRaND global map ofhydrogen, from Prettymanet al. (2012), and a photomicrograph(crossed polars) of a howardite samplecontaining dark clasts of carbonaceouschondrite.FIGURE 7SUMMARYACKNOWLEDGMENTSCoupling the petrologic, geochemical, and geochronologic information afforded by laboratory studies of HEDmeteorites with the geologic context provided by Dawn’sorbital exploration of Vesta allows an understanding ofthis unique, antique asteroid—the kind of objects thataccreted to form our own planet. Its early differentiationand magmatic evolution, violent collisional history, andinteraction with the space environment are all imprintedon its surface and written in its rocks. Asteroid Vesta nowjoins the Moon and Mars as astronomical objects that havebeen transformed into geologic worlds.We gratefully acknowledge the efforts of the DawnOperations and Science Teams (CT Russell, PrincipalInvestigator) and reviews by T. J. McCoy and J. A. Barrat.This work was supported by NASA’s Discovery Programthrough contracts to UCLA (HYM) and the Jet PropulsionLaboratory (THP), and by the Italian Space Agency (MCD).REFERENCESBarrat JA, Yamaguchi A, Greenwood RC,Bohn M, Cotton J, Benoit M, FranchiIA (2007) The Stannern trend eucrites:Contamination of main group eucriticmagmas by crustal partial melts.Geochimica et Cosmochimica Acta 71:4108-4124Barrat JA, Bohn M, Gillet P, YamaguchiA (2009) Evidence for K-rich terraneson Vesta from impact spherules.Meteoritics & Planetary Science 44:359-374E LEMENTSBinzel RP, Xu S (1993) Chips off asteroid4 Vesta: Evidence for the parent body ofbasaltic achondrite meteorites. Science260: 186-191Buczkowski DL and 19 coauthors (2012)Large-scale troughs on Vesta: A signature of planetary tectonics. GeophysicalResearch Letters 39: L18205De Sanctis MC and 22 coauthors (2012a)Spectroscopic characterization of mineralogy and its diversity across Vesta.Science 336: 697-70043De Sanctis MC and 20 coauthors (2012b)Detection of widespread hydratedmaterials on Vesta by the VIR imagingspectrometer on board the Dawnmission. Astrophysical Journal Letters758: L36Fu RR and 8 coauthors (2012) An ancientcore dynamo in asteroid Vesta. Science338: 238-241Greenwood RC, Franchi IA, JambonA, Buchanan PC (2005) Widespreadmagma oceans on asteroidal bodiesin the early Solar System. Nature 435:916-918F EBRUARY 2014
Jaumann R and 42 coauthors (2012)Vesta’s shape and morphology. Science336: 687-690Jutzi M, Asphaug E, Gillet P, Barrat J-A,Benz W (2013) The structure of theasteroid 4 Vesta as revealed by modelsof planet-scale collisions. Nature 494:207-210Keil K (2002) Geological history ofasteroid 4 Vesta: The “smallest terrestrial planet”. In: Bottke W, Cellino A,Paolicchi P, Binzel RP (eds) Asteroids III.University of Arizona Press, Tucson, pp573-584Mandler BE, Elkins-Tanton LT (2013)The origin of eucrites, diogenites,and olivine diogenites: Magma oceancrystallization and shallow magmachamber processes on Vesta. Meteoritics& Planetary Science 48: 2333-2349Marchi S and 11 coauthors (2012) Theviolent collisional history of asteroid 4Vesta. Science 336: 690-694McCord TB, Adams JB, Johnson TV (1970)Asteroid Vesta: Spectral reflectivity andcompositional implications. Science168: 1445-1447McSween HY Jr, Mittlefehldt DW, BeckAW, Mayne RG, McCoy TJ (2011) HEDmeteorites and their relationship to thegeology of Vesta and the Dawn mission.Space Science Reviews 163: 141-174McSween HY and 21 coauthors (2013)Composition of the Rheasilvia basin,a window into Vesta’s interior. Journalof Geophysical Research: Planets 118:335-346Mittlefehldt DW, Beck AW, Lee C-TA,McSween HY Jr, Buchanan PC (2012)Compositional constraints on thegenesis of diogenites. Meteoritics &Planetary Science 47: 72-98Pieters CM and 16 coauthors (2012)Distinctive space weathering on Vestafrom regolith mixing processes. Nature491: 79-82Prettyman TH and 19 coauthors (2012)Elemental mapping by Dawn revealsexogenic H in Vesta’s regolith. Science338: 242-246Reddy V and 24 coauthors (2012)Delivery of dark material to Vesta viacarbonaceous chondritic impacts. Icarus221: 544-559Righter K, Drake MJ (1997) A magmaocean on Vesta: Core formation andpetrogenesis of eucrites and diogenites.Meteoritics & Planetary Science 32:929-944Russell CT and 27 coauthors (2012) Dawnat Vesta: Testing the protoplanetaryparadigm. Science 336: 684-686Schenk P and 13 coauthors (2012) Thegeologically recent giant impact basinsat Vesta’s south pole. Science 336:694-697Shearer CK, Fowler GW, Papike JJ (1997)Petrogenetic models for magmatism onthe eucrite parent body: Evidence fromothopyroxene in diogenites. Meteoritics& Planetary Science 32: 877-889Stolper EM (1977) Experimental petrologyof eucritic meteorites. Geochimica etCosmochimica Acta 41: 587-681Warren PH, Kallemeyn GW, Huber H,Ulf-Møller F, Choe W (2009) Siderophileand other geochemical constraintson mixing relationships amongHED-meteoritic breccias. Geochimica etCosmochimica Acta 73: 5918-5943Wilson L and Keil K (2012) Volcanicactivity on differentiated asteroids: Areview and analysis. Chemie der Erde72: 289-321Russell CT, Raymond CA (2011) TheDawn mission to Vesta and Ceres. SpaceScience Reviews 163: 3-23A hypothetical question of course! But evenif we could ask them, the SPECTRO MS makesthe question redundant. This novel ICP massspectrometer analyzes the entire relevant massspectrum completely simultaneously; faster andmore precisely to boot.SPECTRO MS- Double focusing sector field mass spectrometerwith newly developed ion optic and pioneeringdetector technology- Simultaneous measurement of more than75 elements with 210 isotopes for improvedprecision together with highest sample throughput- Fast fingerprinting, internal standardization inreal time- Compatible with EPA, FDA, CLP and 21 CFR Part 11as well as additional standards and guidelinesDo You Think IonsLike Queuing Up?Find out more aboutthe SPECTRO MS atwww.spectro.com/msPlease visit us atPITTCON 2014, 2-6 March,Chicago, IL, Booth: 3931/4031.SPECTRO MS: A New Era in ICP Mass Spectrometry2011E LEMENTS44F EBRUARY 2014
Unique, Antique Vesta VESTA—OUTSIDE AND IN Asteroid Vesta, once called the smallest terrestrial planet (Keil 2002), is a leftover planetary building block. It was recently imaged, analyzed, and mapped from orbit by the Dawn spacecraft mission (described in Box 1). Vesta has an average diameter of 510 km and a mean
Accessing Vesta Learning Management System Vesta LMS system is web based and must be accessed through a web browser (Chrome recommended) by visiting https://lms.vestaevv.com. Note: Vesta LMS cannot be accessed via the remote desktop. Users may access Vesta LMS via any device that has a web browser and internet access. Prior to accessing Vesta .
renewed lunar exploration, scientists have accumulated new insights from a new generation of robotic spacecraft sent to the Moon. These spacecraft include the United States’s Clementine, Lunar Prospector, Lunar Reconnaissance Orbiter, Gravity Recovery and Interior Laboratory (GRAIL), and Lunar Atmosphere and Dust Environment Explorer
System (GPS) to identify the location of a visit ONLY at the time a CDS employee clocks in and clocks out. The Vesta Mobile Application does not use GPS at any other time during a visit. The Vesta Mobile Application uses data and not minutes from a smartphone plan. There is minimal impact to mobile phone data costs.
2. From Vesta CDV, click the menu button and select My Profile. a. The Agency ID is located under the Provider Information. b. The Employee EVV ID and Vesta Mobile Pin is located under the CDS employee section. Smart Phone Requirement Smart Phone: A CDS employee may enter information into the EVV system by using a smart phone. To do so,
VESTA Sterile valves provide a surface quality of R a 0.8 μm (optionally electro-polished) in product-wetted areas by default. Higher surface finishes are available upon request. Production quality and material traceability VESTA Sterile valves are subject to the highest quality criteria in their production. A high production depth and a
"Vesta" is heard when the CDS employee calls the Vesta EVV toll-free phone number. This indicates the EVV system captured the caller ID. The CDS employee must call from the CDS member's documented home landline phone number for the EVV system to recognize they are calling from the CDS member's home. Step 1: Enter the Employee ID.
The Lunar Quest Program (LQP), previously the Lunar Science Project, is now moved to its own stand-alone budget and program line. Project elements under LQP includes the Lunar Atmosphere and Dust Environment Explorer (LADEE) and the International Lunar Network (ILN) missions, and the Lunar Science Research.
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