Directory Of Research Projects - CORE
https://ntrs.nasa.gov/search.jsp?R 19900017427 2020-03-19T21:17:45 00:00ZNASA TechnicalDirectoryof ologyand4211ProjectsGeophysicsEditorof SpaceD.C.NI ANational Aeronautics andSpace AdministrationOffice of ManagementScientificand ndApplicationsProgram
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PLANETARYGEOLOGY AND GEOPHYSICS PROGRAM1300012000[]4.5ZS IN1000'SCOLA11000 100O0fIIIFY 87FY 88FY 89FY 909OOOFY 86SUPPORT TASK AL
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DonaldR.Davis,PhilipA.De Hon,ReneA.Dermott,StanleyF.Durham,WilliamB.U WACalTechWash.UU AZJPLJPLUSGS,U HIU VAFY90FlagstaffCarnegieInst.ofU S,MenloAZSt UUSGS,DenverUSGS,MenloU kCorp.USGSFlagstaffNELAUU FLGainesvilleLLNLU NMU MIStanfordU COU HIAZSt UElston,WolfgangE.England,A. k,MatthewP.WellesleyNASAGSFCRPIJPLU AZJPLJPLviiWash.
ESTIGATORw tNASA/JSCU HIAZSt UU AZM.I.T.U PittsburghJPLPSIU HIBrownU WAN AZUU AZU VAU COU CA,BerkeleyU VAJPLUCLAUSGS,FlagstaffAZ St USUNY,BuffaloUSGS,DenverUSGS,FlagstaffORSt UU AZU COU AZSUNY,StonyBrookUSGS,FlagstaffU HIU AZAZSt liamMelosh,Metzger,Moore,H. J.AlbertHenryJ.Mouginis-Mark,U HIUSGS,U CA,U MA,NASA/ARCWash.U AZJPLUSGS,U kWash.
mesB.Ostro,StevenJ.Owen,TobiasC.Paige,DavidA pkinsSanFranciscoStJPLU HIUCLABrownLosAlamosNatl.U CA,SMUBrownJPLSantaNASA/ARCNASA/ARCU AZU ChicagoCorne i staffBoeingUCLABrownUSGSFlagstaffLPIAZStUUSGSU CalTechU COU AZUSGSFlagstaffCornellJPLU AZCornellStanfordKSSt UCorneliJosephixBarbaraULab.
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PROPOSALPRINCIPALINVESTIGATORSUMMARY!ABSTRACTJohn B. AdamsDept. of GeologicalSciencesUniversity of WashingtonSeattle, WA 98195(206)543-6221CO-INVESTIGATORSMilton O. SmithPROPOSALSpectralTITLEReflectanceAJ-20of PlanetarySurfacesABSTRACTa. Our overall research objective is to provide new information on the chemistry,mineralgy and geologyof planetary surfaces using muttispectralimages and reflectance spectra in the visible and near-infraredwavelengthregion. The approach is to interpret the remotely sensed data in terms of laboratoryreference spectra, and to use spectral mixing models to quantify mineral phase-abundances.b. We worked with Ray Arvidson'sgroup on two approachesto the intercomparisonof Viking Lander,Viking Orbiter, telescopicand laboratory reflectivity spectra. We calibrated Viking multispectralimagesusing available informationon the instrument responses, and we derived photometricand atmosphericparameters.We also calibrated the data sets using a spectral mixing model. The two approacheswerecompared.They provide a basis for interpreting the surface compositionof Mars at a wide range ofspatial scales.We continued work with Paul Johnson on a semiempiricalmodel for calculating binarymineral mixtures which vary in particle size and illumination geometry. Calculatedmixtures are withinlaboratory experimentalerrors. . In the coming year we propose to investigate:1) the effect ol spatial scale on spectral mixing; and 2)the spectral mixing systematicsof sets of telescopic spectra of Mars, the moon and asteroids.d.Johnson P.E., Singer R.B., Smith M.Q., and Adams J.B. Quantitativedeterminationof mineralabundancesand particle sizes from reflectance spectra, J. Geo0hys. Res., in press.Adams J.B., Smith M.O., GuinnessE.A., and Arvidson R.E.1988.Geologic units on Mars: Spectraland textural mixing evidence from Viking Orbiter, J. Geoohvs. ResL, in preparation.Arvidson R.E., Dale-BannisterM.A., GuinnessE.A., Adams J.B., Smith M.O., ChristensenP.R., andSinger R.1988.Nature and distribution of surficial deposits in Chryse Planitia and vindnity, Mars, J.GeoDhvs.Res,, 94.82,1573-1587.Smith M.O. and Adams J.B.,Isolation of compositionalvariance from Viking Lander multispectralimages, (abs.) Lunar and Planetary Science ConferenceXX, March, 1989.(a)(b)(c)(d)Type abstract single-spaced, paragraphs numbered:brief statement of the overall objectives and justification of the work;brief statement of accomplishments of prior year,or "new proposal";brief listing of what will be done this year, how, and why;one or two of recent publications relevant to proposed work.
PROPOSALPRINCIPALINVESTIGATOR:SUMMARYThomasJ. AhrensSeismologicalLaboratoryCalifornia Institute of TechnologyPasadena,CA ateringCalculationsABSTRACT:a.Objectives:To describe and understandthe physics of impact cratering,both normal and oblique,on planetarysurfaces composedof solid silicates, ices, and their regoliths, as well asimpacts into planetaryatmospheresand proto-atmospheresand into the ocean. On a largerscale we expect to constrain impact conditions for partial and complete loss of atmospheresas well as whole planet, devolatilizationmelting and/or disruption.This includesdeterminingenergy partitioning,ejecta distributions(with regard to size, velocity, energycontent, and sorting), and condensationphysics of impact produced vapor as well as theimpact productionof aerosols from the liquid and solid state.b.Accomplishments:1) Developeda computermodel which can explicitly describe impact onto a selfgravitatingexponentialplanetary atmosphereand the resulting solid cedflow from a large (10 km-diameter,20 km/sec)bolide onto an earth-sizedplanet with an exponentialatmosphere.We have determinedthatsome 6% of bolide energy couples to the atmosphere.This is close to the value, 5.3%,inferred from similarity variable analysis of the hemisphericalshock wave in the air.2) We have begun test calculationsusing a new smooth particle hydrodynamiccodecapable of studying atmosphericloss and total planet melting and disruptionupon impact oftwo like-sizedself gravitatingplanetary-sizedobjects.3) Determined,via finite-differencecalculations,the effect of planetary crustalstrength and planetarygravity and/or impactor energy on the transition between crateringcontrolledby strength, versus, that controlledby gravity. ngth and crater scale gives rise to gravity-inducedcrater rebound.We have demonstratedthat the crater diameter for transition from simple to complex cratersvaries as g-1 for silicate terrestrialplanets and variesdependingon the effective viscosity of the satellite.from g-0.3 to g-l.0for icy satellites
4) In analyzingtheeffectof impactof a ,we haveexaminedtheexperimentaldatafor impactinducedfine ejectain theaerosol( 11.tm)rangeandfind thatonly 10-5 of the3-20x 1018g of ejectafrom a K/Timpactoris in fines 1 I.tm.This is a factorof 102to alloftedintothestratosphere.c.ProposedProgram1) Conduct atmosphericimpact cratering calculationsto determine the mass ofatmosphereejected and lost from a planet (with exponentialatmospheres)upon impact ofdifferent density, diameter, and velocity bolides.2) Completea study of the effect of gravity, velocity target strength, and projectiledimensionson the depth of excavationand crater shape upon impact of large bolides onplanetarysurfaces.The major effect we expect to study is the scaling appropriatefor highvelocity impacts where shock-inducedvaporizationaccounts for a major fraction of thecrater volume.3) We propose to study very large body impacts with our self-gravitatingsmoothparticle hydrodynamiccode. We expect to examine partitioningof energy and momentumfor different velocity, impact angle and equation of state, as well as the degree of planetarymelting and devolatilization.d.References1. Ahrens,T. J., O'Keefe,J. D., and Lange, M. A., 1989, Formationof atmospheresduring accretion of the terrestrial planets, Planet and Satellite Atmospheres:Originand Evolution,ed. S. Atreya and J. Pollack, U. Ariz. Press, Tucson, AZ., in press.2. Lange, M. A. and Ahrens, T. J., 1989, Atmosphericblow-off during accretionof theterrestrialplanetaryatmospheres,submitted to Icarus.3. O'Keefe,J. D. and Ahrens, T. J., 1989, Impact producedcondensateand droplet sizedistributions,submittedto Icarus.4. O'Keefe,J. D. and Ahrens, T. J., 1989, Impact productionof CO2 by the K-Textinctionbolideand the suddenheatingof the Earth,Nature,338, 247-249.
PROPOSALPRINCIPALINVESTIGATOR:SUMMARYThomasJ. AhrensSeismologicalLaboratoryCalifornia Institute of TechnologyPasadena,CA 91125818/356-6906CO-INVESTIGATOR(S):"ITI"LE"Impact and Collisionalthe Solar SystemProcessesinABSTRACT:a.Objectives:We are carrying out experimentalresearch on mechanicaland thermodynamicaspectsof shock and impact cratering and accretionaryprocesses in solid planets, and theiratmospheresand sateUites. Experimentsare being conducted to understandimpact inducedmelting and vaporizationof minerals on the terrestrial planets, their satellites and the icysatellites of the outer solar system.Recent theories of the impact origin of the moon andimpact devolatilizationof Mercury need to be tested with these data.We measure the shock pressure, and hence, infer correspondingimpact velocitiesofinfalling planetesimalsduring planetary accretion which are required to induce melting ofiron, sulfides, and oxides which precedes planetarycore formation.We are studying therelease of volatiles by impact on water-,carbon dioxide-, sulfur-bearingminerals, andhydrocarbonsin the laboratorybecause this process is believed to underlie the accretion ofplanetaryatmospheres.Studies of noble gas devolatilizationare conducted to constraintheories of atmosphericevolution.We combine experimentaldata on shock inducedmelting and vaporizationand theories of planetary atmosphericgrowth to understandthechemistryof interactionof hot proto-planetarysurfaces with proto-atmospheres.Tounderstandimpact productionof melt and vapor from silicates and formation of magmaoceans on the earth, Moon, and Venus, we are studying shock temperaturesin the mineralsof planetarycrusts and mantles.We are conductingshock loading experimentson rocks inorder to understandand be able to describe their mechanicalresponse which gives rise tothe observed negative Bouguer gravity anomalies observed over impact craters on the earthand moon and seismic velocity deficits beneath impact and explosion craters.b.Accomplishments:1) We have carried out the first experimental studies of the solubility of At" in carbonglass in order to both understandhow noble gases become dissolved in carbonaceousmaterial in the solar nebulae and to provide sample material to conduct impactdevolatilizationexperiments.4
2) conductedonserpentine,serpentineenriched in D, and Murchison carbonaceouschondrite.All threematerials demonstratethat incipient to complete loss of water occurs upon subjectingthesematerials to shock pressuresin the range of 100 to 300 kbar. This is in approximateagreementwith previous experimentsin which only the solid phase was recoveredandanalyzed.Marked depletionof the evolved water and hydrogen in deuteriumby as much asASD - 1007o0 was discovered.We atlributethe preferentialpartitioningof deuteriumintothe solid phase as a result of a kinetic effect in the reaction of iron with water during theshock devolatilizationprocess.If this process occurs during planetary accretion, it leads toa new scenario in which the early deuterium depleted atmosphereis lost by Jeans' loss orby hydrodynamicescape and a later forming atmospherehas a greater D/H ratio. Wepropose that such a scenario might have occurred on Mars and Venus.3) New Hugoniotequation of state data for brucite Mg(OH)2 to 60 GPa demonstratethat like MgO, this mineral does not undergo a phase change over this pressure range.Moreover,these shock data when analyzed in terms of possible breakdownto MgO H20may permit determinationof whether water remains associated in the solid state at highpressuresin planetary mantles.The release isentrope data for brucite shows strongevidence for devolatilizationupon pressure relea3e and needs to be analyzed in detail andcomparedto previous shock recoverydata.4. We have nearly completedconstructionof VISAR (Velocity InterferometerSystem for a ReflectingSurface) which will be used to conduct a rigorous program ofstudy of the impact vaporizationof rocks. Virtually no experimentaldata on the conditionsfor impact volatilizationof rocks are available, yet the most recent theories of the origin ofthe moon and the devolatilizationof Mercury appeal to this, at present, poorly understoodprocess.5) We have conducteda series of impact experimentson blocks of San Marcosgabbro and Bedford limestonewhich demonstrate30 and 50% crack-inducedreduction inP-wave velocity due to 900 MPa shock pressures.One-dimensionalspall experimentstorelate dynamic tensile stress to the resulting velocity deficit and crack density are also beingconductedon these rocks.e.ProposedProgramWe propose to:1) continue our initial study of the uptake of Ar and other noble gases in carbon andhydrocarbonsand study their devolatilizationboth via shock and via annealing.We expectto start dissolvingnoble gases in silicates and also study the devolatilizationbehavior ofother minerals.In collaborationwith Professor Frank Podosek and Dr. ThomasBernatowicz,meteorites.we expectto study the impactdevolatilizationof noble gases from primitive2) search for and analyze the solid phases (MgSiO3,Mg2SiO4,Mg3Si205(OH)4)remainingupon partial devolatilizationof serpentine and Murchisonmeteorites.Theserpentineis predictedto be enriched in D/H. We propose to also study the gaseousspecies producedupon shocking Murchisonmeteorite and elucidate the chemistryandisotopic variationswhich appear to occur in the gas phase.3) conduct further analysis of the equation of state of brucite and construct a modelwhich describes the release isentropesin terms of the equation of state and thermodynamicpropertiesof MgO and H20.4) conduct further experimentson the cracking and hence density and seismicvelocity deficit induced by shock waves in both hemisphericaland planar geometry in dryand wet rocks. We expect to examine the data prescribingthe regions of velocity deficits
minewhatconstraintstheseanomaliescanplaceon theimpactprocess.5) Conductfurtherexperimentalimpactstudiesof gon theproductionof aerosol-sizedejecta.d. References1. Lange,M. A. andAhrens,2.3.4.5.T. J., 1987, Impact experimentsin low temperatureice,Icarus,69, p. 506-518.Tyburczy,J. A. and Ahrens, T. J., 1988, Dehydrationkinetics of shocked serpentine,Proceedingsof the 18th Lunar and PlanetaryScience Conference,CambridgeUniv.Press, p. 435-442.Schmitt, D. R. and Ahrens, T. J., 1988, Shock temperaturesin silica glass, J.Geophys.Res., in press.Tyburczy,J. A., Krishnamurthy,R. V., Epstein,S., and Ahrens, T. J., 1989, Impactinduced devolatilizationand hydrogen isotopic fractionationof serpentine:Implicationsfor planetaryaccretion, submitted, Earth Planet. Sci. Letr.Tan, H. and Ahrens, T. J., 1989, Shock-inducedpolymorphictransitionin quartz,carbon, and boron nitride, J. Appl. Phys.6
:INVESTIGATORS:TITLE:89-1386SUMMARYJames R. ArnoldCalifornia Space Institute, A-021Scripps Institution of OceanographyUniversity of California, San Diego"La Jolla, CA 92093(619)534-2908K. NishiizumiE. M. ShoemakerAge and ErosionalUsing CosmogenicHistory of MeteoriteNuclidesCratersABSTRACT:(a) We propose to measure the age of the five known meteorite impact craters in Australia,by acombination of measurementsof cosmogenic nuclides in meteorite specimens and in samples of quartzbearing rocks exposed by the impact.Samples of both sorts have been collected for this work by E.and C. Shoemaker;further collectionsare planned.For older craters the terrestrial quartz data willmeasure primarily erosion rates in crater and ejecta materials; for younger ones crater age determinationmay be possible.The most important radionuclidesare 14C (to be measured at Arizona), 10Be and26A1 (to be measured at Pennsylvania).These measurementscan provide estimates of the impact rateson earth of iron and stony-iron meteoroids in the 1-50 meter size range, and of the rate of disappearanceof impact craters in arid regions.As part of this study we will continue our dating and erosion studiesof Meteor Crater, Arizona.(b) New Proposal(c) With our AMS colleagueswe will measure 14C, 10Be, and 26A1 in terrestrial quartz collectedthe five Australian craters and at Meteor Crater, Arizona. We will also measure these radionuclidesmeteoritic metal collected at these craters. Some further sampling will be carried out in Auslralia.(d)NishiizumiNishiizumiet al (1989b)et al (1989c)atin
OR:SCIENTIFICRaymondE. Arvidson.ProfessorMcDonnellCenter for the Space SciencesDepartmentof Earth and PlanetarySciencesWashingtonUniversitySt. Louis, MO 63130Telephone:314-889-5609EdwardA. Anne KahleRalphDanielJamesNASAKahnMcCleeseR. StephenSaundersJakob Van ZylRichardZurekJet rResearchScientistGreeleyState UniversityPollackAmes ityof ArizonaANALYSISOF REMOTESENSINGTHE TERRESTRIALPLANETSFOR THESURFACESOFAoObjectives:Acquisitionand analysis of airborneAVIRIS,TIMS,quad-polradar, andgrounddata over GRSFE test sites to test models for-extractionof surface propertyinformation.Data and documentationto be archivedfor planetarycommunityuse.Geologyof Venus,includingrates of resurfacingby both endogenicand exogenicprocesses.Surficialgeologyof Mars using ticrelationshipsbetweenlocal bedrockand sedimentarycover.B,Accomplishments:(I) Detailedplanningfor joint EL/EE airborneand ground GRSFEIdeploymentusing AVIRIS,TIMS,quad-polradar systems;(2) Used Seasat data to simulategeologicalinformationin Venera and Magellanimages:(3) Re-evaluatedevidenceforclusteringof craterson Venus and whethera productionpopulationexists; (4) Generatedreview articles(with H. Moore,J. Gooding)on Viking Lander results,on PlanetaryGeology,and on Martianweathering(with Goodinget al.); (5) Analyzedimpact craterpopulationon Mars south pole; (6) Pursueduse of visible,thermal,microwavetocharacterizeand map Mars surficialmaterialsexposedin Oxia and surroundings;(7)Photogeologicalanalysesof GoldstoneVenus images.C.ProposedWork in 1990:(!) Reduce and analyzeairborneand groundremote sensingdataover GRSFE test sites in Mojave desert.Assemblyof archive of reduceddata anddocumentation.With PDS help. publish set of 10 CD-ROMsof GRSFE data for communityuse: (2) Exploreseparationof reflectivityfrom roughness,and geologicalramificationsofresults using GoldstoneVenus data;(3) Implementvisible throughthermalIR radiativetransfermodels for extractionof surface informationfrom Viking data; (4) CharacterizeMartiansurface materialsin northernequatorialregion using multi-angleViking images,IRTM.and radar data;(5) Studies of aeolian geologyof Venus with Greeley.D.Publications:SeeAppendixII and Tableof Contents.
oneNumber)VictorSUMMARYR.BakerDepartmentof Geosciences,Arizona,Tucson,AZ 85721Universityof(602) lowline.Letteredparagraphs(a) through(d)shouldinclude:a. onof thework;b.briefstatementoftheaccomplishmentsof theprioryear,or"newproposal;"c.brieflisdingof whatwillbedonethisyear,wellas howandwhy;andd. oneor twoof .SoDeterminethe origins,ages, and s,and relatedhydrogeomorphicfeaturesMars throughphotointerpretationof orbitalimagery,comparisonterrestrialanalogs,and theoreticalstudiesof fluvial/hillslopemechanicsand hydrologicprocesses.i) Appliednewof to the calculationflood parametersfor the ChanneledScablandand forchannels.2) Improvedthe understandingof sappingfor some Martianvalleynetworksby studiesof Hawaiianvalleys.3) Developeda preliminaryhydrothermalmodeltothe originof most Martianvalleys.4) Documentedthecharacterof valleyson Alba Paterain relationto thetimingand inferredprocessesof valleyformationon Mars.Developnew theoreticalcriteriafor relatingMars channel-erosionalevidenceto causativeflow processmechanics.Use appropriatefielddata from ChanneledScablandto test model predictions.Adapt thermalsystems.modelsCompareused for simulatingpredictionsof thehydrothermalhypothesisto atmosphericmodelsof pale.climaticchangeon Mars.Continueto use is,photointerpretation,and theoreticalanalysisof advanceunderstandingof Mars hydrogeomorphology,and extendthisexperienceto megageomorphologicalcomparisonof Earth,Mars,andVenus.DoBaker,V.R.,1988, Geologicalfluvialgeomorphology:GeologicalSocietyof AmericaBulletin,v. i00, p. 1157-1167.Baker,V.R.,1988, The channelsof Mars, in The NASA MarsConference:AmericanAstronaut.S.c., v. 71, p. 75-90.as
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PROPOSALPRINCIPALINVESTIGATOR:W. BruceSUMMARYBanerdtJet PropulsionLaboratory,MS 183-5014800 Oak Grove Drik, ePasadena,CA 91109(818) 354-5413(FTS) icsABSTRACTA. The broad objectiveis to better understandthe mechanicalthe crusts and upper mantles of the solid planets and satellites.behavior,structure,and historyofB. During the past six months we have:(i) reconcileddifferencesbetween existing stress modelsfor Tharsis and generatedhigh resolutionplots for use in comparingmapped tectonic features withtheoreticalpredictions;(ii) continuedthe investigationof mechanical/petrologicalconstraintson theevolutionof Tharsis, with one paper publishedand another manuscriptsubmittedfor publication;(iii) completedthe study of early thermal gradients on Europa using lithosphericstrength envelopesand observationsof extensionaltectonic features, with a manuscriptsubmitted for publication.C. I proposeto do the following:(i) continue the investigationof the effects of mantle dynamicson surface stress fields in planetary lithospheres,and perform regional studies of the state of stressin selectedareas on Venus at moderateresolutionin order to refine regionalmodelsof thelithosphereand upper mantle of Venus; (ii) continue the work underway using stress predictions,petrologicalconstraints,and tectonicobservationsto test variousmodels for the thermalandtectonic history of the Tharsis region of Mars, and develop a general thermomechanicalmodellingframework for further extending these studies; and (iii) investigate tectonic deformationprocessesand subsurfacestructureon Io using realistic rheologicalassumptions.D.SelectedReferences:Baner
McEwen, Alfred S. McFadden, Lucy-Ann McGill, George E. McKay, christopher McKinnon, William B. Melosh, H. J. Metzger, Albert E. Moore, Henry J. Mouginis-Mark, Peter J. NASA/JSC U HI AZ St U U AZ M.I.T. U Pittsburgh JPL PSI U HI Brown U WA N AZ U U AZ U VA U CO U CA, Berkeley U VA JPL UCLA US
Listed under: Home Automation Projects, LED Projects, Projects 23. Bootload an Arduino with a ZIF Socket Bootloading an Arduino with a ZIF socket allows you to easily program a lot of chips at once without worrying about . 9/6/22, 2:15 PM Advanced View Arduino Projects List - Use Arduino for Projects. Projects Projects Projects. Projects .
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projects. These projects can be managed code COBOL projects or native code COBOL projects or can be C# projects or VB.NET projects, etc. Visual COBOL projects can contain only COBOL programs or classes but these programs and classes can interact with the programs or classes contained within projects written in a different language like C#.
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