NASA/JPL

J. Y. P. Mui, Low Cost Solar Array Project, NASA/JPL Contract 954334, Union Carbide Corp., June 1979. 

Fig. 3.14 Left. NASA Mars-Exploration-Rover (artist view courtesy NASA, JPL, Cornell). On the front side of the Rover the robotic arm carrying the Mossbauer spectrometer and other instruments can be seen in stowed position. Right, robotic arm before placement on soil target at Victoria crater rim, Meridian Planum, Mars. The Mossbauer instrument MIMOS II with its circular contact plate can be seen, pointing towards the rover camera. See also Sect. 8.3...

Fig. 8.27 NASA Mars-Exploration-Rover artist view (courtesy NASA, JPL, Cornell). On the front side of the Rover, the robotic arm (IDD) carrying the Mossbauer spectrometer and other instruments can be seen...

Fig. 8.36 Leyt Spectrum of the soil close to the crater rim where Opportunity entered and exited the crater. The basaltic soil is unusually high in hematite (but no indication of significant contribution Irom hematitic spherules). Middle rover tracks. Right 750 m diameter (. 75 m deep) eroded impact crater Victoria Crater, formed in sulfate-rich sedimentary rocks. Image acquired by the Mars Reconnaissance Orbiter High-Resolution Science Experiment camera (Hirise). The red line is the drive path of Opportunity exploring the crater. (Courtesy NASA, JPL, ASU, Cornell University)...

Fig. 8.38 (Left) The Mossbauer spectrum of the rock called Heat Shield rock, clearly shows with high intensity the mineral Kamacite, an Fe-Ni alloy with about 6-7% Ni (Right) The iron-nickel meteorite Meridiani Planum (originally called Heat Shield Rock ) at Opportunity landing site, close to the crater Endurance. The meteorite is about 30 cm across (Courtesy NASA, JPL, Cornell University)...

Fig. 11.1 Pseudo-colour radar picture of the north polar region of Titan (NASA/JPL, 2007)...

We acknowledge funding by NSF grant AST-0307851, NASA/JPL contract 1228235, the David and Lucile Packard Foundation, Robert J. Huskey Travel fellowship, AAS International Travel Grant, and the F.H. Levinson Fund of the Peninsula Community Foundation. 

Figure 10.1 This image taken by the Cassini probe is in the infrared centred at 980 nm (Image scale is 7 kilometers per pixel) and shows features on the leading hemisphere of Titan, including the bright, crescent-shaped Hotei arcus (right of center), which is also informally called "the Smile" by researchers. (Reproduced by permission of NASA/JPL/Space Science Institute)...

WB DeMore, SP Sander, DM Golden, RF Hampson, MJ Kurylo, CJ Howard, AR Ravishankara, CE Kolb, MJ Molina. Chemical Kinetics and Photochemical Data for Use in Stratospheric Modeling, JPL Publication 97-4. Pasadena NASA JPL, 1997. 

NASA-JPL. 1999. Public health assessment for jet propulsion laboratory (NASA), Pasadena, Los Angeles County, California. Region 9, CERCLIS no. CA9800013030. Atlanta, GA Agency for Toxic Substances and Disease Registry, Division of Health Assessment and Consultation. PB 99 167 470. 

Figure 6.1. The Jovian moon lo deep ultraviolet (UV) photolysis of its methane atmosphere proceeds with electron ejection, generating the molecular ion of methane (see color insert). NASA JPL Galileo program image from Voyager 1, http //www.jpl.nasa.gov/galileo/io/...

Genesis spacecraft with solar wind collectors deployed. Image courtesy of NASA/JPL-Caltech. 

NASA / JPL-Geltech / L Allen G.X, Koenig [Harvard-Sm, iionran CfA)... 

Tables on the "reaction probalility or "uptake coefficient" have been summarized for various heterogeneous reactions in a recent review article [87], and by the IUPAC [88] and NASA-JPL [86] evaluation teams. For the purpose of this article, a rough comparison is made of the uptake rates for the reactions (1) to (5) on the different type surfaces. Three major type of surfaces have been considered a) NAT, or Type I PSC, b) Water ice, or Type II PSC and c) sulfuric acid aerosol, which is normally a liquid surface generally composed of 60-80 wt % H,S04 and 40-20 wt % H,0 also considered is the solid form SAT (sulfuric acid tetrahydrate) with a composition of 57.5 wt % H,S04. The importance of chlorine activation on sulfuric acid solutions has been demonstrated in a recent article [89]. Halogen activation on seasalt material will shortly be reviewed as part of the tropospheric processes.

Fig. 5.13. The landing site (Gusev Crater) of the Mars Spirit rover. Courtesy NASA / JPL/Caltech...

Fig. 5.20. An artist rendition of a cross-sectional view of Europa. Courtesy NASA/JPL/Caltech...

We also thank the following publishers for permission to reproduce published graphs, tables, and text American Journal of Science, ASM Press, Cambridge University Press, Cold Regions Research and Engineering Laboratory, Elsevier Limited, Mary Ann Liebert Inc., NASA/JPL/Caltech, and Springer Science and Business Media. 

The aim of the present work is to derive the enthalpies of formation of HOI and IONO2 via ab initio methods. The latter is used to investigate the kinetics of reaction (5). The NASA-JPL recommendation [9] for AfH(HOI) is based on calculations by Hassanzadeh and Irikura [10] and previous work from our laboratory on OH + CF3I kinetics [11]. In the intervening decade there have been revisions to most of the ancillary thermochemical and kinetic data used in these calculations, and advances in computational technology and methodology make... 

These estimates bracket the NASA-JPL and lUPAC recommendations of 6.5x10 and 7.7 x 10 cm molecule s [9,60]. It is therefore possible fo reconcile fhe thermochemistry proposed here with the observed lO + NO2 recombination kinetics while employing reasonable input parameters for the unimolecular model. Nevertheless it must be stressed, as emphasized earlier [16], that there is considerable uncertainty in some of the input parameters to an RRKM analysis, especially the Frot term. It is of interest to compare the present kinetic calculations with the Multiwell [61] Master Equation calculations on this system by Golden [16]. He used a Morse potential to locate the centrifugal maximum, and from the bond extension Frot 2.1 is derived, about 1/7 of fhaf used here. On the other hand, the higher Eo value yields a density of sfafes larger by a facfor of 6, and fhese two factors largely cancel. 

D. E. Brinza, S. Y. Chung, T. K. Minton and R. H. Liang, Final Report on the NASA/JPL Evaluation of Oxygen Interactions with Materials — 3 (EOIM-3), NASA Contractor Report 198865, JPL Publication 94-31 (NASA, Pasadena, CA, 1994). 

George T (2003) Overview of MEMS/NEMS technology development for space applications at NASA/JPL. SPIE 5116 136-148... 

This image of the Martian rock "Humphrey" shows a hole made by a grinding tool carried on the Mars Exploration Rover Spirit, which landed on Mars on January 4, 2004. The grinding process revealed the inner structure of the rock and produced a sample that could be tested for chemical composition. (NASA/JPL/Photo Researchers, Inc.)... 

NASA/JPL (Jet Propulsion Laboratory California Institute of Tech-nology)... 

FIGURE 17-18 Spectra from Mars rover Spirit showing an unidentified mineral containing txiund water in its crystal structure. Minerals such as zeolites and gypsum are possible candidates. Mini-TES = mini thermal-emission spectrometer. (Courtesy of NASA/JPL/Arizona State University.)... 

Fig. 1.4 FIR instruments in chronological order from left to right IRAS (1983), 0.6-m dish cooled at 2K and operating at 12, 25, 60 and 100 xm ISO (1995), 0.6-m dish cooled at 2-3 K operating in the band 3-200 p.m Spitzer (2003), 0.85 m dish cooled at 4 K operating in the band 3-180 xm Herschel (2009), 3.5-m dish cooled at 80 K operating in the band 55-670 xm. [Credit, respectively NASA/JPL ESA NASA/JPL-Caltech ESA/AOES Medialab, background from Hubble Space Telescope image (NASA/ESA/STScI)]...

The home page of the NASA/JPL Gravity Recovery and Climate experiment to make precise measurements of the earth s gravitational field... 

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