nasa scientific and technical aerospace reports phần 6 docx

of physics The focus is on the appearance of chaos in a beam distribution A study of the problem is based on two observations The First observation is that using Lyapunov method and its extension we obtain solutions of partial differential equations Using this approach we discuss the problem of finding a solution of Vlasov-Poisson equation, i.e., some stationary solution where we consider magnetic field as some disturbance with a small parameter Thus the solution of Vlasov equation yields an asymptotic series such that the solution of Vlasov-Poisson equation is the basis solution for one The second observation is that physical chaos is weakly limit of, well known, the Landau bifurcation’s This fact we have proved using ideas on the Nature of Turbulence NTIS Partial Differential Equations; Vlasov Equations; Poisson Equation; Particle Accelerators; Beams (Radiation) 20050169872 Brookhaven National Lab., Upton, NY, USA Surface Reactions Studied by Synchrotron Based Photoelectron Spectroscopy Hrbek, J.; 1999; 70 pp.; In English Report No.(s): DE2004-770789; BNL-66043; No Copyright; Avail: Department of Energy Information Bridge The goal of this article is to illustrate the use of synchrotron radiation for investigating surface chemical reactions by photoelectron spectroscopy A brief introduction and background information is followed by examples of layer resolved spectroscopy, oxidation and sulfidation of metallic, semiconducting and oxide surfaces NTIS Chemical Reactions; Photoelectron Spectroscopy; Surface Reactions; Synchrotron Radiation 20050169873 Brookhaven National Lab., Upton, NY, USA, Florida Univ., Gainesville, FL, USA Investigation of Coherent Emission from the NSLS VUV Ring Carr, G L.; Kramer, S L.; Murphy, J B.; La Veigne, J.; Lobo, R P S M.; Mar 1999; 10 pp.; In English Report No.(s): DE2004-770804; BNL-66994; No Copyright; Avail: Department of Energy Information Bridge Bursts of coherent radiation are observed from the NSLS VUV ring near a wavelength of 7mm The bursts occur when the electron beam current exceeds to threshold value which itself varies with ring operation conditions Beyond threshold, the average intensity of the emission is found to increase as current squared With other parameters held nearby constant the threshold current is found to increase quadratically with the synchrotron frequency, indicating a linear dependence on momentum compaction It is believed that the coherent emission is a consequence of micro-bunching of the electron beam due to the microwave instability NTIS Coherent Radiation; Synchrotrons; Synchrotron Radiation; Ultraviolet Radiation 20050169875 Brookhaven National Lab., Upton, NY Instabilities in the Spallation Neutron Source (SNS) Blaskiewicz, M.; 1999; 10 pp.; In English Report No.(s): DE2004-770762; BNL-65933; No Copyright; Avail: Department of Energy Information Bridge The 2MW Spallation Neutron Source (SNS) will have a D.C beam current of 40 A at extraction, making it one of the worlds most intense accelerators Coherent instabilities are a major concern and efforts to predict beam behavior are described NTIS Neutron Sources; Spallation; Stability; Particle Accelerators 20050169876 Brookhaven National Lab., Upton, NY Flying Wire System in the AGS Huang, H.; Buxton, W.; Mahler, G.; Marusic, A.; Roser, T.; 1999; 10 pp.; In English Report No.(s): DE2004-770758; BNL-65923; No Copyright; Avail: Department of Energy Information Bridge As the AGS prepares to serve as the injector for RHIC, monitoring and control of the beam transverse emittance become a major and important topic Before the installation of the flying wire system, the emittance was measured with ionization profile monitors in the AGS, which require correction for space charge effects It is desirable to have a second means of measuring profile that is less dependent on intensity A flying wire system has been installed in the AGS recently to perform this task This paper discusses the hardware and software setup and the capabilities of the system NTIS Emittance; Wire; Synchrotrons 295 20050169878 Brookhaven National Lab., Upton, NY, USA Design of a Resonant Extraction System for the AGS Booster Brown, K.; Cullen, J.; Glenn, J W.; Lee, Y Y.; McNerney, A.; 1999; 10 pp.; In English Report No.(s): DE2004-770771; BNL-65976; No Copyright; Avail: Department of Energy Information Bridge The Booster Application Facility (BAF) will employ heavy ion beams of many different ion species and at beam energies ranging from 0.04 to 3.07 GeV/nucleon Resonant extraction is required in order to deliver a continuous stream of particles In this report they describe the beam requirements and the system design The basic design is a third integer resonant extraction process which employs a single thin magnetic septum and a thick septum ejector magnet The expected extraction efficiency is about 85%, based on the thin septum thickness and the predicted step size of the resonant beam at the septum This is more than sufficient for the low intensity low energy heavy ion beams needed for the BAF In this report they present a detailed discussion of the design of the various elements and a discussion of the detailed modeling of resonant extraction from the AGS Booster The extraction process was modeled using a BNL version of MAD which allowed them to interactively observe detailed particle tracking of the process This was a key tool to have in hand which permitted them to pose and answer various questions in a very short period of time NTIS Extraction; Ion Beams; Structural Design 20050169883 Brookhaven National Lab., Upton, NY Collimator Systems for the SNS Ring Ludewig, H.; Simos, N.; Walker, J.; Thieberger, P.; Aronson, A.; 1999; 10 pp.; In English Report No.(s): DE2004-770754; BNL-66594; No Copyright; Avail: Department of Energy Information Bridge The requirements and performance goals for the collimators are to reduce the uncontrolled beam loss by 2 x 10(sup -4), absorb 2 kW of deposited heat, and minimize production and leakage of secondary radiation In order to meet these requirements a self-shielding collimator configuration consisting of a layered structure was designed The front layers (in the direction of the proton beam) are relatively transparent to the protons, and become progressively less transparent (blacker) with depth into the collimator In addition, a high density (iron) shield is added around the outside The protons will be stopped in the center of the collimator, and thus the bulk of the secondary particles are generated at this location The conceptual design described, the method of analysis discussed, and preliminary performance parameters outlined NTIS Collimators; Proton Beams 20050169884 Brookhaven National Lab., Upton, NY Optimization of the Parameters in the RHIC Single Crystal Heavy Ion Collimation Biryukov, V M.; Chesnokov, Y A.; Kotov, V I.; Trbojevic, D.; Stevens, A.; 1999; 10 pp.; In English Report No.(s): DE2004-770753; BNL-69593; No Copyright; Avail: Department of Energy Information Bridge In the framework of the project to design and test a collimation system prototype using bent channeling crystal for cleaning of the RHIC heavy ion beam halo, the authors have studied the optimal length and bending angle of a silicon (110) single crystal proposed to be a primary element situated upstream of the traditional heavy amorphous collimator Besides the matters of the channeling and collimation efficiency, they also looked into the impact the crystal may have on the non-channeled particles that go on circulating in the ring, so as to reduce the momentum offset of the particles scattered of the crystal NTIS Collimation; Particle Accelerators 20050169885 Brookhaven National Lab., Upton, NY Design of an AC-Dipole for use in RHIC Parker, B.; Bai, M.; Jain, A.; McIntyre, G.; Meth, M.; 1999; 10 pp.; In English Report No.(s): DE2004-770751; BNL-66578; No Copyright; Avail: Department of Energy Information Bridge The authors present two options for implementing a pair of AC-dipoles in RHIC for spin flipping, measuring linear optical functions and nonlinear diagnostics AC-dipoles are magnets that can be adiabatically excited and de-excited with a continuous sine-wave in order to coherently move circulating beam out to large betatron amplitudes without incurring emittance blow up The AGS already uses a similar device for getting polarized proton beams through depolarizing resonances By placing the magnets in the IP4 common beam region, two AC-dipoles are sufficient to excite both horizontal and vertical motion in both 296 RHIC rings While they initially investigated an iron-dominated magnet design, using available steel tape cores; they now favor a new air coil plus ferrite design featuring mechanical frequency tuning, in order to best match available resources to demanding frequency sweeping requirements Both magnet designs are presented here along with model magnet test results The challenge is to make AC-dipoles available for year 2000 RHIC running NTIS Particle Accelerators; Betatrons; Continuous Radiation 20050169886 Brookhaven National Lab., Upton, NY BNL-Built LHC Magnet Error Impact Analysis and Compensation Ptitsin, V.; Tepikian, S.; Wei, J.; 1999; 10 pp.; In English Report No.(s): DE2004-770749; BNL-66506; No Copyright; Avail: Department of Energy Information Bridge Superconducting magnets built at the Brookhaven National Laboratory will reinstalled in both the Insertion Region IP2 and IP8, and the RF Region of the Large Hadron Collider (LHC) In particular, field quality of these IR dipoles will become important during LHC heavy-ion operation when the (beta)* at IP2 is reduced to 0.5 meters This paper studies the impact of the magnetic errors in BNL-built magnets on LHC performance at injection and collision, both for proton and heavy-ion operation NTIS Particle Accelerators; Superconducting Magnets 20050169951 Lafayette Coll., Easton, PA, USA Volumetric and Optical Studies of High-Pressure Phases of MgSO4-H2O with Applications to Europa and Mars Hogenboom, D L.; Dougherty, A J.; Kargel, J S.; Mushi, S E.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color and black and white illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document We report the first measurements and images obtained using a new high-pressure volumetric cell with sapphire windows to study phase equilibria in a 17 wt.% sample of MgSO4 in H2O Magnesium sulfate was chosen for study because it is regarded as among the most likely constituents of Europa’s ocean and icy shell and constitutes key salts on Mars The 17 wt.% composition is close to the eutectic The new data, when combined with data from our earlier study of the density vs pressure and temperature of MgSO4 solutions, will enable us to identify the phases with greater certainty and describe the phase transitions with greater precision For example, we observe that the process of solidification of the supercooled sample involves a sequence in which a fine-grained structure forms rapidly, followed by the generation of liquid and then slower growth of large-grained crystals The addition of visual images to our capability to track the changes in sample volume is also valuable to assess both stable and reversible phase changes and metastable phase transitions Metastability has proven a key aspect of this system in the lab and in nature Additional information is included in the original extended abstract Author (revised) Magnesium Sulfates; Water; Volumetric Analysis; High Pressure; Phase Stability (Materials) 20050170464 SEMATECH, Austin, TX, USA The Quantitation of Surface Modifications in 200 and 300 mm Wafer Processing with an Automated Contact Angle System Carpio, Ronald; Hudson, David; 1998 IEEE/SEMI Advanced Semiconductor Manufacturing Conference And Workshop; [1998], pp 272-277; In English; See also 20050170458; Copyright; Avail: Other Sources Contact angle measurement, using advanced instrumentation, is assuming an increased role in monitoring those semiconductor manufacturing processes which modify the surface characteristics of wafers Such measurements can provide rapid, nondestructive, and spatially as well as time resolved data in an automated mode This information can be related to processing uniformity and can in many cases provide information on the chemical state of the surface Illustrations are provided in the wafer cleaning, lithography, and interconnect areas New application areas illustrated include measuring the uniformity of UV photostabilization processes, measurement of contrast curves, and determination of receding and advancing contact angles of processed copper wafers Author Quantitative Analysis; Surface Defects; Wafers; Automatic Control 297 20050170468 International Business Machines Corp., Essex Junction, VT, USA Wafer Line Productivity Optimization in a Multi-Technology Multi-Part-Number Fabricator Maynard, Daniel N.; Rosner, Raymond J.; Kerbaugh, Michael L.; Hamilton, Richard a.; Bentlage, James R.; Boye, Carol A.; 1998 IEEE/SEMI Advanced Semiconductor Manufacturing Conference And Workshop; [1998], pp 34-42; In English; See also 20050170458; Copyright; Avail: Other Sources Successful semiconductor manufacturing is driven by wafer-level productivity Increasing profits by reducing manufacturing cost is a matter of optimizing the factors contributing to wafer productivity The major wafer productivity components are chips per wafer (CPW), wafer process or fabricator yield (WPY) and wafer final test WFT) or functional yield CPW is the count of product chips fitting within the useable wafer surface, and is dependent upon the chip size, dicing channel (kerf) space, and wafer-field size WPY yield is the percentage of wafers successfully exiting the line; losses include scrap for broken wafers and failed-wafer specifications WFT yield is the percent of chips that meet all final parametric functional electrical test specifications Derived from text Wafers; Productivity; Optimization; Chips 20050170471 International Business Machines Corp., Essex Junction, VT, USA Correlation of Digital Image Metrics to Production ADC Matching Performance Blais, Jennifer; Fischer, Verlyn; Moalem, Yoel; Saunders, Matthew; 1998 IEEE/SEMI Advanced Semiconductor Manufacturing Conference And Workshop; [1998], pp 86-92; In English; See also 20050170458; Copyright; Avail: Other Sources Automatic Defect Classification (ADC) tool matching requires that consistent quality images captured on all tools Image metrics have been developed and the variance of these metrics have been correlated to classifier matching It is shown that in order to maintain matching, image color balance, focus, and shadowing need to be monitored and maintained at acceptable values Of these metrics, inappropriate color balance has the greatest affect on matching Author Image Analysis; Defects; Classifications 20050170476 Fairchild Semiconductor Corp., South Portland, ME, USA In-Situ Gate Oxide/Electrode Deposition for a 0.5 micron BiCMOS Process Flow Carbone, Thomas A.; Solomon, Gary; 1998 IEEE/SEMI Advanced Semiconductor Manufacturing Conference And Workshop; [1998], pp 174-180; In English; See also 20050170458; Copyright; Avail: Other Sources A method of depositing the gate oxide and electrode in a single chamber for BiCMOS processing is discussed The advantages of the deposition of in-situ gate electrode (DIGE), over the conventional two step oxidation and polycrystalline silicon deposition is related to cycle time and increased gate oxide integrity TEM images and a correlation to metrology measurements are presented Author Deposition; Oxides; Gates (Circuits); Electrodes 20050170492 Analog Devices, Inc., Woburn, MA, USA A Comparison of Critical Area Analysis Tools Fitzpatrick, Sean; ODonoghue, Geoffrey; Cheek, Gary; 1998 IEEE/SEMI Advanced Semiconductor Manufacturing Conference And Workshop; [1998], pp 31-33; In English; See also 20050170458; Copyright; Avail: Other Sources The application of Critical Area Analysis has become more mainstream in the semiconductor industry The critical area of a circuit is a measure of the sensitivity of a product layout to defects, which is subsequently used in accurate yield models Intuitively, if a circuit is more dense, the defect sensitivity is higher than a less dense circuit Only recently, have commercial tools become available to measure critical area Several approaches have been developed to measure layout critical area, a short summary of each approach is described, as well as a brief description of how critical area is incorporated into a yield model The results of applying critical area analysis are then described Author Semiconductors (Materials); Defects; Layouts 298 20050170495 Georgia Inst of Tech., Atlanta, GA, USA Towards Real-Time Fault Identification in Plasma Etching Using Neural Networks Zhang, Ben-Yong; May, Gary S.; 1998 IEEE/SEMI Advanced Semiconductor Manufacturing Conference And Workshop; [1998], pp 61-65; In English; See also 20050170458 Contract(s)/Grant(s): NSF DDM-93-58163; Copyright; Avail: Other Sources Abstract - As the IC industry moves further into submicron fabrication technology, optimal utilization of fabrication equipment is essential Timely and accurate equipment malfunction identification can be a key to success It is also desirable to predict malfunctions well in advance of their actual occurrence In this paper, we use neural networks to model time series data extracted from a three-step plasma etch process for defining active areas in a CMOS ASIC circuit The data consists of real-time measurements from the three-step etch process for 40,000 silicon wafers collected over a six-month per’rod from a Drytek plasma etcher Two types of anomalies were present in this data: 1) constant or slowly advancing time (indicating the presence of a machine fault); and 2) missing steps (indicating something unexpected happened during the etch) Data preprocessing is carried out to eliminate any data acquisition errors in the original data and to correctly separate the total time sequence into three sub-sequences (one for each etch step) A pattern recognition technique is used to determine the process step number for each record The classification results and the prediction error demonstrate accurate determination of the etch step number from the chamber state Dynamic neural network models are then constructed for each step We initially focus on modeling the time series associated with chamber pressure The time series of pressure data is modeled as a function of its previous values and the current time We use this approach to construct time series models of the pressure variations in the etching system using only an initial condition and the time value as inputs Author Real Time Operation; Fault Detection; Plasma Etching; Neural Nets; Pattern Recognition 20050170497 Cypress Semiconductor Corp., San Jose, CA, USA Development of New Methodology and Technique to Accelerate Region Yield Improvement Wong, K.; Mitchell, P.; Nulty, J.; Carpenter, M.; Kavan, L.; Jin, B.; McMahon, G.; Seams, C.; Fewkes, J.; Gordon, A.; Sandstrom, C.; 1998 IEEE/SEMI Advanced Semiconductor Manufacturing Conference And Workshop; [1998], pp 82-86; In English; See also 20050170458; Copyright; Avail: Other Sources A focus in region yield is demonstrated to improve the systematic yield from 75% to upper 90% to achieve quick learning curve in Defect Density on new products A learning curve to drive both the Random and Systematic yield simultaneously are important to accelerate the yield learning on new products as well as existing products This paper showed the systematic yield improvement from a module integration issue to an equipment setup and capability issue A new methodology has been defined to look at the edge region of the wafer, and is used to address wafer edge issue with systematic approaches to drive yield improvement The process variability on the center of the wafer is low, but as one approach the edge of the wafer, large process variations arise which depress the yield at the edge of the wafers This decrease in yield can be caused by technology architecture, process uniformity, wafer misalignment and mark alignment scheme issues Author Yield; Defects; Learning Curves; Technology Assessment 20050170498 International Business Machines Corp., Essex Junction, VT, USA Intelligent Line Monitor: Maximum Productivity through an Integrated and Automated Line Monitoring Strategy Pilon, Tom; Burns, Mark; Fischer, Verlyn; Saunders, Matthew; 1998 IEEE/SEMI Advanced Semiconductor Manufacturing Conference And Workshop; [1998], pp 93-102; In English; See also 20050170458; Copyright; Avail: Other Sources This paper describes an Intelligent Line Monitor system and highlights the features which make it superior to conventional line monitor systems By citing examples from an IBM 0.25 microns technology fabricator, we show that an inte_ated and automated line monitoring strategy reduces time-to-results, provides a low cost-of-ownership, and delivers a short time to return-on-investment The natural expansion and growth possibilities of such as system are also explored Author Monitors; Smart Structures; Automatic Control 20050170512 Analog Devices, Inc., Wilmington, MA, USA Manufacturing and Reliability Improvements in Metal-Oxide-Metal Capacitors - MOMCAPs Lowell, Larry; 1998 IEEE/SEMI Advanced Semiconductor Manufacturing Conference And Workshop; [1998], pp 181-186; In English; See also 20050170458; Copyright; Avail: Other Sources 299 Metal-Oxide-Metal Capacitors, MOMCAPs, have historically demonstrated less than optimal leakage and breakdown characteristics and yields Additionally, the Cpk for capacitance is low Any previous work done to improve the die! tric uniformity has resulted in further degradation of the capacitor characteristics In this paper we will show that the parametric and reliability characteristics are very dependent on the bottom plate material Our standard Ti bottom plate interacts with the capacitor dielectric resulting in degraded performance That interaction renders a more uniform dielectric film unusable We have developed a MOMCAP using TiW as the bottom plate electrode, which minimizes those interactions and improves capacitor characteristics Author Manufacturing; Mom (Semiconductors); Reliability; Capacitors 20050170522 KLA-Tencor Corp., Orlando, FL, USA Correlation of Ellipsonometric Modeling Results To Observe Grain Structure for OPO Film Stacks Robinson, Tod E.; 1998 IEEE/SEMI Advanced Semiconductor Manufacturing Conference And Workshop; [1998], pp 278-288; In English; See also 20050170458; Copyright; Avail: Other Sources One significant, but potentially variable, parameter in the deposition and subsequent processing of polysilicon is its microstructure The purpose of this work was to correlate the model parameters, in this case, percent volume fraction of phase components of polysilicon, generated by regression of model dispersion using Bruggerman Effective Media Approximation to data acquired by the Spectroscopic Ellipsometry technique Several samples are prepared consisting of SiO2/Undoped Poly Si / SiO2 film stacks in order to measure their as-deposited average grain sizes Ellipsonometric data is obtained for the center site of each sample which are then compared to AFM results from similar samples Various grain geometry approximations are applied along with the assumption that the polysilicon structure may be modeled to consist of three components; crystalline Si in a continuous Amorphous Si matrix, and voids A mathematical relation is established between the percent concentration of crystalline Silicon and the mean grain size for the two cases of equiaxed and columnuar microstructures Results indicate there to be good correlation with AFM measured grain sizes Additional work is required to further demonstrate the correlation, and develop software applications to enable in-line product monitoring Author Ellipsometry; Grain Size; Silicon Polymers; Microstructure; Mathematical Models 20050170523 International Business Machines Corp., Essex Junction, VT, USA Beyond Cost-of-Ownership: A Causal Methodology for Costing Wafer Processing Miraglia, Stephanie; Miller, Peter; Richardson, Thomas; Blunt, Gregory; Blouin, Cathy; 1998 IEEE/SEMI Advanced Semiconductor Manufacturing Conference And Workshop; [1998], pp 289-293; In English; See also 20050170458; Copyright; Avail: Other Sources Classical cost-of-ownership data provides detailed cost data of equipment assets but does not provide wafer processing costs Starting with a cost-of-ownership model, a wafer processing cost model was developed and validated This cost-of-processing model provides wafer processing cost data from raw wafer through final passivation and parametric testing This new model goes beyond classical cost-of-ownership data and captures more than just equipment costs process, product, and fabricator costs are also captured These costs are then causally spread to wafers via various algorithmic methodologies In order to do this, some historical cost problems had to be addressed, such as how to properly weight equipment usage and account for dedicated equipment requirements, deal with measurement sampling, incorporate idle time and contingency, and account for different photolithographic field sizes Output from the model was fully validated against actual spending and tied to accounting data in order to assure a full dollar capture The model is currently being used for product costing, decisionmaking, and cost reduction activities at the IBM Microelectronics Division Manufacturing Facility in Essex Junction, Vermont Author Cost Reduction; Cost Analysis; Data Processing Equipment; Wafers; Technology Assessment 20050170524 Tefen Ltd., Foster City, CA, USA Simulation of Test Wafer Consumption in a Semiconductor Facility Foster, Bryce; Meyersdorf, Doron; Padillo, Jose M.; Brenner, Rafi; 1998 IEEE/SEMI Advanced Semiconductor Manufacturing Conference And Workshop; [1998], pp 298-302; In English; See also 20050170458; Copyright; Avail: Other Sources A discrete event simulation methodology was developed to assist in managing test wafer usage in semiconductor fabs 300 The purpose of modeling test wafer usage is to predict the number of new test wafers required, test wafer WIP levels, and how to downgrade test wafers to reduce costs of purchasing new test wafers The test wafer simulation methodology is a detailed yet accurate way to predict test wafer consumption The methodology has been implemented in a 200mm development facility resulting in considerable cost savings by reducing the overall WIP levels of test wafers Author Technology Assessment; Wafers; Performance Tests; Models 20050170525 UniSil Corp., Santa Clara, CA, USA Improvement of Silicon Wafer Minority Carrier Lifetime Through The Implementation of a Pre-Thermal Donor Anneal Cleaning Process Martines, Larry; Wang, Charley; Hardenburger, Tom; Barker, Nancie; Shomers, Brian; 1998 IEEE/SEMI Advanced Semiconductor Manufacturing Conference And Workshop; [1998], pp 303-307; In English; See also 20050170458; Copyright; Avail: Other Sources In recent years, to meet the device maker’s continuously smaller device geometry, the requirement of silicon wafer quality has become more and more stringent Now the silicon wafer minority carrier lifetime, or diffusion length has become one routinely required parameter It is well known that, in addition to the crystal growth, metal contamination is one of the major limiting factors for the minority carrier lifetime in silicon wafers It is very critical to optimize the silicon wafer manufacturing process flow to minimize metal contamination sources during the silicon wafer processing Author Silicon; Wafers; Carrier Lifetime; Minority Carriers; Cleaning 20050170526 International Business Machines Corp., Essex Junction, VT, USA Design for Manufacturability: A Key to Semiconductor Manufacturing Excellence Wilcox, R.; Forhan, T.; Starkey, G.; Turner, D.; 1998 IEEE/SEMI Advanced Semiconductor Manufacturing Conference And Workshop; [1998], pp 308-313; In English; See also 20050170458; Copyright; Avail: Other Sources This paper reviews measures of manufacturing excellence and presents a design-for-manufacturability (DFM) program organized around early design and manufacturing teamwork and the economic analysis of design options Typical measures of manufacturing excellence for a semiconductor fabricator are expressed in terms of either operational or economic results Those expressed in terms of operational results are independent of the product mix in the fabricator while those expressed in terms of economic results integrate both fabricator and product design attributes into a single parameter like revenue/wafer Improvements in the operational measures of manufacturing excellence focus upon increases in capacity and throughput, defect density reductions, and cost containment Improvements in the economic measures of manufacturing excellence must focus on both fabricator processing efficiency and the productivity of the design Design-for-manufacturability practices can improve design productivity, time-to-market, and product performance and reliability by closely coupling semiconductor fabrication knowledge with product requirements during the initial phase of a product design Every design decision produces both technical and economic consequences; understanding these consequences and using this knowledge in the design process to optimize product productivity and profitability is key to achieving manufacturing excellence for that product Author Semiconductors (Materials); Manufacturing; Design Analysis; Economic Analysis 20050170527 Siemens, France Highly Selective Oxide to Nitride Etch Processes on BPSG/Nitride/Oxide Structures in a MERIE Etcher Graf, W.; Basso, C.; Gautier, F.; Martin, J M.; Sabouret, E.; Skinner, G.; 1998 IEEE/SEMI Advanced Semiconductor Manufacturing Conference And Workshop; [1998], pp 314-319; In English; See also 20050170458; Copyright; Avail: Other Sources This study is on oxide etch selective to nitride using a C4F8/CO/Ar/O2 chemistry in a RIE chamber It has been tested in a manufacturing environment on several applications for 16 and 64 megabit DRAM chips Film stacks tested included a BPSG/nitride Self-Aligned Contact type of application and a BPSG/nitride/oxide application Aspect ratios ranged from 4:1 to 8:1 Critical dimensions were typically 0.4 microns and 0.3 microns, but for one application, oxide etch had to finally occur in a 0.09 microns wide space Process development started with a Design of Experiment on patterned wafers in order to understand the major trends of the chemistry The wafers were analysed using a SEM Fine tuning of processes for each 301 application involved Optical Emission Spectroscopy (OES) and electrical test yield analysis Author Oxides; Nitrides; Etching; Wafers; Manufacturing; Chips 20050173487 South Carolina Univ., Columbia, SC USA WBGS Epitaxial Materials Development and Scale Up for RF/Microwave-Millimeter Wave Devices Khan, M A.; Simin, G.; Shur, M.; Gaska, R.; May 2005; 9 pp.; In English; Original contains color illustrations Contract(s)/Grant(s): DAAD19-02-1-0236 Report No.(s): AD-A432964; 15530FA16; No Copyright; Avail: Defense Technical Information Center (DTIC) The project aimed at significant improvement of the III-nitride based epitaxial materials and device design and fabrication for high-power heterostructure field-effect transistors (HFETs) The key innovative approaches implemented in this program include novel pulsed atomic layer epitaxy (PALE) technique to grow the buffer layer with low defect density, improved epitaxial uniformity in multi-wafer MOCVD reactor, growing HFET wafers with the sheet resistance below 300 Ohm/square Design improvements include double-heterostructure devices (DHFET) with InGaN electron confinement layer, insulated gate design using SiO2 gate insulator (MOSDHFETs) and innovative field-plate design These new devices demonstrated high RF powers 15-20 W/mm at a drain bias of 50-65 V, and good parameter stability at 19 W/mm CW powers as confirmed by 100+ hours testing DTIC Aluminum Gallium Arsenides; Epitaxy; Microwave Equipment; Millimeter Waves; Radio Frequencies; Semiconductors (Materials) 77 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS Includes quantum mechanics; theoretical physics; and statistical mechanics For related information see also 72 Atomic and Molecular Physics, 73 Nuclear Physics, and 25 Inorganic, Organic and Physical Chemistry 20050169773 Brookhaven National Lab., Upton, NY RHIC Data Correlation Methodology Michnoff, R.; D’Ottavio, T.; Hoff, L.; MacKay, W.; Satogata, T.; 1999; 10 pp.; In English Report No.(s): DE2004-770722; BNL-66031; No Copyright; Avail: Department of Energy Information Bridge A requirement for RHIC data plotting software and physics analysis is the correlation of data from all accelerator data gathering systems Data correlation provides the capability for a user to request a plot of multiple data channels vs time, and to make meaningful time-correlated data comparisons The task of data correlation for RHIC requires careful consideration because data acquisition triggers are generated from various asynchronous sources including events from the RHIC Event Link, events from the two Beam Sync Links, and other unrelated clocks In order to correlate data from asynchronous acquisition systems a common time reference is required The RHIC data correlation methodology will allow all RHIC data to be converted to a common wall clock time, while still preserving native acquisition trigger information A data correlation task force team, composed of the authors of this paper, has been formed to develop data correlation design details and provide guidelines for software developers The overall data correlation methodology will be presented in this paper NTIS Data Acquisition; Particle Accelerators; Data Correlation 20050169775 Brookhaven National Lab., Upton, NY, USA Littlest Higgs Model and One-Loop Electroweak Precision Constraints Chen, M.; Dawson, S.; 2004; 10 pp.; In English Report No.(s): DE2004-15009978; BNL-873293-2004-CP; No Copyright; Avail: Department of Energy Information Bridge We present in this talk the one-loop electroweak precision constraints in the Littlest Higgs model, including the logarithmically enhanced contributions from both fermion and scalar loops We find the one-loop contributions are comparable to the tree level corrections in some regions of parameter space A low cutoff scale is allowed for a non-zero triplet VEV Constraints on various other parameters in the model are also discussed The role of triplet scalars in constructing a consistent renormalization scheme is emphasized NTIS Fermions; Scalars; Electroweak Model 302 20050169843 Brookhaven National Lab., Upton, NY, USA Singlet Free Energies of a Static Quark-Antiquark Pair Petrov, K.; 2004; 12 pp.; In English Report No.(s): DE2004-15009925; BNL-73191-2004-CP; No Copyright; Avail: Department of Energy Information Bridge We study the singlet part of the free energy of a static quark anti-quark (Q(bar Q)) pair at finite temperature The model is three flavor QCD with degenerate quark masses using N(sub (tau)) = 4 and 6 lattices with Asqtad staggered fermion action We look at thermodynamics of the system around phase transition and study its scaling with lattice spacing and quark masses NTIS Free Energy; Quarks; Thermodynamics; Antiparticles 20050171013 Jefferson (Thomas) Lab Computer Center, Newport News, VA, USA Nucleon Electromagnetic Form Factors de Jager, K.; 2004; 34 pp.; In English Report No.(s): DE2004-834525; No Copyright; Avail: Department of Energy Information Bridge Although nucleons account for nearly all the visible mass in the universe, they have a complicated structure that is still incompletely understood The first indication that nucleons have an internal structure, was the measurement of the proton magnetic moment by Frisch and Stern (1933) which revealed a large deviation from the value expected for a point-like Dirac particle The investigation of the spatial structure of the nucleon, resulting in the first quantitative measurement of the proton charge radius, was initiated by the HEPL (Stanford) experiments in the 1950s, for which Hofstadter was awarded the 1961 Nobel prize The first indication of a non-zero neutron charge distribution was obtained by scattering thermal neutrons off atomic electrons The recent revival of its experimental study through the operational implementation of novel instrumentation has instigated a strong theoretical interest Nucleon electro-magnetic form factors (EMFFs) are optimally studied through the exchange of a virtual photon, in elastic electron-nucleon scattering NTIS Nucleons; Form Factors; Neutrons; Protons 20050173407 Oxford Univ., Oxford, UK An Investigation of Certain Thermodynamic Losses in Minature Cryocoolers Reed, Jaime; Jan 2005; 30 pp.; In English; Original contains color illustrations Contract(s)/Grant(s): FA8655-04-1-3011 Report No.(s): AD-A432813; EOARD-SPC-04-3011; No Copyright; Avail: Defense Technical Information Center (DTIC) Stirling cycle cryocoolers developed at Oxford have typically been designed using a second order methods whereby the ideal Stirling efficiency is degraded by a number of discrete loss mechanisms In all cases the eventual machines perform less well than expected, and it always appears as if an additional thermodynamic loss is acting This empirically calibrated loss is therefore included as part of the normal design procedure and there is anecdotal evidence that this is an approach taken by other manufactures Although this loss might be caused by imperfect heat transfer, existing theories do not agree with its magnitude A project was therefore started to measure the losses in the simplest possible geometry, a linear compressor with a plain ‘top-hat’ cylinder head It was hoped that by characterizing the losses in this geometry and applying them to full machines these called ‘compression loss’ could be explained Since the loss is quite large it could allow significant improvements to be made for future machines A well calibrated measurement system was developed and a linear compressor commissioned To enable a sufficiently good energy balance to be produced electromagnetic motor losses and windage were measured It immediately became clear that these were more significant than had been assumed previous studies In fact it appeared as if a significant proportion of the ‘compression loss’ might be explained by these new measurements With the losses expected from analytic analyses Agreement was not perfect, however, and this is thought to be due to the incompleteness of the heat transfer theory, particularly with regard to the flow through the clearance seal Future possibilities for work are suggested and it is hoped that these measurements can be used as a baseline for testing theoretical work which will enable efficiencies to be increased not just in Stirling type coolers, but also in pulse tubes and linear alternators DTIC Coolers; Cryogenic Cooling; Thermodynamics 303 anorthositic regolith breccia with minor mare basalt component Additional information is included in the original extended abstract Author Lunar Rocks; Meteorites; Anorthosite; Petrology 20050169949 Pennsylvania State Univ., University Park, PA, USA Basalt Weathering Rates in a Mars Analog Environment: Clues to the Duration of Water on Mars? Hausrath, E M.; Brantley, S L.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color and black and white illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document Extensive evidence, most recently from the Mars Exploration Rovers, documents that liquid water once existed on the surface of Mars However, significant uncertainty still exists as to the duration of liquid water on the surface of Mars Mineral dissolution rates may provide information on maximum durations of water on Mars However, field and laboratory weathering rates on earth differ significantly, by up to 5 orders of magnitude Few field weathering rates for basalt and olivine have been published The climate history of Mars is not well-constrained; however, field weathering rates of minerals in Mars-analog environments may provide information on the duration of water on Mars Spitsbergen (Norway) provides three examples of basalts weathering in a Mars-analog environment: outcrops of the Quaternary volcano, Sverrefjell, plateau basalt lavas emplaced approximately 10 million years ago, and a basalt dike Sverrefjell has been well documented as a Mars analog containing carbonate globules that are very similar to those found in ALH84001 These three basalts with different chemistries will allow us to study basalt weathering in a cold, dry climate Basalt samples were collected from each of the three locations as part of AMASE, the Arctic Mars Analog Svalbard Expedition in August of 2004 They were then observed by optical microscopy, backscattered electron microscopy, and energy dispersive x-ray spectroscopy Derived from text Basalt; Mars Surface; Water; Weathering; Analogs; Mars Environment 20050169950 Geological Survey of Canada, Ottawa, Ontario, Canada On the Need for an Atlas of Chondrule Textures Herd, R K.; Hunt, P A.; Venance, K E.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 1 pp.; In English; See also 20050169945; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document There is a need for an atlas of chondritic meteorites to serve as a reference for research A recent publication o n zircon textures in terrestrial rocks provides a useful analogy: The paper presents a selection of both the most typical, but also of the less common, features seen in zircon, categorized according to the different geological processes responsible for their formation A similar reference on the features seen in chondrules, perhaps categorized by the different extraterrestrial processes (thought to be) responsible for their formation, is necessary We propose a community effort among those researchers interested in sharing such information The advent of digital imaging techniques means that digital photomicrographs and scanning-electron microscope images derived from systematic textural studies can be readily shared and discussed We are proposing to do this through a dedicated web site and list Derived from text Chondrule; Meteoritic Composition; Textures; Petrology 20050169952 Massachusetts Univ., Amherst, MA, USA Morphometry of Large Martian Impact Craters Howenstine, Jared B.; Kiefer, Walter S.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document The topography of impact craters and basins contains important information about both the initial formation and the subsequent modification of the structure Previous studies of the morphometry of martian impact structures using MOLA topography data examined craters smaller than 110 km in diameter In this study, we emphasize larger craters in order to build a database that will support subsequent gravity modeling of large martian craters Derived from text Mars Craters; Mars Surface; Topography; Hypervelocity Impact 339 20050169954 University Coll., London, UK Basalts in Mare Serenitatis, Lacus Somniorum, Lacus Mortis and Part of Mare Tranquillitatis Hackwill, Terence; Guest, John; Spudis, Paul; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document We have identified a number of discreet basaltic units in the area being studied An assessment of their ages, their extent, trends in their chemistry and an indication of the volume of basalt within the basin may provide new information about the geological history of the area A number of previous studies have tried to determine the existence and boundaries of basaltic units within the area we examined We have used the higher resolution Clementine ultraviolet/visible data (down to 200m/pixel) to try and determine the boundaries of units within the region Additionally we have used Clementine FeO and TiO2 wt% data to see if they can suggest variations in the thickness of basalts in the region We have also used crater depths to suggest the volume of basalt within Mare Serenitatis Additional information is included in the original extended abstract Author (revised) Lunar Maria; Basalt; Lunar Composition; Ultraviolet Astronomy 20050169955 Washington Univ., Saint Louis, MO, USA Tectonic Pressurization of Aquifers in the Formation of Mangala and Athabasca Valles on Mars Hanna, J C.; Phillips, R J.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document A distinct class of martian outflow channels, including Mangala and Athabasca Valles, originate within extensional tectonic features Here we demonstrate that the stress change in the crust associated with the tectonism would result in a significant near-instantaneous pressurization of the aquifer contained therein, if such an aquifer existed at the time, resulting in the floods that carved the observed channels Additional information is included in the original extended abstract Author (revised) Mars Surface; Tectonics; Valleys; Aquifers; Hydrogeology 20050169956 Brown Univ., Providence, RI, USA Accessory Phases in Argentine Impact Breccias: Implications for Shock History, Emplacement Dynamics, Vapor Composition and Target Lithologies Harris, R S.; Schultz, P H.; Bunch, T.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color and black and white illustrations Contract(s)/Grant(s): NSF EAR-00-01047; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document Vesicular glasses preserved in the thick loess-like sediments of the Argentine Pampas are interpreted to represent as many as seven different impacts since the late Miocene With the exception of those formed during the most recent Rio Cuarto event (2-6 ka), unequivocal shock indicators (e.g., planar deformation features) in these glasses have not been reported Instead their ages, extents, abundances, and geologic settings together with excellent petrographic evidence of extremely high transient temperatures (e.g., baddeleyite and lechatelierite) and rapid quenching support an impact origin Typical shock indicators in quartz and feldspars might be exceedingly rare in pampean glasses due to the highlyporous nature of the presumed target materials Loessoid targets should facilitate both poor shock coupling and high post-shock temperatures; consequently, many of the few grains that do develop shock signatures may be thermally altered or melted thereafter Therefore, we have endeavored to identify shock indicators in minerals less susceptible to the complications of impedance or digestion Ilmenite provides a good candidate because it is common in loessoid sediments, has a very high melting temperature, and is sensitive to shock pressures less than 10 GPa Initial results are presented here Derived from text Breccia; Lithology; Shock Waves; Petrography; Vapors; Composition (Property); Argentina 20050169957 Indiana Univ., Bloomington, IN, USA The Hydration and Dehydration of Hydrous Ferric Iron Sulfates Hasenmueller, E A.; Bish, D L.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document 340 Data collected by Viking, Pathfinder, and the Mars Exploration Rovers and by orbiters (e.g., Odyssey) provide multiple lines of evidence for the historical and present-day existence of water on Mars For example, Mars Odyssey detected up to approx.10 wt% equivalent H2O in equatorial regions of Mars where water ice is not stable [1] It has been theorized that sulfate minerals, including hydrated ferric sulfates, may be part of the inventory of hydrous phases that account for water on the martian surface [2, 3, 4] Several Fe-bearing minerals, such as jarosite and goethite, as well as Mg and Ca sulfates have already been identified in the martian regolith [5, 6, 7] Knowledge of the martian regolith mineralogy is essential to understanding Mars hydro-geologic history, and hydrous minerals may serve as useful records of past aqueous alteration events Indeed, important inferences about past conditions have been made from the presence of jarosite and goethite [5, 6], and it has been determined that jarosite is thermodynamically stable under assumed martian surface conditions [8] Laboratory data measured under simulated martian surface conditions are crucial to provide constraints on hydrous mineral stability [9], and guided by current martian soil chemistry data we selected hydrated ferric sulfates for study (in lieu of ferrous sulfate minerals) Derived from text Sulfates; Iron Oxides; Hydration; Dehydration; Mars Exploration; Water; Surface Properties 20050169958 Deutsche Forschungsanstalt fuer Luft- und Raumfahrt, Berlin, Germany Interior Layered Deposits in Valles Marineris, Mars: Insights from 3D-Data Obtained by the High Resolution Stereo Camera (HRSC) Hauber, E.; Gwinner, R.; Stesky, R.; Fueten, F.; Michael, G.; Reiss, D.; Zegers, T.; Hoffmann, H.; Jaumann, R.; vanGaaelt, S., et al.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color and black and white illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document The Interior Layered Deposits (ILD) in the Valles Marineris depressions on Mars may be of volcanic or sedimentary origin Either way, their presence has profound implications for the formation of the Valles Marineris itself: A volcanic origin might support a formation of the Valles Marineris as a tectonic (rift-like) feature, while a sedimentary origin might support a formation by collapse processes The High Resolution Stereo Camera (HRSC) on board the Mars Express mission obtains high-resolution stereo and multispectral images, which are particularly well suited for the geomorphologic analysis of the ILD Derived from text High Resolution; Mars Surface; Tectonics; Mineral Deposits; Mars Volcanoes; Stereophotography; Three Dimensional Models 20050169961 Brown Univ., Providence, RI, USA Evidence for Snow and Ice Accumulation Aiding Debris Flow and Glacial Flow at Mid- to Low-Latitudes on Mars Hiesinger, H.; Head, J W.; Neukum, G.; Jaumann, R.; Hauber, E.; Carr, M.; Masson, P.; Foing, B.; Hoffmann, H.; Kreslavsky, M., et al.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color and black and white illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document Mars Express HRSC (High-Resolution Stereo Camera) image data of eastern Hellas reveal details of debris aprons at the base of massifs characterized by numerous concentrically ridged lobate and pitted features suggesting extremely ice-rich glacier-like viscous flow and sublimation This, together with new evidence for recent ice-rich debris-covered glaciers at the base of the Olympus Mons scarp suggests geologically recent and recurring glacial activity in low- and mid-latitude regions of Mars Additional information is included in the original extended abstract Author (revised) Mars Environment; Planetary Geology; Glacial Drift; Glaciers 20050169962 Melbourne Univ., Parkville, Australia Origin of the Northern Lowlands of Mars in a Single String-of-Pearls Impact Hoffman, ick; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document It has long been recognized that the Northern Lowlands of Mars were formed very early in the history of the observed planetary surface and may well be the earliest geologic event that is still visible today Models of the formation process have included early asymmetric convection, whether in a magma ocean or by slower plate-style tectonics Alternatively, one or 341 more giant basin-forming impacts may have formed the crustal dichotomy by excavation of originally uniform crust To date, it has been deemed improbable that an impact origin can explain the detailed shape of the crustal dichotomy, since it is far from circular and would require multiple impacts to generate the detailed shape of the boundary Statistically, random impacts are highly unlikely to have only struck one hemisphere of Mars One impact model has not received attention to date, yet holds the key to simultaneous explaining the coincidental location of multiple impacts A ‘String-of-Pearls’ impactor, similar to comet Shoemaker-Levy 9, impacting about 40 degrees from the spin axis of Paleo-Mars would carve a series of overlapping impact basins, distributed around a small circle These overlapping impact basins would define a composite basin with a scalloped and irregular margin, essentially identical to the observed crustal dichotomy on Mars Additional information is included in the original extended abstract Author (revised) Mars Surface; Northern Hemisphere; Mars Craters; Structural Basins; Meteorite Collisions 20050169963 Colorado Univ., Boulder, CO, USA Comparison of Newly Acquired Lunar Spectra with the Titanium Abundance Maps Derived from Clementine Holsclaw, G M.; McClintock, W E.; Robinson, M S.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document The Mercury Atmospheric and Surface Composition Spectrometer (MASCS) is one of seven science instruments onboard NASA’s MESSENGER mission, currently en-route to the planet Mercury One of MASCS s components, referred to as the Visible and Near Infrared Spectrograph (VIRS), will record reflectance spectra of the surface in order to characterize the mineralogy of the planet [1] The lunar highlands and the average mercurian crust are proposed to be compositionally similar [i.e 2] In preparation to interpret VIRS reflectance spectra of Mercury to be first obtained in 2008, the Moon has been observed with an engineering model of the VIRS from a ground-based telescope In this study, the ultraviolet and visible region of the spectrum is compared with titanium content in the lunar regolith Derived from text Visible Spectrum; Lunar Rocks; Planetary Surfaces; Near Infrared Radiation; Titanium; Surface Layers; Atmospheric Composition; Highlands; Crusts 20050169964 Boeing Co., Seattle, WA, USA Nudging an Asteroid with Explosives or Impacts Housen, K R.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document Explosives or direct kinetic energy mechanisms are often cited in discussions of altering asteroid orbits This is usually applied to the deflection of potentially hazardous objects, but also has applications for asteroid science While detailed reviews of various mechanisms have been given, the purpose of this brief report is to estimate the velocity change that can be imparted to an asteroid via a near surface explosion These results also apply to impacts, given the well-known equivalence between impacts and shallow explosions Derived from text Asteroids; Kinetic Energy; Fragmentation; Impact Velocity 20050169965 Academia Sinica, Nanjing, China Fremdlinge in Chondrules and Matrix of the Ningqiang Carbonaceous Chondrite Hua, Xin; Wang, Ying; Hsu, Wei-Biao; Sharp, T G.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains black and white illustrations Contract(s)/Grant(s): NSFC-40325009; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document We report here the petrographic and mineralogical studies of Fremdlinge in chondrules and matrix of the Ningqiang carbonaceous chondrite Fremdlinge, or so-called opaque assemblages, were previously found in Ca-Al-rich inclusions (CAIs) of CV chondrites The mineralogy of Fremdlinge is very complex, containing phases apparently formed at high and low temperatures and under highly reducing and oxidizing conditions Identified phases include Fe, Ni metals, sulfides, Fe-oxides, phosphates, silicates and Pt-metal grains Fremdlinge were thought to be exotic objects incorporated into the host CAIs and thus represented the oldest solids in the solar system However, because of their complex mineral assemblages, their origin 342 is not as readily explained Other authors have argued for a local origin of these objects Ningqiang is an anomalous carbonaceous chondrite with many similarities close to CV3 meteorites In this work, numerous relatively large Fremdlinge are observed in chondrules as well as in matrix of Ningqiang We carried out a petrographic study of these objects in order to gain additional insights into their formation Derived from text Carbonaceous Chondrites; Chondrule; Meteoritic Composition; Petrography; Mineralogy 20050169966 Brown Univ., Providence, RI, USA Regional Mid-Latitude Glaciation on Mars: Evidence for Marginal Glacial Deposits Adjacent to Lineated Valley Fill Head, J W.; Marchant, D R.; Fastook, J L.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains black and white illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document Recent analysis of the orbital parameters of Mars [1] leads to the conclusion that chaotic diffusion prevails; analytical assessment of the density function of different orbital parameters leads to the prediction that the mean obliquity over geological time is approx.38deg, and that the probability is 63% that it exceeded 60deg in the past Ga Thus, Mars is currently in a period of anomalously low obliquity (approx.23deg), and typical obliquity values in the history of Mars (and thus climate zones and the distribution of surface and near-surface water ice [2]) are likely to be much different than now Indeed, synthesis of recent observational data suggest that Mars underwent an ice age in the last few million years from which it is currently emerging, during which time obliquity exceeded 30deg and polar ice was mobilized and transported equatorward and deposited down to latitudes of approx.30deg in both hemispheres [3] What happens when obliquity exceeds 30deg for extended periods of time? Where is water deposited, in what volumes, and how is it manifested in terms of geological processes? Geological evidence suggests that extensive water ice was deposited at mid-latitudes in the past associated with lineated valley fill and lobate debris aprons [4,5] and the case has been presented for extensive past tropical mountain glaciation [6,7] Recent general circulation model analyses provide evidence for significant mobilization of polar ice during periods of high obliquity and redeposition equatorward in the form of low to mid-latitude ice deposits [8-11] Derived from text Mars Surface; Glaciers; Geology; Deposits; Valleys 20050169967 NASA Ames Research Center, Moffett Field, CA, USA The Planetesimal Bow Shock Model for Chondrule Formation: More Detailed Simulations in the Near Vicinity of the Planetesimal Hood, Lon L.; Ciesla, Fred J.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains black and white illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document Gas dynamic shock waves in a low temperature nebula have been considered to be a leading candidate mechanism for providing the repetitive, short-duration heating events that are believed to have been responsible for the formation of chondrules in chondrites It has been found, for example, that shocks with Mach numbers greater than 4 or 5 would be capable of rapidly melting 0.1-1 mm sized silicate particles as required by meteoritic data Near the nebula midplane where chondrite parent bodies are believed to have formed, possible energy sources for generating multiple shocks include mass concentrations in a gravitationally unstable nebula, tidal interactions of proto-Jupiter with the nebula, and bow waves upstream of planetesimals scattered gravitationally into eccentric orbits by proto- Jupiter In a recent study, we have found that chondrule precursors that are melted following passage through a planetesimal bow shock would likely cool at rates that are too rapid to be consistent with meteoritic evidence However, that study was limited to the bowshock exterior to about 1.5 planetesimal radii (measured perpendicular to the symmetry axis) to avoid complications interior to this distance where large pressure gradients and lateral flow occur as the gas flows around the planetesimal In this paper, we reconsider the planetesimal bow shock model and report more detailed numerical simulations of chondrule precursor heating, cooling, and dynamical histories in the near vicinity of a representative planetesimal Author Chondrule; Formation; Shock Waves; Models; Gas Flow; Gas Dynamics 20050169969 Geological Museum, Copenhagen, Denmark Why Small is Beautiful - and How to Detect Another 10 Billion Small Main Belt Asteroids Haack, Henning; Bidstrup, Philip R.; Michelsen, Rene; Andersen, Anja C.; Jorgensen, John Leif; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document 343 Estimates of the size distribution of main belt asteroids suggest that there is a population of approximately 10 billion objects in the meter to km range These objects have, so far, escaped detection Current Earth-based telescopes have, except for a few objects, not been able to detect the faint and distant sub-kilometer asteroids in the main belt Long integration times cannot be used unless the object can be tracked - which is not possible for an unknown object Small asteroids can be observed closeup from a spacecraft but, so far, missions to the asteroid belt have not had the ability to automatically detect previously unknown asteroids Since small asteroids can only be observed from the spacecraft for a very limited time it is not possible to operate the spacecraft from the distant Earth - a fully autonomous mission is required We have explored the possibilities to build such a fully autonomous spacecraft using existing technology and have named the mission proposal Bering Small asteroids are of great interest for a number of reasons: 1) Small low-gravity asteroids probably have less regolith cover thus providing a clearer picture of their interior structure and type; 2) Due to the Yarkovsky effect small asteroids have shorter lifetimes and therefore probably younger, less space weathered surfaces; 3) Small asteroids bridge the gap between the known big asteroids and the NEAs, meteoroids and meteorites; 4) Mapping the orbital parameters of small object may allow us to associate streams of small fragments with their parent asteroids thus further constraining the link between meteorites and asteroids and provide constraints on the transfer mechanics of material from the main belt to the inner Solar System; 5) Due to their shorter lifetime smallest asteroids may be used to constrain the most recent collisional evolution of the asteroid belt; 6) Measuring the actual size distribution of asteroids in the main belt can be used to constrain models of the collisional evolution of main belt asteroids Additional information is included in the original extended abstract Author (revised) Asteroid Belts; Asteroid Detection; Space Probes 20050169970 Southwest Research Inst., Boulder, CO, USA Tharsis Recharge and the Martian Outflow Channels: Observations and Recent Modeling Harrison, K H.; Grimm, R E.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document The history of the martian hydrological cycle cannot be fully understood without a comprehensive model for the large Hesperian outflow channels (OCs) that debouch into Chryse Planitia Their morphology indicates erosion by groundwater discharged to the surface through disruptions in a cryosphere What remains to be established, however, is a suitable mechanism for supplying the OC s with the required volume of groundwater (about 10(exp 6) cubic kilometers), greater than can be stored in the regional aquifer We suggest that low-latitude Hesperian ice-sheets recharged the Tharsis aquifer, providing sufficient groundwater for outflow channel formation The ice sheets developed during periods of high planetary obliquity when net deposition of volatiles occurred at low latitudes Regionally elevated crustal heat due to Tharsis magmatic processes allowed the ice sheets to melt at their bases, producing aquifer infiltration We present advances in previous numerical models of outflow channel discharge that compare Tharsis recharge with South Polar recharge We also present observational evidence supporting low-latitude paleo-ice sheets Derived from text Hydrological Cycle; Mars Surface; Mathematical Models; Channel Flow 20050169971 Planetary Science Inst., Tucson, AZ, USA Adventures (Arrrggghh!) in Crater Counting: Small Crater Controversies Hartmann, W K.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document This invited presentation reviews basic elements of Martian crater counting as a technique for estimating Martian surface ages Further historical review and response to recent critiques are given Mars Global Surveyor s Mars Orbital Camera (MGS/MOC), for the first time, allowed crater counts down to diameters (D) of approximately 10 m, extending the effective D range of Martian crater statistics by an order of magnitude or more (The major previous review paper, in 1992, cited Martian crater statistics only down to D = a few km.) The new data offer tremendous opportunities and at the same time significant problems in terms of dating Martian stratigraphic units Derived from text Mars Craters; Mars Surface; Geochronology 344 20050169972 Case Western Reserve Univ., Cleveland, OH, USA Syrtis Major as the Source Region of the Nakhlite/Chassigny Group of Martian Meteorites: Implications for the Geological History of Mars Harvey, R P.; Hamilton, V E.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color and black and white illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document A major challenge facing ongoing studies of Mars is that the lack of datable surface samples leaves accepted crater counting-based chronologies proposed for Mars merely relative Although the mechanism of Martian meteorite delivery destroys their original geographical context, it is theoretically possible for these samples to provide the missing context through matching the unique physical, geochemical and spectral properties of meteorites with potential parent volcanic units on Mars An obvious additional requirement is that such regions must contain at least one crater whose size and apparent age provides a plausible mechanism for transfer of material to Earth Derived from text Mars Volcanoes; Planetary Geology; Geochronology; Mars Surface; SNC Meteorites 20050169973 Los Alamos National Lab., NM, USA Revised Thorium Abundances for Lunar Red Spots Hagerty, J J.; Lawrence, D J.; Elphic, R C.; Feldman, W C.; Vaniman, D T.; Hawke, B R.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color illustrations Contract(s)/Grant(s): W-7405-eng-36; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document Lunar red spots are features on the nearside of the Moon that are characterized by high albedo and by a strong absorption in the ultraviolet These red spots include the Gruithuisen domes, the Mairan domes, Hansteen Alpha, the southern portion of Montes Riphaeus, Darney Chi and Tau, Helmet, and an area near the Lassell crater It has been suggested that many of the red spots are extrusive, nonmare, volcanic features that could be composed of an evolved lithlogy enriched in thorium In fact, Hawke et al used morphological characteristics to show that Hansteen Alpha is a nonmare volcanic construct However, because the apparent Th abundances (6 - 7 ppm) were lower than that expected for evolved rock types, Hawke et al concluded that Hansteen Alpha was composed of an unknown rock type Subsequent studies by Lawrence et al used improved knowledge of the Th spatial distribution for small area features on the lunar surface to revisit the interpretation of Th abundances at the Hansteen Alpha red spot As part of their study, Lawrence et al used a forward modeling technique to show that the Th abundance at Hansteen Alpha is not 6 ppm, but is more likely closer to 25 ppm, a value consistent with evolved lithologies This positive correlation between the morphology and composition of Hansteen Alpha provides support for the presence of evolved lithologies on the lunar surface It is possible, however, that Hansteen Alpha represents an isolated occurrence of non-mare volcanism That is why we have chosen to use the forward modeling technique of Lawrence et al to investigate the Th abundances at other lunar red spots, starting with the Gruithuisen domes Additional information is included in the original extended abstract Author (revised) Lunar Composition; Abundance; Thorium; Domes (Geology); Color; Gamma Ray Astronomy 20050169974 Waseda Univ., Tokyo, Japan Planetary Gamma-Ray Imager Using High Pressure Xenon Time Projection Chamber Hasebe, N.; Yamashita, N.; Kobayashi, M.-N.; Miyachi, T.; Miyajima, M.; Okudaira, O.; Kobayashi, S.; Hosojima, T.; Pushkin, K N.; Tzuka, C., et al.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document Explorations of lunar and planetary surfaces by gamma-ray spectroscopy have been obtaining excellent results in recent missions However, due to the difficulty of gamma-ray collimation, the spatial resolution of gamma-ray spectrometers is not comparable to X-ray, visible, UV, or IR cameras Compton Telescopes cannot uniquely identify the arrival direction of a single incident gamma ray, and are only applicable for point-like sources The spatial resolution of a conventional omnidirectional gamma-ray spectrometer is a function of the altitude In order to survey small to medium sized geological structures, the improvement in spatial resolution of gamma-ray observation is desired By introducing a new method of gamma-ray measurement, gamma-ray imaging camera is considered for planetary science Derived from text Gamma Ray Spectrometers; High Pressure; Imaging Techniques; Planetary Surfaces; Xenon 345 20050169975 State Univ of New York, Stony Brook, NY, USA Integrating Global-Scale Mission Datasets: Understanding the Martian Crust Hahn, B C.; McLennan, S M.; Taylor, G J.; Boynton, W V.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document Constraining the composition of the chemical reservoirs of the Martian crust and mantle is critical to understanding its evolution Over more than a half-decade, a suite of instruments on multiple spacecraft have been mapping the surface of Mars, producing a variety of different global geochemical and geophysical datasets However, individual chemical datasets, while revealing, need to be cross-correlated with other data, such as surface age, topography or crustal thickness, to fully describe the processes that shape the Martian surface and sub-surface over geologic time In this study, we present our first results in attempting to correlate various global datasets We also attempt to constrain the rate of Martian crustal growth and crustal recycling Past studies have estimated the surface crustal recycling regime for Earth using calculations based on a combination of surface age versus area, Nd and Hf isotope compositions of sedimentary rocks and the geochemical evolution of sedimentary rocks The degree of crustal recycling is crucial for determining the long-term evolution of a planetary crust/mantle system Using existing surface geology data, a similar preliminary estimate can be made for the Martian surface Additional information is included in the original extended abstract Author (revised) Planetary Mapping; Planetary Crusts; Mars Surface; Mars (Planet); Data Integration; Planetary Geology 20050169976 Jet Propulsion Lab., California Inst of Tech., Pasadena, CA, USA Comparing Goldstone Solar System Radar Earth-based Observations of Mars with Orbital Datasets Haldemann, A F C.; Larsen, K W.; Jurgens, R F.; Slade, M A.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document The Goldstone Solar System Radar (GSSR) has collected a self-consistent set of delay-Doppler near-nadir radar echo data from Mars since 1988 Prior to the Mars Global Surveyor (MGS) Mars Orbiter Laser Altimeter (MOLA) global topography for Mars, these radar data provided local elevation information, along with radar scattering information with global coverage Two kinds of GSSR Mars delay-Doppler data exist: low 5 km x 150 km resolution and, more recently, high (5 to 10 km) spatial resolution Radar data, and non-imaging delay-Doppler data in particular, requires significant data processing to extract elevation, reflectivity and roughness of the reflecting surface Interpretation of these parameters, while limited by the complexities of electromagnetic scattering, provide information directly relevant to geophysical and geomorphic analyses of Mars In this presentation we want to demonstrate how to compare GSSR delay-Doppler data to other Mars datasets, including some idiosyncracies of the radar data Additional information is included in the original extended abstract Author (revised) Radar Astronomy; Mars (Planet); Radar Data; Data Processing; Doppler Radar 20050169977 Jet Propulsion Lab., California Inst of Tech., Pasadena, CA, USA Water Ice Clouds in the Martian Atmosphere: A View from MGS TES Hale, A S.; Tamppari, L K.; Christensen, P R.; Smith, M D.; Bass, Deborah; Qu, Zheng; Pearl, J C.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document We use the method of Tamppari et al to map water ice clouds in the Martian atmosphere This technique was originally developed to analyze the broadband Viking IRTM channels and we have now applied it to the TES data To do this, the TES spectra are convolved to the IRTM bandshapes and spatial resolutions, enabling use of the same processing techniques as were used in Tamppari et al This retrieval technique relies on using the temperature difference recorded in the 20 micron and 11 micron IRTM bands (or IRTM convolved TES bands) to map cold water ice clouds above the warmer Martian surface Careful removal of surface contributions to the observed radiance is therefore necessary, and we have used both older Viking-derived basemaps of the surface emissivity and albedo, and new MGS derived basemaps in order the explore any possible differences on cloud retrieval due to differences in surface contribution removal These results will be presented in our poster Our previous work has concentrated primarily on comparing MGS TES to Viking data; that work saw that large-scale cloud features, such as the aphelion cloud belt, are quite repeatable from year to year, though small scale behavior shows some variation Comparison of Viking and MGS era cloud maps will be presented in our poster In the current stage of our study, we have concentrated our efforts on close analysis of water ice cloud behavior in the northern summer of the three MGS 346 mapping years on relatively small spatial scales, and present our results below Additional information is included in the original extended abstract Author (revised) Planetary Meteorology; Ice Clouds; Planetary Mapping; Mars Atmosphere; Water; Thermal Emission; Spectroscopy 20050169978 Brown Univ., Providence, RI, USA Evidence for Shocked Feldspars and Ballen Quartz in 450,000 Year Old Argentine Impact Melt Breccias Harris, R S.; Schultz, P H.; Bunch, T.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color and black and white illustrations Contract(s)/Grant(s): NSF EAR-00-01047; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document Vesicular glasses found in the vicinity of Centinela del Mar (CdM), Argentina have been interpreted as products of a bolide impact into thick loessoid sediments approximately 450 ka The age, abundance, and stratigraphic setting of these glasses in addition to petrographic evidence of extremely high temperatures (baddeleyite, lechatelierite) and rapid quenching (beta-cristobalite) support an impact origin However, specific examples of shock-induced transformations previously have not been reported Here we report the identification of diaplectic glass, planar deformation features (PDFs), and other planar lamellae in plagioclase and alkali feldspar grains, entrained in the CdM glasses, that only have been observed in association with hypervelocity collisions and nuclear explosions We also report the presence of ballen quartz grains which have been considered diagnostic of shock formation Derived from text Argentina; Breccia; Feldspars; Impact Melts; Quartz; Petrography 20050169979 Southwest Research Inst., Boulder, CO, USA Evolution of Martian Valley Network Formation: Surface Runoff to Groundwater Discharge Harrison, K P.; Grimm, R E.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains black and white illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document The ubiquitous Martian valley networks have traditionally been used to invoke a warm, wet early climate This simple hypothesis has been complicated with each successive improvement in imaging data Mariner 9 and Viking images revealed the importance of groundwater sapping morphology, typified by abrupt, alcove-like terminations, small numbers of tributaries, and poor interfluve dissection High resolution MGS MOC data revealed a more complex picture of groundwater processes, including evidence of groundwater erosion downstream of head reaches, in addition to typical headward erosion However, MOC images also showed denser networks suggestive of surface runoff Martian valley networks may thus be separated into two broad groups: dense networks influenced by surface runoff and sparse networks influenced predominantly by groundwater processes We propose that the two groups mark a temporal shift in fluvial erosion processes spanning the late Noachian and Hesperian The details of this hypothesis may be described in relation to a warm or cold early climate as follows Derived from text Ground Water; Mars Surface; Valleys; Planetary Evolution; Drainage 20050169980 Deutsche Forschungsanstalt fuer Luft- und Raumfahrt, Berlin, Germany Delta-like Deposits in Xanthe Terra, Mars, as Seen with the High Resolution Stereo Camera (HRSC) Hauber, E.; Gwinner, K.; Reiss, D.; Scholten, F.; Michael, G.; Jaumann, R.; Ori, G G.; Marinangeli, L.; Neukum, G., et al.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color and black and white illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document HRSC images reveal the existence of several fan- or delta-like deposits in the Xanthe Terra region of Mars We report on our investigation of two possible lacustrine deltas at the mouths of Nanedi and Sabrina Valles, respectively Their morphologic characteristics suggest a formation as Gilbert deltas by clastic sedimentation of fluvially transported material in crater lakes Derived from text Mars Photographs; High Resolution; Mars Surface; Mineral Deposits; Mars Volcanoes; Cameras; Deltas 347 20050169981 Minnesota Univ., Duluth, MN, USA Crustal Plateaus as Ancient Large Impact Features: A Hypothesis Hansen, V L.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document Venusian crustal plateau formation is one of the most hotly debated topics to emerge form NASA’s Magellan Mission Crustal plateaus, approx 1500-2500 km diameter quasi-circular topographic plateaus that rise approx 4 to 0.5 km above the surrounding terrain host distinctive deformation fabrics Scientists generally agree that thickened crust supports crustal plateaus, as evidenced by small gravity anomalies, low gravity to topography ratios, shallow apparent depths of compensation, and consistent admittance spectra Debate centers on crust thickening mechanism The downwelling hypothesis involves thickening by subsolidus flow and horizontal lithospheric accretion associated with cold mantle downwelling, whereas the plume hypothesis accommodates thickening via magmatic under-plating and vertical accretion due to interaction of ancient thin lithosphere with a large thermal mantle plume Examination of surface geologic relations within four crustal plateau areas leads to new observations, and refined geologic surface histories presented in a companion abstract The resulting surface history interpreted from each plateau surface is difficult to address within the context of either the downwelling or plume hypothesis of plateau formation In this contribution a third hypothesis for crustal plateau is put forth, plateau formation involving crystallization of a huge lava pond In this contribution the emerge alternate hypothesis of crustal plateau formation is discussed and explored, including possible lava pond formation resulting from massive melting of the mantle as a result of bolide impact with ancient thin Venus lithosphere Impact models have recently also been proposed for other large igneous provinces including Great Ontong Java Plateau on Earth and the Tharis region of Mars Additional information is included in the original extended abstract Author (revised) Planetary Crusts; Plateaus; Planetary Geology; Craters; Venus Surface 20050169982 Minnesota Univ., Duluth, MN, USA New Observations of Crustal Plateau Surface Histories, Venus: Implications for Crustal Plateau Hypotheses Hansen, V L.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document Venusian crustal plateau formation is one of the most hotly debated topics to emerge form NASA’s Magellan Mission Crustal plateaus, approx 1500-2500 km diameter quasi-circular topographic plateaus that rise approx 4 to 0.5 km above the surrounding terrain host distinctive deformation fabrics Scientists generally agree that thickened crust supports crustal plateaus, as evidenced by small gravity anomalies, low gravity to topography ratios, shallow apparent depths of compensation, and consistent admittance spectra Debate centers on crust thickening mechanism The downwelling hypothesis involves thickening by subsolidus flow and horizontal lithospheric accretion associated with cold mantle downwelling, whereas the plume hypothesis accommodates thickening via magmatic under-plating and vertical accretion due to interaction of ancient thin lithosphere with a large thermal mantle plume Examination of surface geologic relations within four crustal plateau areas leads to new observations, and refined geologic surface histories The new observations and resulting geologic histories are difficult to accommodate in either the downwelling or the plume hypotheses, and lead to the suggestion of a third hypothesis for crustal plateau formation Additional information is included in the original extended abstract Author (revised) Venus Surface; Planetary Crusts; Plateaus; Planetary Geology 20050169983 Hawaii Univ., Honolulu, HI, USA Experimental Crystallization of Fe-rich Basalt: Application to Cooling Rate and Oxygen Fugacity of Nakhlite MIL-03346 Hammer, J E.; Rutherford, M J.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color and black and white illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document The SNC meteorites, including the clinopyroxenite-wherlite group of cumulates, Nakhla, Lafayette, and Governador Valadares, have proven integral for estimating the timing of planetary differentiation, constraining mantle compositions, and interpreting surface reflectance spectra The textures and compositions of these igneous rocks also provide clues about the intensive conditions near the planet s surface A protracted, sub-surface cooling history at oxidizing conditions has been proposed for the formation of the Nakhlites, based on the nature of chemical disequilibrium between phenocryst phases and compositions of coexisting Fe-Ti oxides The recently discovered groundmass-rich Nakhlite MIL-03346 provides a new opportunity to assess crystallization conditions of the mesostasis Cooling rate and oxygen fugacity was varied in a series of 348 experiments on Fe-rich, Al-poor synthetic starting material in order to evaluate kinetic factors governing the liquid lines of descent, modes, compositions, and textures of rapidly-cooled basalt.Fe-rich basalt synthesized from reagents was imparted with an intrinsic fO2 equivalent to the desired oxygen buffer assemblage, then placed in Mo foil, Pt-Fe alloy, or pure Pt capsules and sealed inside evacuated SiO2 glass tubes with separate, crimped containers of Fe(sup o)+FeO (IW), SiO2+Fe2SiO4+Fe3O4, (QFM), Ni(sup o)+NiO (NNO), or MnO+Mn3O4 (MNO) Samples were heated to 1210 C, annealed for 5 h, and then cooled to \h350 C at one of several constant rates (231, 71, 9, 6, or 3 C/h) Additional information is included in the original extended abstract Author (revised) Crystallization; Basalt; Nakhlites; Experimentation 20050169984 Arizona Univ., Tucson, AZ, USA Thermo-Chemical Convection in Europa’s Icy Shell with Salinity Han, L.; Showman, A P.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color and black and white illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document Europa’s icy surface displays numerous pits, uplifts, and chaos terrains that have been suggested to result from solid-state thermal convection in the ice shell, perhaps aided by partial melting However, numerical simulations of thermal convection show that plumes have insufficient buoyancy to produce surface deformation Here we present numerical simulations of thermochemical convection to test the hypothesis that convection with salinity can produce Europa’s pits and domes Our simulations show that domes (200-300 m) and pits (300-400 m) comparable to the observations can be produced in an ice shell of 15 km thick with 5-10% compositional density variation if the maximum viscosity is less than 10(exp 18) Pa sec Additional information is included in the original extended abstract Author Europa; Ice; Convection; Salinity; Satellite Surfaces; Thermal Simulation 20050169985 Hawaii Univ., Honolulu, HI, USA The Earliest Mare Basalts Hawke, B R.; Gillis, J J.; Giguere, T A.; Blewett, D T.; Lawrence, D J.; Lucey, P G.; Peterson, C A.; Smith, G A.; Spudis, P D.; Taylor, G J.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document Cryptomaria are covered or hidden mare deposits that are obscured from view by the emplacement of subsequent deposits of higher albedo Investigations of cryptomaria can provide information that is critical to understanding the evolution of the Moon At present, the time of the onset of mare volcanism is not accurately known Since cryptomaria represent the earliest mare basalts, determination of their ages will provide information concerning the initiation of extrusive mare volcanism Cryptomaria were formed by magmas generated by very early partial melting of the lunar mantle Chemical data for cryptomaria provide evidence concerning the composition of these early partial melts We have used FeO, TiO2, and optical maturity maps produced from Clementine UV-VIS images, Lunar Prospector orbital chemistry data, Earth-based near-IR reflectance spectra, and a variety of spacecraft imagery to identify cryptomare deposits and to investigate the ages and compositions of the buried mare basalts Derived from text Basalt; Lunar Maria; Volcanology; Mineral Deposits 20050169986 Raytheon Co., Tucson, AZ, USA Autonomous Low Cost Precision Lander for Lunar Exploration Head, J N.; Hoppa, G V.; Gardner, T G.; Seybold, K S.; Svitek, T.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document For 60 years the US Defense Department has invested heavily in producing small, low mass, precision guided vehicles The technologies matured under these programs include terrain-aided guidance and navigation, closed loop terminal guidance algorithms, robust autopilots, high thrust-to-weight propulsion systems , autonomous mission management software, sensors, vehicle state estimation, and data fusion These technologies will aid NASA in addressing the requirements flowing from the Vision for Space Exploration articulated in January 2004 as well as New Millennium Science and Technology Establishing and resupplying a long term lunar presence will require automated landing precision not demonstrated to date Precision 349 landing (CEP less than 10 m) will allow the targeting of scientifically interesting locations heretofore off-limits due to vehicle safety and mission success concerns In the DOD world, precision guidance and the associated enabling technologies are used routinely and reliably Hence, it is timely to generate a point design based on these mature technologies for a precise planetary lander useful for lunar exploration In this design science instruments amount to 10 kg, 16% of the lander vehicle mass This compares favorably with 7% for Mars Pathfinder and less than 15% for Surveyor Derived from text Autonomy; Low Cost; Lunar Exploration; Mars Landing Sites 20050169987 NASA Ames Research Center, Moffett Field, CA, USA Northern Hemisphere Gullies on Mars: Analysis of Spacecraft Data and Implications for Formation Mechanisms Heldmann, J L.; Johansson, H.; Carlsson, E.; Mellon, M T.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document The origin of geologically recent gullies on Mars has remained controversial since the discovery of these features by Malin and Edgett in 2000 Numerous models have been proposed which invoke various physical processes as well as various agents of erosion to explain the origin of the Martian gullies Hypotheses to explain the formation of the gullies invoke shallow liquid water aquifers, deep liquid water aquifers, melting ground ice, snowmelt, dry landslides, and carbon dioxide aquifers We test the validity of such gully formation mechanisms by analyzing data from the Mars Global Surveyor and Mars Odyssey spacecrafts to uncover trends in the dimensional and physical properties of the gullies and their surrounding terrain A similar study has previously been completed for gullies located in the southern hemisphere of Mars The work presented here focuses exclusively on gullies in the northern hemisphere based on the identification of 136 Mars Orbiter Camera (MOC) images containing clear evidence of gully landforms, distributed in the northern mid and high latitudes These sites have been analyzed in combination with Mars Orbiter Laser Altimeter (MOLA), Thermal Emission Spectrometer (TES), and Gamma Ray Spectrometer (GRS) data to provide quantitative measurements of numerous gully characteristics Parameters measured include apparent source depth and distribution, vertical and horizontal dimensions, slopes, compass orientations, near-surface ice content, and factors controlling present-day climatic conditions Derived from text Northern Hemisphere; Mars Surface; Aquifers 20050169988 NASA Ames Research Center, Moffett Field, CA, USA Formation of Martian Gullies by the Action of Liquid Water Flowing Under Current Martian Environmental Conditions Heldmann, J L.; Toon, O B.; Pollard, W H.; Mellon, M T.; Pitlick, J.; McKay, C P.; Andersen, D T.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains black and white illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document Images from the Mars Orbiter Camera (MOC) on the Mars Global Surveyor (MGS) spacecraft show geologically young small-scale features resembling terrestrial water-carved gullies An improved understanding of these features has the potential to reveal important information about the hydrological system on Mars, which is of general interest to the planetary science community as well as the field of astrobiology and the search for life on Mars The young geologic age of these gullies is often thought to be a paradox because liquid water is unstable at the Martian surface Current temperatures and pressures are generally below the triple point of water (273 K, 6.1 mbar) so that liquid water will spontaneously boil and/or freeze We therefore examine the flow of water on Mars to determine what conditions are consistent with the observed features of the gullies Derived from text Extraterrestrial Life; Mars Surface; Water Currents; Mars Environment; Water Flow 20050169989 Jet Propulsion Lab., California Inst of Tech., Pasadena, CA, USA An Overview of Cassini UVIS Icy Satellite Results So Far Hendrix, A R.; Hansen, C J.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document The icy satellites of the Saturn system exhibit a remarkable amount of variability From dark, battered Phoebe orbiting at 200 R(sub S) to black-and-white Iapetus, the wispy streaks of Dione, heavily cratered Tethys and Mimas, to potentially geologically active Enceladus, the extent of geological phenomena exhibited by these bodies is tremendous Phoebe, Iapetus 350 and Hyperion all orbit outside Saturn s magnetosphere, while Mimas, Enceladus, Dione Tethys and Rhea all orbit within the magnetosphere Furthermore, Mimas, Enceladus, Tethys and Dione all orbit within the E-ring so the extent of exogenic effects on these icy satellites is wide-ranging After 9 months in orbit around Saturn, we present UV results so far from Phoebe, Tethys, Dione, Iapetus, Mimas, Enceladus and Rhea We expect that the UV signatures of these icy satellites are strongly influenced not only by their composition, but by external effects and magnetospheric environments Derived from text Icy Satellites; Ultraviolet Spectra; General Overviews; Cassini Mission 20050169990 Jet Propulsion Lab., California Inst of Tech., Pasadena, CA, USA Iapetus and Phoebe as Measured by the Cassini UVIS Hendrix, A R.; Hansen, C J.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document The bizarre appearance of Iapetus has long intrigued researchers of this Saturnian moon The leading hemisphere is very dark and reddish in color at visible-near-IR wavelengths In contrast, the trailing hemisphere is relatively bright and its near-IR spectrum is dominated by water ice The severe hemispherical brightness dichotomy has been explained by both endogenic and exogenic models The primary endogenic model involves eruption of dark material onto the leading hemisphere from the interior of Iapetus Exogenic models include exposure of dark underlying material by micrometeorite bombardment, contamination of Iapetus leading hemisphere by Titan tholin material, and the coating of the leading hemisphere by Phoebe dust It has been shown that the dark material on Iapetus leading hemisphere is redder in color at visible wavelengths than Phoebe, which is spectrally gray at visible wavelengths An additional exogenic model involves the coating of both Iapetus leading hemisphere and Hyperion with material from small retrograde satellites, which are reddish in color at visible wavelengths We present the first FUV spectra of Iapetus and Phoebe to investigate whether the UV wavelength range can contribute to solving the puzzle of Iapetus Derived from text Iapetus; Ultraviolet Radiation; Light (Visible Radiation); Phoebe; Cassini Mission 20050169991 Manchester Univ., UK IDLE: (Interstellar Dust Laser Explorer), a New Instrument for Submicron Analyses of Stardust - Quantification in SIMS and Laser SNMS Henkel, T.; Tizard, J.; Lyon, I.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document Pre-solar grains are circumstellar condensates that survived the formation of the solar system and can be found in primitive meteorites As direct samples of extreme astrophysical environments, analysis of these grains is the only way to study, within the laboratory, nucleosynthetic processes occurring in stars The main types of grains discovered are silicon carbide, diamond, graphite, silicon nitride and corundum The study of their extreme isotopic compositions (isotope ratios of carbon, oxygen, magnesium and silicon may vary by up to 4 orders of magnitude compared with terrestrial materials) is currently being used to directly model nucleosynthetic processes in AGB stars, novae and supernovae The grains may also be structured on a sub-micron scale and retain evidence of their passage through interstellar space In a 1 micron diameter grain there are as few as several thousand atoms of each of the heavy elements (especially rare earth elements and actinides) requiring an average detection efficiency for these low abundance elements of at least 1% and preferably greater than 10% An instrument capable of analyzing element and isotope ratios in these grains must therefore be able to achieve a spatial resolution of at least 100nm and be able to extract and detect atoms from the grain with very high efficiency Derived from text Astrophysics; Interstellar Matter; Stardust Mission; Secondary Ion Mass Spectrometry; Lasers 20050169992 NASA Ames Research Center, Moffett Field, CA, USA Overview of Athena Microscopic Imager Results Herkenhoff, K.; Squyres, S.; Arvidson, R.; Bass, D.; Bell, J., III; Bertelsen, P.; Cabrol, N.; Ehlmann, B.; Farrand, W.; Gaddis, L., et al.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains black and white illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document The Athena science payload on the Mars Exploration Rovers (MER) includes the Microscopic Imager (MI) The MI is 351 a fixed-focus camera mounted on an extendable arm, the Instrument Deployment Device (IDD) The MI acquires images at a spatial resolution of 31 microns/pixel over a broad spectral range (400 - 700 nm) The MI uses the same electronics design as the other MER cameras but its optics yield a field of view of 32 32 mm across a 1024 1024 pixel CCD image The MI acquires images using only solar or skylight illumination of the target surface The MI science objectives, instrument design and calibration, operation, and data processing were described by Herkenhoff et al Initial results of the MI experiment on both MER rovers (Spirit and Opportunity) have been published previously Highlights of these and more recent results are described Derived from text Mars Exploration; General Overviews; Mars Roving Vehicles; Imaging Techniques 20050169994 Morgan State Univ., Baltimore, MD, USA Anomalous Spectra of High-Ca Pyroxenes: Further Correlations Between NIR and Mossbauer Patterns Hoffman, E J.; Schade, U.; Moroz, L.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document Near-infrared (NIR) reflectance spectroscopy gives intriguing results for three well studied angrites, meteorites containing large abundances of high-Ca pyroxenes Their spectra correspond to the Type A (normal) and Type B (anomalous) patterns that turn up almost at random in spectra of terrestrial high-Ca pyroxenes (clinopyroxenes) Fe ions are responsible for the pertinent absorption bands, and an additional Fe sensitive method, Mossbauer spectroscopy, shows a similar dichotomy of results, with an anomalously intense ferric-ion signature appearing for most NIR Type B samples In a few samples, detailed microscopic analysis suggests that minute amounts of iron-rich minor phases may be responsible NIR spectroscopy is a principal tool in the study of igneous rock whether remote or in the laboratory, so planetary science would benefit from knowledge of the origin and probable extent of the anomaly This report presents Mossbauer data for an additional set of NIR-characterized pyroxenes in the hope of contributing to clarification Derived from text Anomalies; Pyroxenes; Calcium; Near Infrared Radiation; Infrared Spectra 20050169995 Hawaii Univ., Honolulu, HI, USA Alteration Phases Associated with High Concentrations of Orthopyroxene and Olivine on Mars Hamilton, V E.; Schneider, R D.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document Data collected by the Mars Global Surveyor Thermal Emission Spectrometer (TES) have revealed numerous regions on Mars with high abundances of olivine relative to typical Martian basalts and a single location with high abundances (up to 40 vol %) of orthopyroxene These high concentrations of mafic materials were identified initially using band matching approaches or deconvolutions that used lithologic, rather than mineral, end members Based on new deconvolution analyses using mineral end members, we now are able to place quantitative constraints on the abundances of alteration phases associated with high concentrations of orthopyroxene and olivine on Mars Additional information is included in the original extended abstract Author (revised) Mars (Planet); Planetary Composition; Mineralogy; Planetary Geology; Pyroxenes; Olivine 20050169997 Jet Propulsion Lab., California Inst of Tech., Pasadena, CA, USA Ultraviolet Views of Enceladus, Tethys, and Dione Hansen, C J.; Hendrix, A R.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document The Cassini Ultraviolet Imaging Spectrograph (UVIS) has collected ultraviolet observations of many of Saturn’s icy moons since Cassini’s insertion into orbit around Saturn We will report on results from Enceladus, Tethys and Dione, orbiting in the Saturn system at distances of 3.95, 4.88 and 6.26 Saturn radii, respectively Icy satellite science objectives of the UVIS include investigations of surface age and evolution, surface composition and chemistry, and tenuous exospheres We address these objectives by producing albedo maps, and reflection and emission spectra, and observing stellar occultations UVIS has four channels: EUV: Extreme Ultraviolet (55 nm to 110 nm), FUV: Far Ultraviolet (110 to 190 nm), HSP: High Speed Photometer, and HDAC: Hydrogen-Deuterium Absorption Cell The EUV and FUV spectrographs image onto a 2-dimensional 352 detector, with 64 spatial rows by 1024 spectral columns To-date we have focused primarily on the far ultraviolet data acquired with the low resolution slit width (4.8 angstrom spectral resolution) Additional information is included in the original extended abstract Author (revised) Ultraviolet Astronomy; Enceladus; Tethys; Dione; Ultraviolet Spectrometers 20050169998 Jet Propulsion Lab., California Inst of Tech., Pasadena, CA, USA A Cassini ISS Search for Regolith-Texture Variations on Tethys Helfenstein, P.; Thomas, P.; Ververka, J.; Denk, T.; Neukum, G.; West, R A.; Knowles, B.; Porco, C.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains black and white illustrations; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document On October 28, 2004 the Cassini spacecraft flew within 255,500km of Saturn’s heavily-cratered icy moon, Tethys The ISS Narrow Angle Camera (NAC) obtained its first closeup multi-color images of Tethys at a Voyager-comparable spatial resolution of 1.5 km/pixel The imaging sequence provided 23 NAC images covering 10 NAC color-filter bandpasses (ranging from 338nm to 930nm wavelengths), as well as a Wide Angle Camera (WAC), 3-color (BGR) image set The images show whole-disk views of Tethys’ trailing hemisphere viewed at a phase angle of 50 degrees and with a sub-spacecraft point of (22 deg N, 270 deg W) At the spatial resolution of our NAC images, Tethys’ 1060 km diameter presents a disk-size of about 350 pixels Among the images returned are nine frames obtained through NAC polarization-filters at three different spectral bandpasses (UV3: 341nm, GRN: 569nm, and MT2: 727 nm, respectively) In the present study, we use these polarization images to search for possible variations in the microscopic texture of regolith on Tethys Derived from text Cassini Mission; Regolith; Tethys; Textures; International Space Station 20050169999 NASA Johnson Space Center, Houston, TX, USA Meteorite WIS91600: A New Sample Related to a D- or T-type Asteroid Hiroi, T.; Tonui, E.; Pieters, C M.; Zolensky, M E.; Ueda, Y.; Miyamoto, M.; Sasaki, S.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Original contains color illustrations Contract(s)/Grant(s): NAG5-13609; NAG5-12847; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document Since the Tagish Lake meteorite fell in January 2000, the assumed one-of-the-kind meteorite has become the hottest issue among a diversity of scientists Meanwhile, as the physical origin of the meteorite in our solar system, D or T asteroids have been suggested by Hiroi et al based on comparison of their visible-near-infrared (VNIR) reflectance spectra While it is probably still true that the Tagish Lake meteorite is possibly the first recovered sample from a D or T asteroid as a meteorite fall, we report in this paper that the meteorite WIS91600 may actually be the first recovered sample from one of those asteroids as a meteorite find Derived from text Asteroids; Meteoritic Composition; Solar System 20050170000 NASA Johnson Space Center, Houston, TX, USA Detailed Mineralogical Characterizations of Four S-Asteroids: 138 Tolosa, 306 Unitas, 346 Hermentaria, and 480 Hansa Hardersen, P S.; Gaffey, M J.; Abell, P A.; Lunar and Planetary Science XXXVI, Part 8; [2005]; 2 pp.; In English; See also 20050169945; Copyright; Avail: CASI; A01, Hardcopy; Available from CASI on CD-ROM only as part of the entire parent document The S-asteroid taxonomic class is the second largest grouping of main-belt asteroids that are primarily located in the inner main belt (a \h 3.0 AU) [1] These asteroids have historically been the subject of interest within the asteroid community for several reasons Continuing discussions about the nature of the S-asteroids (ordinary chondrite-like or thermally-evolved) and the putative space weathering effect on S-asteroids serve as examples of issues currently unresolved within the community [2,3] Despite this general interest, detailed mineralogical investigations of individual S-asteroids has been relatively rare A few workers have studied individual, or small groups of, S-asteroids [4,5,6,7] Gaffey et al [2] published their S-asteroid survey in 1993 that characterized 39 of the 144 then-classified S-asteroids Despite the work already accomplished, the need 353 ... generates heading and speed commands to maneuver the vehicle towards the desired position The vehicle controller executes the speed and heading commands and ensures the vehicle fast and safe response... mechanics; space plasmas; and interstellar and interplanetary gases and dust 20050 169 562 Johns Hopkins Univ., Baltimore, MD, USA FUSE Observations of QSOs behind Galaxy Clusters and of Galactic O VI... approx 50 - 60 and less than 50 x 160 pixels across the nucleus, yet it sufficed for groups at the USGS and DLR to produce digital elevation models (DEMs) and study the morphology and photometry