Planetary Science Institute

MULTIPLE YEAR AWARD WITH INCREMENTAL FUNDING FOR YEARS ONE TO FIVE. THIS PROPOSAL IS ENTITLED "TREX: TOOLBOX FOR RESEARCH AND EXPLORATION." THIS IS AWARDED IN RESPONSE TO COOPERATIVE AGREEMENT NOTICE (CAN) NO. NNH16ZDA009C NASA SOLAR SYSTEM EXPLORATION RESEARCH VIRTUAL INSTITUTE (SSERVI) CYCLE THREE. THE PRINCIPAL INVESTIGATOR IS DR. AMANDA R. HENDRIX WITH PLANETARY SCIENCE INSTITUTE (PSI). PROJECT SUMMARY: THE OVERARCHING GOAL OF THE TREX TEAM IS DEVELOP TOOLS AND RESEARCH METHODS FOR EXPLORATION OF AIRLESS SURFACES THAT ARE COATED IN FINE-GRAINED DUST TO PREPARE FOR HUMAN MISSIONS. OUR TEAM WILL USING LABORATORY SPECTRAL MEASUREMENTS AND EXPERIMENTS ACCOMPANIED BY STUDIES OF EXISTING DATA FROM THE MOON AND SMALL BODIES TO UNDERSTAND THEIR SURFACE CHARACTERISTICS AND TO INVESTIGATE IN SITU RESOURCE UTILIZATION (ISRU) POTENTIAL ON SMALL-BODY TARGETS. ADDITIONALLY OUR TEAM WILL DEVELOP INSTRUMENTATION (ESPECIALLY ULTRA-VIOLET_UV_VISIBLE CAPABILITIES) AND SOFTWARE FOR FUTURE USE AT THOSE BODIES (EITHER REMOTELY AND/OR WITH HUMANS). THESE TOOLS WILL IMPROVE MISSION SUCCESS BY DECREASING RISK AND ASSURING THE SAFETY OF ASTRONAUTS AND SPACECRAFT. THE TREX TASKS COMPLEMENT THOSE OF CURRENT SSERVI TEAMS BY EMPHASIZING ANALYSES OF THE FINEST FRACTION OF GRAINS AND UV WAVELENGTHS. TREX HAS 4 THEMES THAT WILL BE ADDRESSED THROUGH THE LIFE TIME OF THE AWARD. THEY ARE: 1) DEVELOPMENT OF NON-AMBIENT (VACUUM MULTI-TEMPERATURE) BROAD WAVELENGTH SPECTRAL DATABASE OF PLANETARY MATERIALS. WE WILL UTILIZE A RANGE OF FACILITIES TO MAKE THE SPECTRAL MEASUREMENTS WITH UNIQUE AND OVERLAPPING CAPABILITIES IN ORDER TO DERIVE A ROBUST SET OF CROSS-CALIBRATED LAB DATA. 2) INVESTIGATIONS OF FINE-GRAINED MATERIALS ON THE LUNAR SURFACE. LAB DATA FROM THEME ONE WILL BE USED ALONG WITH SPACECRAFT DATA OF THE MOON AND MODELING TECHNIQUES TO CHARACTERIZE LUNAR GRAIN SIZE MINERALOGY AND CORRELATIONS WITH GEOLOGIC FEATURES WITH AN OVERALL GOAL OF INVESTIGATION ISRU POTENTIAL AND FUTURE INSTRUMENT DEVELOPMENT NEEDS. 3) INVESTIGATIONS OF FINE GRAINED MATERIALS ON THE SURFACES OF SMALL BODIES. NEAR EARTH OBJECTS (NEO) AND THE MARTIAN MOONS ARE POTENTIAL FUTURE HUMAN DESTINATIONS AND EVOKE A NUMBER OF CRITICAL QUESTIONS REGARDING THE DIVERSITY OF THEIR COMPOSITIONS AND DYNAMICAL HISTORIES. AND 4) DECISION-MAKING IN A FINE-GRAINED ANALOG ENVIRONMENT. WE WILL DEVELOP BOTH SOFTWARE AND INSTRUMENTATION FOR SUE IN THE FIELD AS A TESTING GROUND FOR FUTURE ROBOTIC PLANETARY USES. THE TASKS ACCOMPLISHED BY THE TREX TEAM WILL ENABLE NASA' EXPLORATION OF THE MOON NEO AND THE MOONS OF THE MARS BY ACQUIRING THE INFORMATION AND KNOWLEDGE THAT WILL SERVE AS TOOLS FOR FUTURE HUMAN AND ROBOTIC EXPLORATION. TREX HAS ASSEMBLED AN INTERNATIONAL TEAM OF EXPERTS TO ADDRESS THESE FOUR THEMES LEVERAGING A NUMBER OF MEMBERS OF THE EXISTING DISTRIBUTED PSI STAFF STRUCTURE AND THEIR EXTENSIVE KNOWLEDGE OF THE MOON SMALL BODIES DATA ANALYSIS AND INSTRUMENT TECHNIQUES AND BY INCORPORATING STUDENTS POST-DOCTORAL RESEARCHERS AND KEY PARTNERS AT OTHER INSTITUTIONS.

RENEWAL FOR THE COOPERATIVE AGREEMENT NOTICE - THE SMALL BODIES NODE OF NASA'S PLANETARY DATA SYSTEM WITH THE MINOR PLANET CENTER

PURPOSE THE OVERALL GOAL IS TO CURATE THE EXISTING AND ARCHIVE THE FUTURE SMALL BODIES DATA (COMETS, ASTEROIDS, METEORITES, NEOS, TNOS), ACT AS LEAD

THE ULTRAVIOLET MICROMIRROR IMAGING SPECTROGRAPH

THE SMALL BODIES NODE (SBN) WAS FIRST CREATED IN A CALL FOR PROPOSALS APPROXIMATELY 15 YEARS AGO. THE ORIGINAL TEAM WAS FORMED FROM PARTICIPANTS IN T

THE NEAR INFRARED VOLATILES SPECTROMETER SYSTEM (NIRVSS) IS AN INSTRUMENT PACKAGE DESIGNED TO ACQUIRE IMAGING AND SPECTRAL DATA OF TARGETS WITHIN THE LUNAR PERMANENTLY SHADED REGIONS (PSRS). AT ITS CORE THE INSTRUMENT CONSISTS OF A MONOCHROMATIC IMAGER AND A SPECTROMETER THAT COVERS THE WAVELENGTH RANGE OF 1.3 M TO 4 M AT A SPECTRAL RESOLUTION OF 15 TO 30 NM. THE IMAGER USES A SET OF COLOR LEDS TO ILLUMINATE THE TARGET AT DIFFERENT WAVELENGTHS WHEREAS A TUNGSTEN LAMP ILLUMINATES THE TARGET FOR THE SPECTROMETER. THREE VERSIONS OF THIS INSTRUMENT ARE EXPECTED TO FLY TO THE MOON AS PAYLOADS ON THE ASTROBOTICS LANDER ON CL19 AND ON THE VOLATILES INVESTIGATING POLAR EXPLORATION ROVER (VIPER) TO BE LAUNCHED ON 2021 2022 AND 2023 RESPECTIVELY. WE PROPOSE HERE TO SUPPORT THE DEVELOPMENT AND OPERATIONS OF NIRVSS BY: 1) DEVELOPING DATA ANALYSIS TOOLS TO USE IN THE INTERPRETATION OF NIRVSS DATA. 2) SUPPORTING DATA ANALYSIS AND INTERPRETATION. 3) PREPARING THE DATA FOR RELEASE WITH THE PDS.

WE PLAN TO INVESTIGATE GEOLOGIC AND TOPOGRAPHIC SETTINGS AND TRIGGERS OF LARGE HISTORIC PRE-HISTORIC AND FUTURE LANDSLIDES IN THE HIMALAYA AND KARAKORAM INCLUDING RIVER DAMMING AND OTHER ASSOCIATED HAZARDOUS EVENTS OF TRANSBOUNDARY CONSEQUENCES. THE REGION OF INTEREST INVOLVES THE INTERNATIONAL BORDER AREAS WITHIN THE LARGER REGION DEPICTED IN FIGURE 1. WE WILL MODEL SUSCEPTIBILITIES OF THE TERRAIN TO PRODUCE SIMILAR LARGE LANDSLIDES IN THE FUTURE DUE TO ICE MELT SEISMICITY OR STOCHASTIC FAILURES. WE WILL USE U OF A S DISTRIBUTED MEMORY CLUSTER TO COMPUTE SEISMIC WAVE PROPAGATION AND SURFACE INTERACTION IN THE COMPLEX TOPOGRAPHY AND FIRST-ORDER GEOLOGIC STRUCTURE OF THE 2015 GORKHA-EARTHQUAKE-AFFECTED HIMALAYAN REGION AND THE 2005 KASHMIR EARTHQUAKE AREA IN THE KARAKORAM. SHAKING-RELATED LANDSLIDE SUSCEPTIBILITY WILL BE TESTED USING OUTCOME OF THE 2015 GORKHA EARTHQUAKE; MONSOON RELATED LANDSLIDES WILL BE EVALUATED NEARBY BUT WHERE SEISMICITY WAS WEAK.

COLLABORATIVE RESEARCH: CULTIVATING TOMORROW'S INNOVATORS THROUGH EXPLORING PLANETARY IMAGES WITH ARTIFICIAL INTELLIGENCE -THE RAPID PERMEATION OF AI INTO NEARLY ALL WALKS OF LIFE AND EVERY PROFESSION CALLS FOR INNOVATIVE APPROACHES OF PUBLIC AI LITERACY AND EDUCATION IN ALL SETTINGS. THIS PROJECT WILL DESIGN, DEVELOP, AND TEST A SEQUENCE OF LESSONS FOR HIGH SCHOOL AGED YOUTH FROM EAST TENNESSEE THAT WILL TEACH THEM ARTIFICIAL INTELLIGENCE CONCEPTS BY USING IMAGES FROM PLANETARY EXPLORATION AND EMERGING GENERATIVE AI TOOLS TO CREATE VISUALLY APPEALING GENERATIVE ARTWORKS AND DIGITAL STORIES. AI CONCEPTS GROUNDED IN TOPICS THAT ARE RELEVANT AND ENGAGING THROUGH THE LENS OF CREATIVE WORKS CAN SERVE AS AN INVITATION FOR UNDERREPRESENTED AND UNDER-RESOURCED YOUTHS TO EXPLORE FIELDS THAT THEY WOULD NOT OTHERWISE CHOOSE OR HAVE THE OPPORTUNITY TO LEARN ABOUT. THE PROJECT TEAM INCLUDING AI RESEARCHERS AND EDUCATORS, STEM DISCIPLINARY EXPERTS AND THE BROADER CREATIVE WORKS COMMUNITY WILL EMPLOY A MIXTURE OF OUT-OF-SCHOOL AND ONLINE ACTIVITIES, INTEGRATING PLANETARY SCIENCE, PLANETARY EXPLORATION, BIG DATA, CREATIVE WORKS, AND GENERATIVE AI. THE WORKS CREATED BY YOUTHS WITH THE ASSISTANCE OF GENERATIVE AI AND VALIDATED BY SCIENTISTS ON PLANETARY EXPLORATION AND PLANETARY SCIENCE WILL BE SHOWCASED ONLINE, AT THE AMERICAN MUSEUM OF SCIENCE AND ENERGY, AND OTHER PUBLIC PLACES. THIS INTEGRATING RESEARCH & PRACTICE PROJECT IS FUNDED BY THE ADVANCING INFORMAL STEM LEARNING (AISL) PROGRAM, WHICH SUPPORTS PROJECTS THAT: (A) CONTRIBUTE TO RESEARCH AND PRACTICE THAT CONSIDERS INFORMAL STEM LEARNING'S ROLE IN EQUITY AND BELONGING IN STEM; (B) PROMOTE PERSONAL AND EDUCATIONAL SUCCESS IN STEM; (C) ADVANCE PUBLIC ENGAGEMENT IN SCIENTIFIC DISCOVERY; (D) FOSTER INTEREST IN STEM CAREERS; (E) CREATE AND ENHANCE THE THEORETICAL AND EMPIRICAL FOUNDATIONS FOR EFFECTIVE INFORMAL STEM LEARNING; (F) IMPROVE COMMUNITY VIBRANCY; AND/OR (G) ENHANCE SCIENCE COMMUNICATION AND THE PUBLIC'S ENGAGEMENT IN AND UNDERSTANDING OF STEM AND STEM PROCESSES, AND CO-FUNDED BY THE INNOVATIVE TECHNOLOGY EXPERIENCES FOR STUDENTS AND TEACHERS (ITEST) PROGRAM, WHICH SUPPORTS PROJECTS THAT BUILD UNDERSTANDINGS OF PRACTICES, PROGRAM ELEMENTS, CONTEXTS AND PROCESSES CONTRIBUTING TO INCREASING STUDENTS' KNOWLEDGE AND INTEREST IN SCIENCE, TECHNOLOGY, ENGINEERING, AND MATHEMATICS (STEM) AND INFORMATION AND COMMUNICATION TECHNOLOGY (ICT) CAREERS. OVER THE THREE-YEAR PROJECT DURATION, THE PROJECT WILL DIRECTLY IMPACT APPROXIMATELY 360 HIGH SCHOOL YOUTH AND WILL REACH OUT TO A MUCH LARGER NUMBER OF PARTICIPANTS THROUGH ONLINE WEBINARS, WORKSHOPS, NEWSLETTERS, AND EXHIBITS. THE PROJECT WILL INVESTIGATE FOUR RESEARCH QUESTIONS: (1) HOW DOES PARTICIPATION IN AN INTERDISCIPLINARY OUT-OF-SCHOOL STEM PROGRAM INFLUENCE HIGH SCHOOL YOUTHS' AI KNOWLEDGE AND SKILLS, STEM ENGAGEMENT AND IDENTITY, AND SENSE OF BELONGING TO A SCIENTIFIC COMMUNITY? (2) WHAT DO YOUTHS LEARN ABOUT THE VALUE OF THEIR PERSONAL AND CULTURAL KNOWLEDGE AND SKILLS (I.E., ASSETS) TO THE LOCAL AND BROADER COMMUNITY? (3) WHAT PROGRAM CHALLENGES, FEATURES, AND CONTENT APPEAR TO HAVE THE GREATEST INFLUENCE ON ENGAGEMENT, IDENTITY, AND BELONGING? (4) HOW DO OUTCOMES VARY BY YOUTH DEMOGRAPHICS INCLUDING GENDER, ETHNICITY, AND URBAN/RURAL ENVIRONMENT? THE RESEARCH WILL USE A MIXED-METHODS DESIGN, COMBINING QUANTITATIVE SURVEYS WITH QUALITATIVE WRITTEN REFLECTIONS AND PICTURES WITH COMMENTARY. IN THE FINAL YEAR OF THE PROJECT, PROFESSIONAL DEVELOPMENT WORKSHOPS WILL TRAIN EDUCATORS TO USE LEARNING MATERIALS GENERATED FROM THE PROJECT. RESEARCH FINDINGS PRODUCED THROUGH THIS WORK WILL CONTRIBUTE NEW KNOWLEDGE ON METHODS AND LEARNING DESIGNS IN INTEGRATING AI, STEM AND ART FOR INFORMAL STEM EDUCATION. THIS AWARD REFLECTS NSF'S STATUTORY MISSION AND HAS BEEN DEEMED WORTHY OF SUPPORT THROUGH EVALUATION USING THE FOUNDATION'S INTELLECTUAL MERIT AND BROADER IMPACTS REVIEW CRITERIA.- SUBAWARDS ARE PLANNED FOR THIS AWARD.

THIS PROPOSAL IS TO SUPPORT THE PI'S ACTIVITIES AS DEPUTY PRINCIPAL INVESTIGATOR OF THE CHEMIN MINERALOGICAL INSTRUMENT THAT IS PART OF THE MARS SCIE

MOTIVATION: THE LUNAR HEAT FLUX RADIOMETER (HFR) WILL PEER INTO THE LUNAR SUBSURFACE USING MICROWAVE WAVELENGTHS (~10-200CM 300MHZ TO 6GHZ AND A 90GHZ SURFACE RADIOMETER) PROVIDING A MEASUREMENT OF GEOTHERMAL HEAT FLUX WITHOUT NEED FOR DRILLING.

22-MDAP22_2-0035 HIGH-RESOLUTION 3D RADAR MAPPING ANALYSIS AND MODELING OF THE INTERNAL LAYERS WITHIN THE NORTH POLAR LAYERED DEPOSITS

UNDERSTANDING RADIATION PROCESSING AND ALTERATION OF ICY REGOLITHS

22-ANGSA22_2-0002 SPECTROSCOPIES FOR ASSESSING REDOX CONDITIONS (SPARC)

SHAPE, TOPOGRAPHY AND INTERNAL STRUCTURE OF MERCURY FROM MDIS DATA DURING THE PAST TWO DECADES, I HAVE DEVELOPED TECHNIQUES FOR COMBINING STEREOGRAPH

INVESTIGATING THE GEOPHYSICAL CONTROL OF 67P CHURYUMOV GERASIMENKOS OUTBURST PLUMES

SATELLITE ALTIMETRY HAS RESHAPED OUR VISION OF THE GLOBAL EDDY FIELD WITH LONG-LIVED PROPAGATING COHERENT EDDIES NOW UNDERSTOOD TO BE A MAJOR FEATURE OF THE OCEAN CIRCULATION. MUCH OF OUR UNDERSTANDING OF THE GLOBAL EDDY FIELD IS BASED ON GRIDDED

PLANETARY SCIENCE INSTITUTE US NEAR-EARTH OBJECT SURVEILLANCE SATELLITE SCIENCE TEAM SUPPORT: THIS PROPOSAL REQUESTS SUPPORT FOR THE PARTICIPATION

THE AIM OF THE PROPOSED WORK IS TO EVALUATE A NEW SCINTILLATOR, EUROPIUM DOPED STRONTIUM IODIDE, FOR PLANETARY GAMMA RAY SPECTROSCOPY. THE PROPOSAL W

WE PROPOSE TO STUDY AN INSTRUMENT CONCEPT TO IMPROVE UPON CURRENT CAPABILITIES IN UV IMAGING SPECTROSCOPY FOR PLANETARY USES. THE CONCEPT IS A UV MICROMIRROR SPECTROGRAPH WITH A WIDE VARIETY OF POTENTIAL APPLICATIONS INCLUDING DISCOVERY- AND NEW FRONTIERS-CLASS MISSIONS. THE STATE-OF-THE-ART UV IMAGING SPECTROGRAPHS SUCH AS THE SWRI-BUILT ALICE INSTRUMENTS (INCLUDING JUNO UVS ROSETTA ALICE AND LRO LAMP) AND THE LASP-BUILT CASSINI UVIS AND MAVEN IUVS RETURN USEFUL DATASETS FROM THEIR TARGETS AND HAVE OPENED UP THE FIELD TO THE NEXT QUESTIONS TO ADDRESS. RECENT TECHNOLOGICAL ADVANCES HAVE ENABLED INSTRUMENT IMPROVEMENTS FOR THE NEXT GENERATION OF PLANETARY SCIENCE MISSIONS. FURTHERMORE A RANGE OF POSSIBLE UPCOMING MISSIONS COULD SUCCESSFULLY UTILIZE SUCH IMPROVED UV INSTRUMENTATION. THE GOAL OF THIS PROGRAM IS TO DEVELOP A PROOF-OF-CONCEPT INSTRUMENT FOR INTEGRAL FIELD FAR-UV SPECTROSCOPY. BY UTILIZING A PAIR OF DIGITAL MICROMIRROR ARRAYS THIS CONCEPT INSTRUMENT WILL BE CAPABLE OF DISSECTING THE FOCAL PLANE AND RE-FORMING IT INTO A SERIES OF SLITSHAPES TO OVERCOME THE LIMITATIONS OF SPECTRAL CONFUSION. THE TRL OF THE SYSTEM IS CURRENTLY ESTIMATED AT ~2. WE EXPECT TO ADVANCE THE TRL TO ~4 THROUGH THIS PICASSO PROGRAM TO BE READY TO PROPOSE TO MATISSE FOR FOLLOW-ON WORK AND FURTHER TRL ADVANCEMENT.

NASA S DAWN SPACECRAFT COMPLETED ITS YEARLONG MAPPING MISSION AROUND ASTEROID (4) VESTA IN AUGUST 2012. DURING THIS PERIOD, THE DAWN FRAMING CAMERA (

THIS PROPOSAL COVERS DR. DAVID VANIMAN'S ACTIVITIES AS A CO-INVESTIGATOR FOR THE CHEMIN MINERALOGICAL INSTRUMENT WHICH IS PART OF THE INSTRUMENT SUITE ON THE MARS SCIENCE LABORATORY (MSL) ROVER CURIOSITY DURING THE EXTENDED MISSION PHASE THROUGH 2019 AND INTO 2021. THE PROPOSAL INCLUDES CONTINUING SUPPORT FOR STEVE CHIPERA AS WELL AS COVERAGE FOR DR. PATRICIA CRAIG AS A CHEMIN POST-DOCTORAL RESEARCH SCIENTIST. DR. VANIMAN WAS A NAMED CO-I ON THE ORIGINAL CHEMIN INSTRUMENT PROPOSAL SUBMITTED TO THE MSL MISSION ANNOUNCEMENT OF OPPORTUNITY AND HIS INCLUSION WAS VALIDATED AT THAT TIME BY DR. MICHAEL MEYER MARS PROGRAM SCIENTIST AT NASA HEADQUARTERS. IN THE INTERVAL BETWEEN CHEMIN'S SELECTION AS AN MSL PAYLOAD ELEMENT AND THE LAUNCH OFMSL (PHASES A-D OF THE INSTRUMENT PROJECT) DR. VANIMAN WAS SUPPORTED THROUGH CONTRACTS ADMINISTERED DIRECTLY FROM THE MARS PROGRAM OFFICE AT THE JET PROPULSION LABORATORY DURING WHICH TIME HE WAS MADE DEPUTY PI OF CHEMIN. IN THIS CAPACITY DAVID VANIMAN HAS HAD EQUAL AUTHORITY AND RESPONSIBILITY TO THE CHEMIN PI DR. DAVID BLAKE. DURING PHASE E OF THE INSTRUMENT PROJECT (MISSION OPERATIONS) VANIMAN'S ACTIVITIES HAVE BEEN SUPPORTED THROUGH COOP AGREEMENTS ADMINISTERED THROUGH AMES RESEARCH CENTER. IN 2017 THE DEPUTY PI WERE TRANSFERRED TO ELIZABETH RAMPE OFNASA-JSC AND VANIMAN TRANSITIONED TO CO-I STATUS; THIS TRANSITION WAS AGREED TO BY MICHAEL MEYER MARS PROGRAM SCIENTIST AT NASA HEADQUARTERS. THE DUTIES AND OBLIGATIONS OF CHEMIN CO-I'S FOR THE PRIME MISSION WERE DELINEATED IN THE CHEMIN EXPERIMENT OPERATIONS PLAN (JPL D-36918) "CHEMIN EOP" OR "EOP" AND PUBLICATIONS LISTED THEREIN. THESE DUTIES AND OBLIGATIONS HAVE WORKED WELL DURING THE PRIME MISSION AND THE FIRST AND SECOND EXTENDED MISSIONS AND WILL BE MAINTAINED INTO THE THIRD EXTENDED MISSION.

EXTENDED MISSION 4 SUPPORT FOR THE CHEMIN MINERALOGICAL INSTRUMENT ONBOARD MARS SCIENCE LABORATORY: EXPERIMENT PLANNING DATA ANALYSIS AND MISSION OPERATIONS

THE PLANETARY SCIENCE INSTITUTE (PSI) WITH OUR PARTNER THE TUCSON REGIONAL SCIENCE CENTER (RSC) PROPOSES TO: 1) OFFER A SERIES OF PROFESSIONAL DEVE

WE WILL OBSERVE 38 UHJS USING THREE SITES IN THE NORTHERN AND SOUTHERN HEMISPHERE USING MOSTLY MODERATE-APERTURE ROBOTICIZED TELESCOPES TO ACQUIRE HUNDREDS OF TRANSITS WITH MIDTIMES ACCURATE TO 1-2 MINUTES. WE WILL UPDATE THE TRANSIT EPHEMERIDES

SULFATES ARE A COMMON MINERAL IDENTIFIED FROM ORBITAL REMOTE SENSING DATA OF MARS WITH SEVERAL LOCATIONS HAVING LARGE DEPOSITS SUCH AS MERIDIANI PLANUM VALLES MARINERIS AND THE CENTRAL MOUND IN GALE CRATER (AEOLIS MONS). THE GALE SULFATES LIE ABOVE A PHYLLOSILICATE UNIT AND BELOW A SPECTRALLY BLAND POSSIBLE AEOLIAN DEPOSIT. BOTH MONOHYDRATED AND POLYHYDRATED SULFATES HAVE BEEN IDENTIFIED WITHIN AEOLIS MONS. ADDITIONALLY A DARK-TONED MARKER BED IS OBSERVED WITHIN THE SULFATES AT GALE BUT ITS EXTENT AND ORIGIN ARE UNKNOWN. IN PREPARATION FOR THE SULFATE INVESTIGATION BY THE CURIOSITY ROVER WE INTEND TO PERFORM A DETAILED STUDY OF THE SULFATES ACROSS AEOLIS MONS USING ORBITAL REMOTE SENSING DATA SETS. FOR THIS PROJECT WE HAVE OUTLINED SEVERAL TASKS THAT WILL CHARACTERIZE AND INTERPRET THE SULFATES AND MARKER BED WITHIN AEOLIS MONS TO PROVIDE ADDITIONAL INSIGHTS INTO THE GEOLOGIC HISTORY OF GALE CRATER AND THE FORMATION OF SULFATES ON MARS. TASK 1 WILL USE CRISM IMAGES TO DETERMINE THE COMPOSITION OF THE SULFATES IN PARTICULAR DISTINGUISHING BETWEEN MONOHYDRATED AND POLYHYDRATED SULFATES AS WELL AS OTHER MINERALS MIXED WITH THE SULFATES. THESE CRISM IMAGES COMBINED WITH VISIBLE IMAGES FROM HIRISE CTX AND HRSC IMAGES WILL BE USED FOR GEOLOGIC MAPPING OF THE SULFATES AND MARKER BED ACROSS THE ENTIRE MOUND EXTENDING THE MAPPING CURRENTLY BEING PERFORMED AT 1:60 000 SCALE OF WESTERN AEOLIS MONS BY CO-I THOMSON. TASK 2 WILL PRODUCE 8 NEW HIRISE-DERIVED DIGITAL TERRAIN MODELS (DTMS) AND THEN MEASURE BEDDING ORIENTATION AND THICKNESS OF THE SULFATES AND MARKER BED FROM THESE DTMS. WE WILL CREATE DETAILED STRATIGRAPHIC SECTIONS AT APPROXIMATELY 8-12 LOCATIONS ACROSS AEOLIS MONS THAT ENCOMPASS THE SULFATES AND THE MARKER BED. THE RESULTS WILL ENHANCE OUR UNDERSTANDING OF THE VERTICAL AND LATERAL VARIABILITY OF THE SULFATES AND DETERMINE IF THE SULFATES THAT WILL BE EXPLORED BY THE CURIOSITY ROVER ARE REPRESENTATIVE OF ALL THE SULFATES SEEN FROM ORBIT ACROSS AEOLIS MONS. FOR THE MARKER BED WE WILL UTILIZE THE DTMS TO DETERMINE IF THE BED ALWAYS OCCURS BETWEEN THE SAME SULFATE LAYERS MEASURE ITS ELEVATION AND THICKNESS ACROSS AEOLIS MONS AND LOOK FOR VARIATIONS IN SLOPE AND DIP OF THE BED. WE WILL THEN USE THESE MEASUREMENTS TO SUGGEST THE MOST PLAUSIBLE FORMATION MECHANISM(S) FOR THE MARKER BED AS WELL AS IDENTIFY THE KEY QUESTIONS ABOUT THE MARKER BED THAT COULD BE ADDRESSED BY THE MSL ROVER INSTRUMENTS AS PART OF TASK 4. TASK 3 WILL COMPARE OUR RESULTS FROM THE GALE SULFATES TO OTHER SULFATES FOUND ON MARS ESPECIALLY THOSE IN MERIDIANI PLANUM AND VALLES MARINERIS WHERE TEAM MEMBERS HAVE ALREADY CONDUCTED PREVIOUS ANALYSES. THE GOAL IS TO LEARN IF THE GALE SULFATES ARE SIMILAR IN THEIR COMPOSITION AND MORPHOLOGY TO OTHER MARTIAN SULFATE DEPOSITS. FORMATION SCENARIOS FOR THE SULFATES WITHIN THE GALE MOUND WILL BE INVESTIGATED IN RELATION TO OTHERS ON MARS USING PREVIOUSLY PUBLISHED CHEMICAL MODELING AND LABORATORY STUDIES OF SULFATE DEPOSITION. TASK 4 WILL LOOK SPECIFICALLY AT ORBITAL DATA OF THE SULFATES THAT ARE LIKELY TO BE TRAVERSED BY THE CURIOSITY ROVER IN ORDER TO RELAY OUR FINDINGS FROM THIS INVESTIGATION AND PROVIDE KEY QUESTIONS TO THE MSL SCIENCE TEAM THAT COULD BE INVESTIGATED BY THE ROVER ONCE IT REACHES THE SULFATES AND MARKER BED BASED UPON OUR RESULTS FROM TASKS 1-3. THIS PROPOSAL IS RELEVANT TO MDAP BECAUSE IT ADDRESSES THE MDAP GOAL TO ENHANCE THE SCIENTIFIC RETURN FROM MISSIONS TO MARS CONDUCTED BY NASA AND OTHER SPACE AGENCIES BY USING MULTIPLE MARTIAN DATA SETS FROM FOUR SEPARATE ORBITAL MISSIONS (MGS ODY MEX AND MRO) AND WILL CONTRIBUTE TO ONGOING GEOLOGIC ANALYSES OF THE SURFACE OF MARS WITH A FOCUS ON SULFATE DEPOSITS AT GALE CRATER.

COLLABORATIVE RESEARCH: GLOBAL EDDY-DRIVEN TRANSPORT ESTIMATED FROM IN SITU LAGRANGIAN OBSERVATIONS

THE PROPOSED ANALYSES HAVE THE POTENTIAL TO BROADEN OUR UNDERSTANDING OF BOTH PRE-AND POST-ERUPTIVE OXIDATIVE AND REDUCTIVE CONDITIONS IN LUNAR IGNEOUS MATERIALS AND THE LUNAR INTERIOR. THEY OVERCOME A LIMITATION OF CURRENT REDOX STUDIES IN LUNAR GLASSES MANY OF WHICH HAVE BEEN STORED IN TERRESTRIAL AIR SUBSEQUENT TO THEIR RETURN TO EARTH. IT IS KNOWN THAT REDOX STATES IN GLASSES CAN BE HIGHLY REACTIVE. THUS TO TRULY UNDERSTAND THE FO2 EVOLUTION OF THE LUNAR INTERIOR IT IS CRITICAL TO COMPARE PRISTINE LUNAR SAMPLES TO PREVIOUSLY-STUDIED ONES THAT HAVE HAD LENGTHY EXPOSURES TO EARTH S OXYGEN-RICH ATMOSPHERE.

EXPLORING KEY SOLAR SYSTEM EVOLUTION PROCESSES BY DEBIASING THE MAIN ASTEROID BELT

PSI ASTEROID/DUST SUBNODE OF THE NASA ' S PDS SMALL BODIES NODEIN THIS PROPOSAL WE DISCUSS THE GENER

PLANETARY SCIENCE INSTITUTE IMPACTS AND ENVIRONMENTAL CATASTROPHES: INVESTIGATING THE EFFECTS OF IMPACT EVENTS ON THE CLIMATE SYSTEM AN ENVIRONMENTAL

THE OBJECTIVES OF THE PROPOSED RESEARCH ARE RELEVANT TO NASA S SOLAR SYSTEM WORKINGS PROGRAM WHICH SUPPORTS RESEARCH INTO THE GEOLOGIC PROCESSES OCCURRING ON PLANETARY BODIES AND SEEKS TO ADDRESS THE PHYSICAL AND CHEMICAL PROCESSES.

THE GENESIS MISSION COLLECTED SOLAR WIND AND BROUGHT IT BACK TO EARTH IN ORDER TO PROVIDE PRECISE KNOWLEDGE OF SOLAR ISOTOPIC AND ELEMENTAL COMPOSITI

THE DAWN MISSION TO THE MINOR PLANET CERES (DIAMETER 950 KM) BEGAN IN 2014 AFTER ITS SUCCESSFUL MISSION TO VESTA. DAWN ACQUIRED IMAGE SPECTRAL AND TOPOGRAPHIC DATA DURING ITS APPROACH TO CERES (LATE 2014) THROUGH TWO EXTENDED MISSIONS UNTIL THE DAWN MISSION CONCLUDED IN NOVEMBER 2018. GLOBAL GEOLOGIC MAPPING OF CERES BEGAN WITH FRAMING CAMERA IMAGES ACQUIRED DURING THE APPROACH AND SURVEY PHASES OF THE MISSION. DATA ACQUIRED DURING THE HIGH ALTITUDE MAPPING ORBIT (HAMO) PROVIDED A SECOND ITERATION OF THE GLOBAL GEOLOGIC MAP OF CERES TO BE GENERATED AT A SPATIAL RESOLUTION OF 140 M/PIXEL. ACQUISITION OF LOW ALTITUDE MAPPING ORBIT (LAMO) PERMITTED CERES TO BE DIVIDED INTO 15 QUADRANGLES FOR HIGHER RESOLUTION GEOLOGIC MAPPING (35 M/PIXEL). LASTLY FOLLOWING DAWN S NOMINAL MISSION TO CERES TWO EXTENDED MISSIONS WERE APPROVED AND ADDITIONAL DATA AT VARIOUS ALTITUDES (AND RESULTING RESOLUTIONS) WERE ACQUIRED (XM01-XM07) BUT NOT INCORPORATED INTO ANY GLOBAL GEOLOGIC MAPPING PRODUCTS. THIS PROPOSED WORK WILL UTILIZE DAWN FRAMING CAMERA (FC) IMAGES VISIBLE AND INFRARED (VIR) MAPPING SPECTROMETER MULTISPECTRAL DATA GAMMA RAY AND NEUTRON DETECTOR (GRAND) DATA AND DERIVED TOPOGRAPHIC DATA TO CONSTRUCT A REVISED GLOBAL GEOLOGIC MAP OF CERES BASED ON SYSTEMATIC ANALYSIS OF THE COMPLETE DAWN MISSION DATASETS. THIS PROPOSED GEOLOGIC MAP OF CERES WILL BE PUBLISHED AS A U.S. GEOLOGICAL SURVEY (USGS) SPECIAL INVESTIGATION MAP (SIM) AT 1:3M (EQUATORIAL) AND 1:1.5M (POLAR). THIS INVESTIGATION SUPPORTS THE SCIENCE RETURN OF THE DAWN MISSION AND GENERATES A USEFUL DIGITAL GEOLOGIC MAP PRODUCT FOR THE COMMUNITY. WE PROPOSE THREE MAIN RESEARCH TASKS: (1) CONDUCT GEOLOGIC MAPPING. WE WILL PRODUCE A GLOBAL GEOLOGIC MAP OF CERES BUILDING ON PREVIOUS GEOLOGIC MAPS OF CERES AT VARIOUS SCALES. (2) DETERMINE RELATIVE AGES AND STRATIGRAPHY OF MAPPED UNITS AND FEATURES VIA ANALYSIS OF CRATER SIZE-FREQUENCY DISTRIBUTION STATISTICS AND STRATIGRAPHIC RELATIONS (E.G. SUPERPOSITION CROSS-CUTTING). (3) UPDATE CERES CHRONOSTRATIGRAPHY AND GEOLOGIC TIME SCALE (AS NECESSARY). WE PROPOSE TO EVALUATE THE GLOBAL GEOLOGY OF CERES WHERE IMPORTANT SPATIAL AND TEMPORAL RELATIONSHIPS BETWEEN GEOLOGIC MATERIALS AND PROCESSES ARE PRESERVED. IDENTIFYING AND MODELING SURFACE PROCESSES REQUIRES A COMPLETE CHARACTERIZATION AND STRATIGRAPHIC ANALYSIS OF THE RESULTING GEOLOGIC UNITS. WE WILL CONSTRUCT A GLOBAL GEOLOGIC MAP OF THE SURFACE OF CERES TO ADDRESS OUTSTANDING SCIENCE QUESTIONS REGARDING THE NATURE AND STRATIGRAPHY OF ITS IMPACT RECORD AND OTHER PAST GEOLOGIC ACTIVITY. THE OBJECTIVES OF THIS PROPOSAL ARE DIRECTLY RELEVANT TO NASA S DDAP SOLICITATION. THEY WILL ENHANCE THE SCIENTIFIC RETURN OF DISCOVERY PROGRAM MISSIONS AND BROADEN THE SCIENTIFIC PARTICIPATION IN THE ANALYSIS OF DATA COLLECTED BY DISCOVERY MISSIONS. THE RESULTING GEOLOGIC MAP WILL ASSIST IN EVALUATING THE EVOLUTION OF CERES BY COMPLEMENTING THE SCIENCE PRODUCTS PRODUCED BY THE FC VIR AND GRAND TEAMS. OUR TEAM INCLUDES PREVIOUSLY FUNDED MEMBERS OF THE DAWN MISSION AND THE DAWN AT CERES PARTICIPATING SCIENTIST (DAVPS) INVESTIGATION WHO WERE RESPONSIBLE EITHER FOR THE GLOBAL GEOLOGIC MAPPING OF CERES GEOLOGIC MAPPING AT THE LAMO QUAD SCALE AND/OR PROVIDED INSTRUMENT AND DATA SUPPORT. ALSO TEAM MEMBERS HAVE STRONG BACKGROUNDS IN MAPPING THE GEOLOGY OF ROCKY AND ICY PLANETARY BODIES DATA PROCESSING AND/OR ANALYSIS AND EACH MEMBER BRINGS A SPECIFIC SET OF DATA ANALYSIS SKILLS AND GEOLOGIC EXPERTISE THAT WILL ENABLE US TO MAP CERES AND ACCOMPLISH THE SCIENTIFIC OBJECTIVES PROPOSED IN THIS INVESTIGATION.

THE OBJECTIVE IS TO ARCHIVE ALL AVAILABLE IMAGES OBTAINED WITH THE LOWELL OBSERVATORY NEAR EARTH OBJECT SURVEY (LONEOS) TELESCOPE INTO THE SMALL BODIES NODE OF THE PLANETARY DATA SYSTEM (PDS-SBN).

EO14042 3-D SUBSURFACE IMAGING AND ANALYSIS OF GLACIERS AND LAVA FIELDS WITH SHARAD DATA

WE PROPOSE TO DEVELOP A WEB-BASED PLANETARY ORBITAL RADAR PROCESSING AND SIMULATION SYSTEM (PORPASS) BUILT AROUND A NEW GENERALIZED RADAR SOUNDER PROCESSOR (GRASP) AND A NEW 3D ORBITAL RADAR SIMULATOR (OARS).

THE PRIMARY OBJECTIVE OF THIS WORK IS TO PRODUCE A USGS GEOLOGIC MAP AT 1:1 000 000 SCALE FROM 18.5 DEGREES W TO 9.5 DEGREES E AND 0 DEGREES N TO 16 DEGREES N WHICH INCLUDES THE PYROCLASTIC DARK MANTLE DEPOSITS (DMDS) IN SINUS AESTUUM RIMA BODE AND MARE VAPORUM. IN THIS NEW INVESTIGATION WE WILL USE MULTIPLE DATA SETS TO BETTER REFINE THE EXTENT OF PYROCLASTICS FOR THESE THREE DMDS MAP AND DETERMINE THE COMPOSITIONS OF THE MARE AND HIGHLANDS WITHIN OUR STUDY REGION PERFORM CRATER COUNTING TO ESTABLISH AGES EXPLORE THE GEOLOGIC SETTING AND HISTORY OF THE MAPPING REGION IDENTIFY AND MEASURE THE DIMENSIONS OF PLAUSIBLE SOURCE VENTS FOR THE DMDS AND ATTEMPT TO CHARACTERIZE THE ERUPTION(S) THAT EMPLACED EACH DMD. AN IMPROVED UNDERSTANDING OF THE DISTRIBUTION GEOLOGIC SETTING AND ERUPTIONS CONDITIONS THAT PRODUCED THE PYROCLASTIC DEPOSITS GAINED THROUGH STRATIGRAPHIC MORPHOLOGIC AND MINERALOGIC CHARACTERIZATION HAS THE POTENTIAL TO REVEAL IMPORTANT INFORMATION ABOUT THE THERMAL AND VOLCANIC HISTORY OF THE MOON. THERE ARE TWO TASKS FOR THIS INVESTIGATION: TASK 1: PRODUCE A U.S. GEOLOGICAL SURVEY (USGS) MAP AT 1:1 000 000 SCALE COVERING THE STUDY REGION THAT ENCOMPASSES THE THREE DMDS OF SINUS AESTUUM RIMA BODE AND MARE VAPORUM. THE GOAL OF TASK 1 IS TO MAP THE EXTENT AND DISTRIBUTION OF THE PYROCLASTIC DEPOSITS WITHIN EACH DMD THAT IS NEEDED FOR TASK 2. WE WILL ALSO MAP MARE AND HIGHLAND UNITS BASED UPON MORPHOLOGY TOPOGRAPHY AND COMPOSITION IDENTIFY AND MAP LINEAR FEATURES AND PERFORM CRATER COUNTING FOR AGE ASSESSMENT. TASK 2: BASED UPON THE MAPPING OF IRREGULAR CRATERS AND LINEAR FEATURES AS WELL AS THE AERIAL EXTENT OF THE DMDS IN TASK 1 WE WILL IDENTIFY PLAUSIBLE SOURCE VENTS AND CHARACTERIZE THE ERUPTIONS THAT EMPLACED THE DMDS. RESULTS INCLUDE CONSTRAINING THE STYLE OF VOLCANIC ERUPTION (UMBRELLA PLUME VS. FIRE FOUNTAIN) AND THE RELATIONSHIP BETWEEN VENT PHYSICAL PROPERTIES AND DMD EXTENT.

IN THIS STUDY WE PROPOSE TO INVESTIGATE THE GENERATION REDISTRIBUTION AND MIXING OF REGOLITH ON THE MOON AND TO MAKE DIRECT COMPARISONS BETWEEN MODEL SIMULATIONS SPACECRAFT OBSERVATIONS LUNAR SAMPLES AND METEORITES TO BETTER UNDERSTAND THE SURFACE PROCESSES AND TIMESCALES INVOLVED ON A WIDE RANGE OF IMPACT-DOMINATED PLANETARY SURFACES. THE BASIC PROBLEM THAT WE WISH TO ADDRESS IS: WHAT IS THE DISTRIBUTION OF MATERIAL IN THE UPPERMOST LAYERS OF LUNAR REGOLITH THAT HAS BEEN ISOTOPICALLY RESET BY INDIVIDUAL IMPACTS? THE PROPOSED WORK WOULD DEVELOP A FULLY THREE-DIMENSIONAL REGOLITH/MEGAREGOLITH EVOLUTION MODEL WHICH LEVERAGES TWO EXISTING WELLTESTED AND PUBLISHED MODELS: (I) CRATERED TERRAIN EVOLUTION MODEL (CTEM) [RICHARDSON 2009] WHICH NOW INCLUDES DEPOSITION OF PROXIMAL AND DISTAL EJECTA [HUANG ET AL. 2017]; AND (II) A TWO-DIMENSIONAL MODEL OF IMPACT-INDUCED HEATING OF THE CRUST AND IMPACTINDUCED AGE-RESETTING [ABRAMOV ET AL. 2013]. THE PROPOSED COMBINED MODEL WOULD TRACK AGES OF IMPACT MELTS IN SEVERAL ISOTOPIC SYSTEMS AND PREDICT IMPACT MELT AGE DISTRIBUTIONS AS A FUNCTION OF DEPTH. THE MODEL OUTPUT WOULD THEN BE STATISTICALLY COMPARED TO MELT AGES IN LUNAR METEORITES WHICH REPRESENT A FAIRLY RANDOM SAMPLING OF THE UPPER REGOLITH. THROUGH THIS COMPARISON AN ASSESSMENT OF SEVERAL PROPOSED SCENARIOS OF EARLY LUNAR BOMBARDMENT HISTORY WILL BE PERFORMED. IN TASK I A LIBRARY OF EJECTA VOLUMES TEMPERATURE DISTRIBUTIONS AND MEAN MELT FRACTIONS FOR EJECTA BLANKETS ASSOCIATED WITH A BROAD RANGE OF IMPACTORS IN THE 1-200 KM RANGE WILL BE CREATED. IN TASK II AN EXISTING ONE-DIMENSIONAL MODEL OF AGE-RESETTING WITHIN COOLING IMPACT EJECTA BLANKETS WOULD BE USED TO CREATE A LIBRARY OF THE DEGREE OF AGE-RESETTING IN THE DEPTH-TEMPERATURE PARAMETER SPACE. IN TASK III THE REGOLITH AGE-RESETTING MODEL WOULD BE RUN FOR SEVERAL BOMBARDMENT SCENARIOS INCLUDING A POST-ACCRETIONARY EXPONENTIAL DECLINE AS WELL AS "SPIKE-" AND "SAWTOOTH-" TYPE LATE BOMBARDMENTS. IN TASK IV THE RESULTS OF THE REGOLITH MODEL WILL BE COMPARED TO RECORDED MELT AGES IN LUNAR METEORITES USING STATISTICAL METHODS. THE PROPOSED RESEARCH IS DIRECTLY RELEVANT TO THE SOLAR SYSTEM WORKINGS (SSW) PROGRAM WHICH SEEKS TO "ADDRESS THE PHYSICAL AND CHEMICAL PROCESSES THAT AFFECT THE SURFACES ... OF PLANETARY BODIES." THEORETICAL INVESTIGATIONS THAT INCLUDE "DATA SYNTHESIS RELEVANT TO THE PHYSICAL AND CHEMICAL PROCESSES AFFECTING PLANETARY SYSTEMS" ARE ENCOURAGED BY SSW AND PROCESSES THAT RESULT IN "EVOLUTION AND MODIFICATION OF SURFACES" SUCH AS IMPACT CRATERING ARE SPECIFICALLY HIGHLIGHTED. THE PROPOSED INVESTIGATION DOES NOT HAVE A SIGNIFICANT DATA ANALYSIS COMPONENT AND IS THUS MORE APPROPRIATE FOR SSW THAN LUNAR DATA ANALYSIS PROGRAM. THIS PROPOSAL DIRECTLY ADDRESSES THE HIGHEST LUNAR SCIENCE PRIORITIES IDENTIFIED BY THE NATIONAL RESEARCH COUNCIL (NRC) AS WELL AS THE GUIDING THEMES AND OBJECTIVES IN THE SOLAR SYSTEM EXPLORATION ROADMAP AND THE NASA STRATEGIC PLAN.

A FRESH EXAMINATION OF THE MOON'S YOUNG CRATERS: INSIGHTS FROM NEW DATASETS AND ANALYSIS TOOLS

SIMULATION OF SPACE WEATHERING EFFECTS ON THE MOONTHE GOAL OF THE PROPOSED EFFORT IS THE ANALYTIC

ENHANCED THERMOPHYSICAL ANALYSIS TOOLS FOR MARS RESEARCH

DIVERSITY AND INCLUSIVENESS ALONG GENDER ETHNICITY ABILITY SEXUAL ORIENTATION GENERATIONAL AND OTHER AXES IS A BUSINESS AS WELL AS A SOCIAL IMPERATIVE. IT LEADS TO INNOVATION AND PROTECTS AGAINST GROUPTHINK AND STAGNATION. SOCIAL SCIENCE RESEARCH SHOWS THAT INTELLECTUAL CROSS-FERTILIZATION IS AN IMPORTANT SOURCE OF INNOVATION AND NEW IDEAS AND THAT DIVERSE GROUPS COME UP WITH BETTER IDEAS AND SOLUTIONS TO PROBLEMS. THIS IS PARTICULARLY IMPORTANT FOR SCIENCE WHERE WE ARE PUSHING BACK THE FRONTIERS OF HUMAN KNOWLEDGE AND ANSWERING NEW AND UNIQUE QUESTIONS. FURTHERMORE DIVERSITY WITHIN A TEAM GIVES GREATER ABILITY TO REACH NEW GROUPS FOR OUTREACH AND SUPPORT SO A MORE DIVERSE WORKFORCE ENABLES INTERESTING A MORE DIVERSE POPULATION. WHILE ONE OF NASA S 3 MAIN STRATEGIC GOALS INVOLVES SERVING THE AMERICAN PUBLIC THE CURRENT PLANETARY SCIENCE WORKFORCE IS NOT NEARLY AS DIVERSE AS THE U.S. POPULATION. THE PLANETARY SCIENCE WORKFORCE IS 25% WOMEN AND 87% WHITE COMPARED TO THE POPULATION WHICH IS 50% WOMEN AND 64% WHITE. RECENT STUDIES INTO THE COMPOSITION OF ROBOTIC NASA SPACECRAFT MISSIONS DEMONSTRATES THAT WOMEN ARE FURTHER UNDERREPRESENTED ON THOSE SCIENCE TEAMS. NASA S 2014 STRATEGIC PLAN FURTHER STATES THAT NASA S MOST POWERFUL ASSET IS A MULTI-DISCIPLINARY TEAM OF DIVERSE COMPETENT PEOPLE. THE WORK PROPOSED HERE WILL HELP NASA S PLANETARY SCIENCE WORKFORCE TO BECOME MORE DIVERSE AND EQUITABLE. THE GOAL OF THIS PROJECT IS TO QUANTIFY TRENDS IN DIVERSITY WITHIN THE NASA PLANETARY MISSION AND RESEARCH PORTFOLIO AND EXECUTE STRATEGIES TO ENRICH THAT DIVERSITY IN THE NEAR FUTURE. SUCCESSFUL STRATEGIES MUST ADDRESS ANY BARRIERS HINDERING STRONG DIVERSITY IN NASA S PLANETARY SCIENCE PORTFOLIO. TO ACCOMPLISH THIS GOAL WE PROPOSE THREE MAIN TASKS: 1. EXPAND DEMOGRAPHIC STUDIES OF WOMEN AND OTHER UNDERREPRESENTED GROUPS IN MEASURES OF SUCCESS SUCH AS SELECTION ON SPACECRAFT MISSION TEAMS AND R&A PROPOSALS; 2. CONDUCT A NEW SURVEY OF THE PLANETARY SCIENCE WORKFORCE IMPROVING UPON THE 2011 STUDY; 3.WORK WITH SOCIAL SCIENTISTS TO DETERMINE POSSIBLE POLICY CHANGES THAT CAN INCREASE PARTICIPATION OF WOMEN AND OTHER UNDERREPRESENTED GROUPS IN PLANETARY SCIENCE.

ASSESSING THE PRESERVATION OF FLUVIAL PATHWAYS IN THE TERRESTRIAL GEOLOGIC RECORD: ANALOGS FOR THE INVESTIGATION OF MARTIAN RAISED CHANNELSCONSTRAIN

OBJECTIVES: THE OBJECTIVE OF THIS PROPOSAL IS TO CHARACTERIZE THE SIMILARITIES AND DIFFERENCES IN THE REGOLITH PROPERTIES OF LUNAR SWIRLS. THESE SIMILARITIES AND DIFFERENCES CAN BE USED TO HELP DISTINGUISH BETWEEN THE THREE FORMATION MECHANISMS FOR LUNAR SWIRLS. LUNAR SWIRLS ARE SINUOUS HIGH- AND LOW-REFLECTANCE REGIONS ASSOCIATED WITH LOCALIZED MAGNETIC ANOMALIES [1 2]. THE THREE HYPOTHESIS EXPLAINING THEIR ORIGIN INCLUDE: (1) SHIELDING FROM SOLAR WIND IRRADIATION BY THE MAGNETIC ANOMALY WHICH IMPEDES ONE OF THE SPACE WEATHERING PROCESSES ACTIVE ON THE LUNAR SURFACE [3 4] (2) SORTING OF SOIL GRAINS THROUGH ELECTROMAGNETIC DUST LEVITATION WHICH WOULD PREFERENTIALLY ACCUMULATE FELDSPAR-RICH DUST [5] OR SMALL GRAINS WITH A LOWER COMPONENT OF NANOPHASE IRON [6] AND (3) FORMATION FROM COMETARY IMPACTS IN WHICH THE REMANENT MAGNETIC FIELD IS GENERATED BY THE IMPACT EVENT [7]. METHODS: EACH OF THE FORMATION PROCESSES WOULD PRODUCE DIFFERENT REGOLITH PROPERTIES. IN THE SHIELDING HYPOTHESIS THOSE REGIONS THAT ARE SHIELDED WOULD CONTAIN A LOWER QUANTITY OF NANOPHASE IRON THE GRAINS WOULD HAVE THINNER RADIATION-DAMAGE PRODUCED RIMS (AFFECTING SCATTERING PROPERTIES) AND THERE WOULD BE NO SIZE SORTING OF REGOLITH COMPONENTS. IN THE ELECTROMAGNETIC TRANSPORT HYPOTHESIS THERE WOULD BE A LOWER QUANTITY OF GRAINS WITH NANOPHASE IRON RADIATION-DAMAGED RIMS WOULD BE UBIQUITOUS BETWEEN THE HIGH- AND LOW-REFLECTANCE REGIONS AND THERE WOULD BE EVIDENCE OF SIZE SORTING WITH A LARGER COMPONENT OF FINE GRAINS. IN THE COMETARY IMPACT HYPOTHESIS THERE WOULD BE NO DIFFERENCE IN NANOPHASE IRON CONTENT RADIATION-DAMAGED RIMS WOULD BE UBIQUITOUS BETWEEN THE HIGH- AND LOW-REFLECTANCE REGIONS AND THERE WOULD BE NO EVIDENCE OF SIZE SORTING WITHIN THE REGOLITH. THESE REGOLITH PROPERTIES CAN BE CHARACTERIZED USING A COMBINATION OF PHOTOMETRIC AND SPECTROSCOPIC MODELING. USING HAPKE S MODEL THE DIFFERENCES IN THE SCATTERING PROPERTIES OF THE REGOLITH CAN BE QUANTIFIED [8 9]. SPECTRAL MIXING MODELS CAN IDENTIFY THE SIZE AND QUANTITY OF SUBMICROSCOPIC/ NANOPHASE COMPONENTS [10]. USING LUNAR SHAPE MODELS TO DERIVED INCIDENCE EMISSION AND PHASE ANGLES THAT ACCOUNT FOR TOPOGRAPHY LUNAR RECONNAISSANCE ORBITER (LRO) COLOR IMAGES AND MOON MINERALOGY MAPPER (M3) WE WILL APPLY HAPKE S MODEL TO CHARACTERIZE THE SCATTERING PROPERTIES OF THE VARIOUS COMPONENTS OF THE SWIRL REGIONS. USING SPECTRAL MIXING MODELS WE WILL EXAMINE THE QUANTITY SIZE AND COMPOSITION OF THE REGOLITH CONSTITUENTS. WE WILL USE THESE METHODS TO CHARACTERIZE AND MAP SIMILARITIES AND DIFFERENCES BETWEEN VARIOUS SWIRL REGIONS ACROSS THE LUNAR SURFACE.

THE RECIPIENT SEEKS TO DERIVE FROM LOLA DATA LUNAR SURFACE SLOPES AND ROUGHNESS AS A FUNCTION OF SCALE, AND TO STUDY THE INFLUENCE OF THESE MEASUREME

OPTICAL CONSTANTS ARE FUNDAMENTAL INPUT PARAMETERS IN RADIATIVE TRANSFER AND LIGHT SCATTERING CODES USED FOR THE QUANTITATIVE ANALYSIS OF PLANETARY SPECTRAL REMOTE SENSING DATA. THEY ARE NEEDED TO DIRECTLY MODEL HOW LIGHT INTERACTS WITH PARTICULATE S

LABORATORY CHARACTERIZATION OF THE DIFFUSIVE PROPERTIES OF ANALOG SOLAR SYSTEM REGOLITH MATERIALS

PLUTO AND TRITON ARE STRIKINGLY SIMILAR BODIES IN THE OUTER SOLAR SYSTEM WITH COMPARABLE SIZES DENSITIES AND COMPOSITIONS. THEY BOTH CAN BE CONSIDERED LINKS TO EARLY CONDITIONS IN THE OUTER SOLAR SYSTEM WITH TRITON LIKELY TO HAVE ORIGINATED IN

EO14042 ANALYSES OF SULFATES IN CHAOS REGIONS ON MARS

MERCURY, THE PLANET CLOSEST TO THE SUN, IS ONE OF THE LEAST-STUDIED BODIES IN THE SOLAR SYSTEM. THE MESSENGER SPACECRAFT, EN ROUTE TO MERCURY NOW, CO

GEOLOGIC MAP OF SOUTHERN CIRCUM-CHRYSE AND MARGARITIFER TERRA MARS

SPECTROPHOTOMETRIC MODELING OF SPECTROMETER AND IMAGER OBSERVATIONS OBJECTIVES THE OBJECTIVE OF THIS PROPOSAL IS TO FACILITATE MAPPING MINERAL PROPER

WE PROPOSE TO DEVELOP A DETAILED GEOLOGIC MAP AND ACCOMPANYING CHRONOSTRATIGRAPHY OF URVARA CRATER CERES BASED ON HIGH-RESOLUTION IMAGE DATA (3.5-20 M/PX) ACQUIRED AT THE END OF THE DAWN MISSION. CRATER DIAMETER: 170 KM.

CONSTRAINING SURFACE PROPERTIES OF ASTEROID 1999 JU3 USING HAYABUSA2 OPTICAL NAVIGATION CAMERA CLEAR AND COLOR IMAGES BACKGROUND: THE HAYABUSA2 SPACE

THE MOON MINERAL MAPPER (M3) DETECTED OH AND H2O ON THE SURFACE ON THE MOON DURING THE CHANDRAYAAN-1 MISSION. CALIBRATION ISSUES LIMITED THE SPECTROM

EXPLORING THE VOLCANIC HISTORY OF THE CRISIUM BASIN THROUGH GEOLOGIC MAPPING

COORDINATING THE LRO E/PO PROGRAM, MANAGING THE LRO E/PO TEAM, MANAGING THE LRO E/PO BUDGET, REPORTING TO AND COLLABORATING WITH THE LRO PROJECT SCIE

PHOTOMETRIC STUDY ON HOW THE SURFACE PHYSICAL PROPERTIES OF COMET 67P/CHURYUMOV-GERASIMENKO CHANGE WITH ITS PERIHELION PASSAGE COULD PROVIDE CLUES TOWARD UNDERSTANDING OF THE SURFACE EVOLUTION OF JUPITER FAMILY COMETS (JFCS).

23-SSW23-0109 INVESTIGATING THE ORIGINS AND TIMING OF SHALLOW MOONQUAKES

A REVISED GLOBAL GEOLOGIC MAP OF VESTA FROM DAWN IMAGE, SPECTRAL AND ELEMENTAL DATA WHAT CORRELATIONS EXIST BETWEEN MORPHOLOGY, TOPOGRAPHY, AND COMPO

SCIENCE GOALS AND OBJECTIVES. GLOBAL MAPS OF THE RELATIVE ABUNDANCE OF HYDROXYL OH AND WATER (HOH) (2.8 AND 3.0 UM BAND DEPTH RESPECTIVELY) OBTAINED FROM THE MOON MINERALOGY MAPPER (M3) SHOW VARIABILITY CORRELATED WITH LATITUDE LOCAL TIME OF DAY TEMPERATURE AND COMPOSITION SUGGESTING THAT THE SPECIFIC CONDITIONS AND SOIL CHARACTERISTICS FAVOR RETENTION OF OH AND HOH. OUR LONG TERM RESEARCH GOAL IS TO DETERMINE THOSE PROPERTIES OF THE LUNAR SOIL THAT FAVOR THE FORMATION AND RETENTION OF OH AND HOH. THIS DICTATES A PRELIMINARY GOAL OF IMPLEMENTING AN IMPROVED THERMAL EMISSION MODEL FOR M3 SPECTRAL REFLECTANCE DATA FOR THE LOCATIONS SELECTED TO CARRY OUT THIS RESEARCH. OUR PRELIMINARY RESULTS SUGGEST THAT SOIL MATURITY IS A KEY PROPERTY FAVORING RETENTION OF OH/HOH ALTHOUGH SOIL MATURITY IS NOT THE SOLE FACTOR AND THAT OTHER AS YET UNIDENTIFIED SOIL PROPERTIES ALSO AFFECT THE ABILITY OF THE SOIL TO RETAIN OH/HOH. OUR OBJECTIVE IN THE PROPOSED WORK IS TO IDENTIFY THE EXTENT TO WHICH MATURITY AND OTHER SOIL PROPERTIES INFLUENCE OH/HOH RETENTION AND WHAT THAT IMPLIES ABOUT HOW AND WHERE OH/HOH IS RETAINED IN THE MATERIAL. THIS LEADS US TO TWO TESTABLE HYPOTHESES FOR THE HOW THE SURFICAL OH/HOH IS FORMED AND RETAINED ON THE LUNAR SURFACE: (1) FRESHLY FRACTURED CRYSTALLINE MATERIALS (AS BY IMPACTS) PROVIDE DEFECT LATTICE SITES AND DANGLING BONDS PROVIDING AN ELECTROPOSITIVE SURFACE THAT WOULD ENHANCE ADSORPTION (CHEMISORPTION) OR (2) OH/ HOH IS TRAPPED WITHIN THE GLASSY PRODUCTS OF SPACE WEATHERING (I.E. AGGLUTINATES VAPOR-DEPOSITED AMORPHOUS RIMS ON SOIL PARTICLES. METHODOLOGY. TO TEST THESE HYPOTHESES WE WILL USE CLEMENTINE-DERIVED FEO AND TIO2 LRO WAC AND NAC FOR EOMORPHOLOGY AND DIVINER FOR MORPHOLOGY AND TO IMPROVE THE THERMAL MODEL FOR M3 DATA. THE ANALYTICAL PROCEDURE WILL FOCUS ON M3 SPECTRA TO CHARACTERIZE MINERALOGY AND THE RELATIVE CHANGES IN THE SHAPE AND DEPTH OF THE OH AND HOH ABSORPTION BANDS AS A FUNCTION OF: (A) LATITUDE (B) LUNAR TIME OF DAY (C) COMPOSITION (FEO AND TIO2 ABUNDANCE FROM CLEMENTINE; MINERALOGY FROM M3) (D) TEXTURE (E.G. GLASSY VERSUS CRYSTALLINE; MORPHOLOGICALLY FROM LRO WAC AND NAC AND SPECTRALLY FROM M3) AND (E) MATURITY (SPECTRAL CONTINUUM SLOPE RELATIVE MAFIC ABSORPTION BAND DEPTHS FROM M3). RELEVANCE. THE SUCCESSFUL COMPLETION OF THIS PROJECT CAN BE EXPECTED TO HAVE AN IMPORTANT POSITIVE IMPACT ON CURRENT UNDERSTANDING OF THE LUNAR WATER CYCLE THE PROPERTIES OF THE SOIL THAT INFLUENCE THIS PHENOMENON AND CAN SERVE AS A GUIDE FOR PATHS OF FUTURE EXPLORATION AND TECHNOLOGY DEVELOPMENT. AS SUCH THIS RESEARCH DIRECTLY ADDRESSES THE LDAP OBJECTIVES: (1) IDENTIFICATION AND/OR CHARACTERIZATION OF POTENTIAL LANDING SITES OF HIGH LUNAR SCIENCE RETURN (E.G. GEOMORPHOLOGY REGOLITH RADIATION AND COMPOSITIONAL PROPERTIES) (2) IDENTIFICATION DISTRIBUTION TRANSPORT AND CHARACTERIZATION OF VOLATILES IN AND ON THE MOON (3) LUNAR "CHANGE DETECTION" (I.E. DETECTION OF SURFACE OR ATMOSPHERIC CHANGES AS A FUNCTION OF TIME) AND (4) IDENTIFICATION/CHARACTERIZATION OF LUNAR MINERALOGY AS A FUNCTION OF LOCATION AND DEPTH. THE PROPOSED WORK WILL ALSO IMPROVE THE SCIENTIFIC RETURN OF LUNAR DATA THROUGH THE IMPROVEMENT IN THE THERMAL EMISSION REMOVAL FOR M3 DATA.

COLLABORATIVE RESEARCH: BUILDING AND APPLYING A UNIVERSAL PLAGIOCLASE OXYBAROMETER USING X-RAY ABSORPTION SPECTROSCOPY -THE PROJECT FOCUSES ON HOW VOLCANIC MAGMAS CHANGE AS THEY TRAVEL TOWARD THE SURFACE AND ERUPT. THE TEAM IS INTERESTED IN THE OXYGEN CONTENT OF MAGMA AS IT ASCENDS, AND THEY WILL USE THE MOST COMMON ROCK-FORMING MINERAL IN THE EARTH?S CRUST, FELDSPAR, TO STUDY THAT . THIS OXIDATION STATE OF A MAGMA IS IMPORTANT BECAUSE IT PLAYS A LARGE ROLE IN REGULATING THE STYLE OF THE ERUPTION AND HOW EXPLOSIVE IT IS. THE PROJECT WILL APPLY A NEW ANALYTICAL TECHNIQUE TO VOLCANIC PRODUCTS FROM MOUNTS SHASTA AND ST. HELENS TO GAIN A MORE THOROUGH UNDERSTANDING OF HOW THEIR MAGMAS HAVE CHANGED AS THEY ASCEND TO THE SURFACE BEFORE ERUPTION. THIS WORK COULD LEAD TO BETTER INDICES OF HAZARD ASSESSMENT IN ACTIVE VOLCANIC SYSTEMS. THIS PROJECT SUPPORTS A POSTDOCTORAL RESEARCHER WHO WILL BUILD THEIR EXPERTISE IN SPECTROSCOPIC MEASUREMENTS AND GAIN EXPERIENCE IN PROJECT LEADERSHIP. IT WILL ALSO PROVIDE UNDERGRADUATES VALUABLE EXPERIENCE WITH LABORATORY RESEARCH IN THE GEOSCIENCES. BOTH PIS HAVE DEDICATED MUCH OF THEIR CAREERS TO ENCOURAGING AND WORKING WITH STUDENTS FROM UNDERREPRESENTED GROUPS IN THE STEM FIELDS TO GROW DIVERSITY OF SCIENTIFIC THOUGHTS AND BACKGROUNDS AND OPPORTUNITIES FOR ALL. THE PROJECT WILL ENABLE IN SITU MEASUREMENTS OF FELDSPAR CHEMISTRY AND FO2, USING A LARGE DIVERSE CALIBRATION SUITE OF >180 SAMPLES. IT WILL THEN USE THE RESULTANT XAS CALIBRATIONS TO EXAMINE PARTITIONING OF FE3+ AND VARIATIONS IN FO2 IN THREE NATURAL SYSTEMS: THE BUSHVELD COMPLEX, MOUNT SHASTA, AND MOUNT ST. HELENS. IT WILL RESULT IN NEW GEOCHEMICAL CALIBRATIONS AVAILABLE TO THE GEOLOGIC COMMUNITY AND NEW INSIGHTS INTO THE ROLE PLAYED BY FELDSPAR IN PARTITIONING CATIONS WITH COEXISTING MELTS. SPECIFICALLY, THIS PROJECT INCLUDES TASKS THAT WILL ENABLE FE VALENCE STATE AND FO2 TO BE EVALUATED DIRECTLY FROM FELDSPAR SINGLE CRYSTALS USING XAS, AND WILL BE COMPLEMENTED BY OTHER TYPES OF SPECTROSCOPIC MEASUREMENTS: 1) GROW LIQUIDUS FELDSPARS OVER A RANGE OF BULK COMPOSITIONS, FO2, AND TEMPERATURE TO BE USED AS STANDARDS FOR AN XAS FO2 CALIBRATION; 2) CREATE A FELDSPAR CALIBRATION FOR MICROANALYSIS OF FE3+ IN FELDSPAR USING POLARIZED, HIGH-RESOLUTION XAS MEASUREMENTS OF INDEPENDENTLY CONSTRAINED STANDARDS USING THE PRE-EDGE AND MAIN-EDGE REGIONS OF ORIENTED SINGLE CRYSTALS; 3) USE THE EQUILIBRATED FELDSPARS WITH KNOWN FO2 TO CREATE A FELDSPAR CALIBRATION FOR FO2 USING POLARIZED, HIGH-RESOLUTION XAS; 4) TEST AND APPLY OUR FELDSPAR CALIBRATION FOR FO2 ON BUSHVELD, SHASTA, AND MOUNT ST. HELENS SAMPLES; 5) WITH UNDERGRADUATE RESEARCHERS LEADING THE WORK, CHARACTERIZE THE SAME SUITE OF SAMPLES ASSEMBLED FOR THE OXYBAROMETERS USING RAMAN, M?SSBAUER, ULTRAVIOLET (UV), VISIBLE (VIS), ATTENUATED TOTAL REFLECTANCE (ATR) AND REFLECTANCE FTIR SPECTROSCOPIES, LOOKING FOR LINKAGES BETWEEN COMPOSITION AND SPECTRAL RESPONSE. THIS AWARD REFLECTS NSF'S STATUTORY MISSION AND HAS BEEN DEEMED WORTHY OF SUPPORT THROUGH EVALUATION USING THE FOUNDATION'S INTELLECTUAL MERIT AND BROADER IMPACTS REVIEW CRITERIA.

"IN-SITU STUDIES OF TERRESTRIAL DUST DEVILS AND AMBIENT METEOROLOGY: APPLICATION TO MARS' CLIMATE"DUST DEVILS ARE SMALL-SCALE PARTICLE-LOADED CONVE

STUDYING JUPITER'S MAGNETOSPHERIC RESPONSE TO IO'S VOLCANIC ACTIVITY

EXECUTE A BALANCED SCIENCE PROGRAM BASED ON DISCIPLINE-SPECIFIC GUIDANCE FROM THE NATIONAL ACADEMIES OF SCIENCES ENGINEERING AND MEDICINE ADMINISTRATION PRIORITIES AND DIRECTION FROM CONGRESS. PARTICIPATE AS A KEY PARTNER AND ENABLER IN THE AGENCY S EXPLORATION INITIATIVE FOCUSING ON SCIENTIFIC RESEARCH OF ON AND FROM THE MOON LUNAR ORBIT MARS AND BEYOND. ADVANCE DISCOVERY IN EMERGING FIELDS BY IDENTIFYING AND EXPLOITING CROSS-DISCIPLINARY OPPORTUNITIES BETWEEN TRADITIONAL SCIENCE DISCIPLINES DEVELOP A DIRECTORATE-WIDE TARGET-USER FOCUSED APPROACH TO APPLIED PROGRAMS INCLUDING EARTH SCIENCE APPLICATIONS SPACE WEATHER PLANETARY DEFENSE AND SPACE SITUATIONAL AWARENESS.

THE GENESIS MISSION COLLECTED SOLAR WIND AND BROUGHT IT BACK TO EARTH IN ORDER TO PROVIDE PRECISE KNOWLEDGE OF SOLAR ISOTOPIC AND ELEMENTAL COMPOSITI

WE WILL INVESTIGATE THE USE OF GALACTIC COSMIC RAY (GCR) SECONDARY PARTICLES TO PROBE THE DEEP INTERIORS OF SMALL SOLAR SYSTEM BODIES (SSBS), INCLUDI

SUCCESSOR AWARD TO COOPERATIVE AGREEMENT NNX11AO880 FOR SUPPORT FOR THE CHE MIN MINERALOGIACAL INSTURMENT DURING THE MARS SCIENCE LABORATORY (MSL*11) MISSIONCO-I TACTICAL ROLE CURRENTLY IS IN DATA ANALYSIS AND SUPPORT ON ANALOG STUDIES. CHEMIN SAMPLES THAT WERE COLLECTED AND ANALYZED DURING THIS REVIEW PERIOD INCLUDE THE GOBABEB DUNE SAND; THE OKORUSO SANDSTONE AND ITS SILICIFIED EQUIVALENT LUBANGO; THE OUDAM MUDSTONE; THE MARIMBA2 MUDSTONE; THE QUELA MUDSTONE; AND THE SEBINA MUDSTONE. RESEARCH ON THESE SAMPLES IS ONGOING AND PRELIMINARY PUBLICATIONS ARE IN PREPARATION. THE RATE OF SAMPLE COLLECTION FOR CHEMIN HAS ACCELERATED DURING THIS REVIEW PERIOD BY INSTITUTION OF MORE SYSTEMATIC SAMPLING AS THE ROVER ASCENDS MOUNT SHARP. PI HAS CONTINUED TO LEAD CHEMIN TEAM TELECONS ON A WEEKLY BASIS. THESE TELECONS PROVIDE THE MEANS FOR THE TEAM TO COMMUNICATE SHORT-TERM ISSUES AND RESULTS. FOR EACH MEETING NOTES ARE COMPILED AND DISTRIBUTED BY PI TO KEEP A RECORD OF CHEMIN TEAM PLANNING AND ACTIVITIES. PI ALSO PARTICIPATED IN MSL TEAM MEETINGS AT THE CALIFORNIA INSTITUTE OF TECHNOLOGY (APRIL 5-7 2016) AS WELL AS A CHEMIN TEAM MEETING AT THE 2016 LUNAR AND PLANETARY SCIENCE CONFERENCE.

HISTORICAL EXTENT OF MARS' SOUTH POLAR MASSIVE CO2 ICE DEPOSIT

EXECUTE A BALANCED SCIENCE PROGRAM BASED ON DISCIPLINE-SPECIFIC GUIDANCE FROM THE NATIONAL ACADEMIES OF SCIENCES ENGINEERING AND MEDICINE ADMINISTRATION PRIORITIES AND DIRECTION FROM CONGRESS. PARTICIPATE AS A KEY PARTNER AND ENABLER IN THE AGE

A MAJOR GOAL IN COSMOCHEMISTRY IS TO UNDERSTAND THE PROCESSES BY WHICH PRIMITIVE (CHONDRITIC) MATERIALS WERE TRANSFORMED INTO EVOLVED (ACHONDRITIC) M

GEOLOGIC EVOLUTION OF THE WESTERN FLANK OF ALBA MONS, MARS VOLCANISM IS A DOMINANT PROCESS IN THE GEOLOGIC HISTORY OF MARS AND UNDERSTANDING THE GEOL

HELLAS IS THE LARGEST PRESERVED IMPACT FEATURE ON MARS AND ITS DEEPEST DEPOSITIONAL BASIN. THE GEOLOGY OF THE HELLAS BASIN FLOOR RIM AND SURROUNDINGS PRESENTS A DETAILED RECORD OF THE NUMEROUS PROCESSES AFFECTING THE MARTIAN SURFACE FROM THE NOACHI

SATURN S MOON TITAN IS UNIQUE IN THE SOLAR SYSTEM AS THE ONLY BODY BESIDES EARTH WITH AN ACTIVE HYDROLOGICAL SYSTEM. THE DETAILS OF THIS HYDROCARBON-BASED HYDROLOGICAL SYSTEM REMAIN POORLY UNDERSTOOD. THE ASYMMETRY IN THE DISTRIBUTION OF LAKES

THE RECENT RESULTS FROM THE DAWN MISSION SUGGESTED THAT CERES IS AN AQUEOUSLY ALTERED CRYOVOLCANIC WORLD MAYBE AN OCEAN WORLD THAT IS SIMILAR TO SOME OUTER SOLAR SYSTEM ICY SATELLITES IN GEOLOGY GEOPHYSICS GEOCHEMISTRY AND MINERALOGY. THREE GEOLOGICALLY YOUNG FEATURES NAMELY OCCATOR CRATER (AND THE CEREALIA AND VINALIA FACULAE INSIDE IT) AHUNA MONS AND HAULANI CRATER ARE IDENTIFIED TO HAVE HIGH SCIENTIFIC VALUES TO UNDERSTANDING ENDOGENIC PROCESSES SUCH AS CRYOVOLCANISM ON CERES. THEY ALL PRESERVE THE CRYOVOLCANIC AND IMPACT SIGNATURES HOST SEVERAL TYPES OF ICE-RELATED LANDFORMS AND HAVE GOOD DATA COVERAGE AND THE HIGHEST RESOLUTION DAWN IMAGES. THIS PROPOSAL WILL CHARACTERIZE THE SPECTRAL LIGHT-SCATTERING PROPERTIES OF THOSE THREE REGIONS AIMING TO BETTER UNDERSTANDING THE CRYOVOLCANIC CRYOMAGMATIC AND DIAPIRIC PROCESSES ON CERES.

OUR PROJECT PROVIDES A COMPREHENSIVE PICTURE OF THE FLOW OF MATERIAL AND ENERGY ACROSS LARGE DISTANCES IN THE JOVIAN MAGNETOSPHERE INCLUDING ITS ULTIMATE SOURCES AND SINKS. WE SEEK TO ANSWER FUNDAMENTAL QUESTIONS IN JOVIAN MAGNETOSPHERIC PHYSICS WHICH ULTIMATELY ADVANCE OUR UNDERSTANDING OF MASS TRANSPORT AND ENERGY DEPOSITION IN MAGNETIZED PLASMAS. BY ARCHIVING OUR DATA WITH NASA'S PLANETARY DATA SYSTEM WE LEAVE A LEGACY FOR FUTURE PLANETARY SCIENTISTS TO STUDY THE DYNAMIC PLASMA ENVIRONMENTS OF GIANT PLANET MAGNETOSPHERES.

THE SOUTH POLE-AITKEN BASIN (SPA) IS A HIGH-PRIORITY LOCATION FOR SCIENTIFIC STUDIES AND EXPLORATION. SPA DOES NOT APPEAR TO CONTAIN AS MUCH BASALTIC FILL

INVESTIGATING SOLAR SYSTEM EVOLUTION BY IDENTIFYING AND CHARACTERIZING BINARY TROJAN AND HILDA ASTEROIDS THE PRIMARY GOAL OF THIS PROPOSAL IS TO HELP CONSTRAIN THE DYNAMICAL EVOLUTION OF THE SOLAR SYSTEM BY IDENTIFYING AND CHARACTERIZING BINARY ASTEROIDS IN THE JOVIAN TROJAN AND HILDA POPULATIONS. ONE OF THE MOST DEBATED ISSUES IN SOLAR SYSTEM FORMATION IS GIANT PLANET MIGRATION. THE OBJECTS THOUGHT TO BE MOST AFFECTED BY THIS MIGRATION ARE JOVIAN TROJAN ASTEROIDS (HEREAFTER TROJANS) WHICH LIE IN STABLE ORBITS AROUND JUPITERS L4 AND L5 LAGRANGE POINTS. GENTLE PLANETARY MIGRATION MODELS (E.G. MARZARI&SCHOLL 1998) NECESSITATE THAT TROJANS FORMED IN SITU WHILE THE NICE MODEL OF RAPID OUTWARD GIANT PLANET MIGRATION SUGGESTS THAT TROJANS FORMED IN THE OUTER SOLAR SYSTEM AND WERE SCATTERED INTO THEIR PRESENT ORBITS (E.G. MORBIDELLI ET AL. 2005). THE NICE MODEL COMBINED WITH THE GRAND TACK MODEL (E.G. WALSH ET AL. 2011) ALSO PREDICTS THAT TROJANS AND HILDA ASTEROIDS (IN 3:2 ORBITAL RESONANCE WITH JUPITER) SHARE AN ORIGIN. ONE OBSERVABLE PROPERTY THAT SETS POWERFUL CONSTRAINTS ON FORMATION LOCATION IS BULK DENSITY WHICH IS MORE LIKELY TO REFLECT EARLY SOLAR SYSTEM CONDITIONS THAN SURFACE MATERIAL ALTERED BY IRRADIATION. LOW DENSITIES ARE LINKED TO THE ICE-RICH OUTER SOLAR SYSTEM WHILE HIGH DENSITIES ARE CONSISTENT WITH THE WARMER INNER SOLAR SYSTEM ENVIRONMENT. TO HELP DETERMINE THE TROJAN AND HILDA ORIGIN(S) WE WILL IDENTIFY AND CHARACTERIZE THEIR CONSTITUENT CLOSELY SEPARATED BINARY ASTEROID SYSTEMS USE THE BINARIES TO CONSTRAIN DENSITY AND COMPARE THE DENSITIES TO THOSE OF OTHER SMALL BODIES. BINARY CHARACTERIZATION OFFERS THE ONLY MEANS OF DETERMINING DENSITY APART FROM A SPACECRAFT FLY-BY. WE WILL CONDUCT THE FIRST SYSTEMATIC LARGE-SAMPLE STUDY OF TROJAN AND HILDA BINARIES. ANOTHER MAJOR RESULT FROM THIS WORK WILL BE DETERMINATION OF THE FRACTION OF TROJANS AND HILDAS IN CLOSELY SEPARATED BINARY SYSTEMS. A DIFFERENCE BETWEEN BINARY FRACTIONS OF TWO ASTEROID GROUPS IMPLIES DIFFERENT DYNAMICAL HISTORIES. FOR EXAMPLE IF ONE OF THE TROJAN CLOUDS HAS A HIGHER BINARY FRACTION THAN ANOTHER THEN THAT MIGHT SUPPORT THE JUMPING JUPITER MODEL WHICH PROPOSES THAT AN ICE GIANT TRAVERSED ONE OF THE TROJAN CLOUDS. IF THE TROJAN BINARY FRACTION IS INCONSISTENT WITH THE HILDA BINARY FRACTION THEN PERHAPS THEY DO NOT HAVE A COMMON ORIGIN AS SUGGESTED BY THE NICE MODEL. DIRECT IMAGING SURVEYS HAVE BEEN ABLE TO CONSTRAIN THE WIDELY SEPARATED TROJAN BINARY POPULATION BUT ONLY ONE SEARCH FOR CLOSE TROJAN BINARIES HAS BEEN PUBLISHED AND THIS SAMPLE WAS DOMINATED BY LARGE L5 TROJANS (>20KM; MANN ET AL. 2007). THE HILDA BINARY FRACTION HAS NEVER BEEN EXPLORED. TIGHT BINARIES WITH TYPICAL RUBBLE PILE STRUCTURES CAN SOMETIMES BE DISCOVERED BY THEIR ROTATIONAL LIGHT CURVES IF THEIR ORBITAL PLANES ARE IN LINE WITH EARTH (E.G. MANN ET AL. 2007). ALL THREE KNOWN CLOSE TROJAN BINARIES WERE DISCOVERED THIS WAY. USING DATA FROM THE WIDE-FIELD INFRARED SURVEY EXPLORER MISSION WE FOUND 80 TROJANS AND HILDAS (OUT OF ~1500 SEARCHED) WITH LARGE ENOUGH BRIGHTNESS VARIATIONS TO QUALIFY THEM AS POSSIBLE BINARIES (SONNETT ET AL. 2015). THIS SAMPLE SPANS A WIDE RANGE OF SIZES (~5-100KM) AND (FOR THE TROJANS) EQUALLY REPRESENTS BOTH L4 AND L5 CLOUDS. THREE OF THESE BINARY CANDIDATES ARE CONFIRMED THROUGH HISTORICAL DATA BUT THE REMAINDER HAVE YET TO BE CONFIRMED. IN THE PROPOSED WORK WE SEEK TO CONFIRM THEIR BINARITY BY DENSELY SAMPLING THEIR ROTATIONAL LIGHT CURVES DETERMINING THE SPIN PERIOD AND COMPARING BINARY AND SINGLE-BODY MODELS TO THE LIGHT CURVES WHILE SOLVING FOR BULK DENSITY. WE WILL THEN DEBIAS THE RESULTANT BINARY FRACTION AND COMPARE BINARY FRACTIONS TO ASSESS SIMILARITIES IN FORMATION ENVIRONMENTS AND DYNAMICAL HISTORIES. WE HAVE CONDUCTED A PILOT STUDY (9 TARGETS) AND WRITTEN MOST OF THE DEBIASING CODE AS PART OF THE PI S FELLOWSHIP ENDING IN MID-2016. WE THEREFORE SEEK ADDITIONAL SUPPORT FOR AN OBSERVING CAMPAIGN TO TARGE

DETECTION AND CHARACTERIZATION OF CIRCUMBINARY PLANETS AROUND TESS ECLIPSING BINARIES

UNRAVELING THE MYSTERIES OF SMALL-BODY RING SYSTEMS THROUGH NUMERICAL MODELING -RESEARCHERS FROM THE PLANETARY SCIENCE INSTITUTE SEEK TO CHARACTERIZE THE RING SYSTEMS AROUND SMALL SOLAR SYSTEM BODIES, SUCH AS CENTAURS AND KUIPER BELT OBJECTS. THE OBJECTIVE IS TO UNDERSTAND HOW THEY ARE MAINTAINED, GIVEN THAT RING MATERIAL TENDS TO SPREAD OVER TIME. THE RESULTS OF THIS STUDY COULD BE USED TO IMPROVE UNDERSTANDING OF OTHER, LARGER RING SYSTEMS. THE RESEARCH TEAM WILL ALSO DEVELOP PEDAGOGICAL MODULES FOR GRADE 7-9 TEACHERS ON RINGS OF THE SOLAR SYSTEM, AND THEY WILL PARTICIPATE IN GIRLS CAMP IN SOUTH AFRICA PROMOTING STEM CAREERS. THIS PROJECT AIMS TO UNDERSTAND AND IDENTIFY THE FUNDAMENTAL PHYSICS AT PLAY IN THE MAINTENANCE OF THESE RING SYSTEMS. SPECIFICALLY, THE GOALS ARE TO (1) CONFIRM WHETHER A SHEPHERD MOON CAN CONFINE MATERIAL AS OBSERVED AT CHARIKLO AND CHIRON, INCLUDING CONSTRAINING THE MOON?S SIZE AND LOCATION; (2) DISCOVER THE MECHANISMS AND UNDERLYING CAUSES OF UNUSUAL STRUCTURES OR FEATURES OBSERVED IN RINGS AROUND CHARIKLO; AND (3) PARAMETERIZE THE REQUIRED CONDITIONS (INCLUDING NUCLEUS SIZE, SHAPE, AND SPIN RATE) FOR RINGS TO BE STABLE AROUND SMALL, AXISYMMETRIC BODIES. THE PROJECT TEAM PLANS TO CARRY OUT N-BODY SIMULATIONS OF RING PARTICLES MOVING PAST A SATELLITE USING A MODEL PREVIOUSLY DEVELOPED FOR THE STUDY OF SATURN AND MODIFIED FOR SMALL BODIES. MODEL RESULTS WILL BE VERIFIED WITH EXISTING DATA FROM STELLAR OCCULTATIONS AND OTHER OBSERVATIONS OF CHARIKLO AND CHIRON. THIS AWARD REFLECTS NSF'S STATUTORY MISSION AND HAS BEEN DEEMED WORTHY OF SUPPORT THROUGH EVALUATION USING THE FOUNDATION'S INTELLECTUAL MERIT AND BROADER IMPACTS REVIEW CRITERIA.

SCIENTIFIC MOTIVATION: WIND HAS BEEN AN ENDURING GEOLOGIC AGENT THROUGHOUT MARS HISTORY WITH THE PRESENCE OF AEOLIAN BEDFORMS ACROSS A RANGE OF SIZES AND MORPHOLOGIES. MANY OF THESE AEOLIAN BEDFORMS ARE ENIGMATIC AS COMPARED TO CLASSICAL TERRESTRIAL

1. BACKGROUND AND MOTIVATION WIND HAS BEEN AN ENDURING GEOLOGIC AGENT THROUGHOUT MARS HISTORY BUT IT IS OFTEN UNCLEAR WHEN WHERE AND WHY SEDIMENT IS MOBILE IN THE CURRENT EPOCH. SPATIAL VARIATIONS IN SAND FLUXES RELATE TO EXTERNAL FORCING FACTORS

PRODUCTS OF EXPLOSIVE ERUPTIONS PYROCLASTIC DEPOSITS REPRESENT IMPORTANT SOURCES OF INFORMATION ABOUT THE THERMAL HISTORY AND VOLATILE CONTENT OF THE PLANET FROM WHICH THEY ORIGINATE. THE AREAL EXTENT AND PHYSICAL CHARACTERISTICS (GRAIN SIZE SHAPE

CATHERINE WEITZ / PLANETARY SCIENCE INSTITUTE GEOLOGIC HISTORY OF LIGHT-TONED LAYERED DEPOSITS AT VALLES MARINERIS THIS PROPOSAL SEEKS TO EXPLORE

THE STRUCTURE AND COMPOSITION OF THE SURFACES OF ICY SATELLITES ARE AFFECTED BY PRIMARILY EXOGENIC PROCESSES SUCH AS E RING GRAIN BOMBARDMENT AND PLASMA AND ELECTRON INTERACTIONS. WE PROPOSE TO INVESTIGATE THE EFFECTS OF THESE PROCESSES ON THE SUR

THE HAYABUSA SPACECRAFT ARRIVED AT NEAR-EARTH ASTEROID (25143) ITOKAWA IN SEPTEMBER 2005 AND RETURNED SAMPLES TO EARTH IN JUNE 2010. DURING ITS 3-MONTH-LONG ASTEROID PROXIMITY OPERATIONS ASTEROID MULTIBAND IMAGING CAMERA (AMICA) AND NEAR INFRARED SPECTROMETER (NIRS) MAPPED THE SURFACE OF THE ASTEROID. AMICA IMAGED THE SURFACE IN SEVEN COLOR FILTERS (0.38-1.0 MICRONS) AND A BROADBAND CLEAR FILTER CENTERED AROUND 0.65 MICRONS. NIRS INSTRUMENT OBTAINED OVER 80 000 RESOLVED SPECTRA OF ITOKAWA IN 64 CHANNELS COVERING A WAVELENGTH RANGE BETWEEN 0.76-2.25 MICRONS. THE FOCUS OF OUR 4-YEAR PROPOSAL IS TO A) CALIBRATE AND RESTORE THE HAYABUSA AMICA MULTICOLOR DATA TO FULL SPATIAL SPECTRAL AND PHOTOMETRIC ACCURACY AND CREATE A GLOBAL 7 COLOR MOSAICS AT THE BEST RESOLUTION POSSIBLE AND B) PRODUCE PHOTOMETRICALLY CORRECTED NIRS SPECTRAL DATA AND EXTRACT BAND PARAMETER MAPS OF ITOKAWA. USING THESE GLOBAL COLOR/SPECTRAL MOSAICS WE INTEND TO CREATE MINERAL (PYROXENE CHEMISTRY OLIVINE/PYROXENE RATIO) MAPS OF THE ENTIRE VISIBLE SURFACE ITOKAWA. THIS HIGH LEVEL DATASET WILL BE ARCHIVED ON THE PDS AND SERVE THE SCIENCE NEEDS OF THE ENTIRE PLANETARY SCIENCE COMMUNITY.

EVOLUTION OF MARTIAN LAVA FLOW FIELDS: INVESTIGATIONS OF PAHOEHOE-LIKE FLOW MORPHOLOGIES IN THE THARSIS AND ELYSIUM VOLCANIC PROVINCES

LASER-INDUCED BREAKDOWN SPECTROSCOPY HAS BECOME AN IMPORTANT TOOL USED TO ANSWER KEY SCIENCE QUESTIONS ON EXISTING AND PLANNED MISSIONS (MSL CURIOSITY AND MARS 2020 RESPECTIVELY). HOWEVER THE ACCURACY OF THESE LIBS-DERIVED MEASUREMENTS IS PLAGUED B

OBJECTIVES: THIS PROJECT WILL UPDATE THE SPICE DATA AND ARCHIVE GEOMETRIC BACKPLANE DATA FOR THE VISIBLE IMAGES (GEOMETRY INFORMATION) OF ALL COMETS (67P 19P 81P 9P AND 103P) IMAGED BY ROSETTA/OSIRIS-NAC DEEP SPACE 1/MICAS-VISCCD STARDUST/NAVCAM AND DEEP IMPACT/ITS/MRI/HRIV. ALONG WITH THESE TWO KINDS OF PRODUCT WE WILL ALSO ADD SUPPORTING MODULES IN ISIS3 TO BETTER SUPPORT THE IMAGE ANALYSES FROM ALL THESE MISSIONS AND PROVIDE THE COMMUNITY WITH ISIS3 SCRIPTS (ARCHIVED IN USGS ASTRO/ISIS3) FOR CALCULATING BACKPLANE DATA (FOR ROSETTA OSIRIS-WAC AND NAVCAM). CURRENTLY NONE OF THE COMET MISSION DATASETS PROVIDE PIXEL-WISE GEOMETRIC BACKPLANE DATA (INCIDENCE ANGLE EMISSION ANGLE PHASE ANGLE AND COMETOCENTRIC COORDINATES). THE CURRENT VERSIONS OF THE EPHEMERIS (SPICE) DATA OF ALL THESE MISSIONS (DEEP SPACE 1 DEEP IMPACT EPOXI STARDUST STARDUST-NEXT AND ROSETTA) DO NOT SUPPORT SUBPIXEL PRECISION REGISTRATION BETWEEN THE SHAPE MODEL AND ALL IMAGES. IN OTHER WORDS SCIENTISTS WHO NEED TO CALCULATE THE OBSERVING AND ILLUMINATION GEOMETRY FOR MODELING AND MAPPING PURPOSES HAVE TO GO THROUGH TEDIOUS AND REDUNDANT PROCESSES. METHODS: WITH OUR IMAGE PROCESSING TOOLS WE WILL REGISTER THE SHAPE MODEL PRECISELY TO ALL IMAGES TO PRODUCE GEOMETRIC BACKPLANES WITH SUBPIXEL SPATIAL PRECISION. WE WILL CALCULATE THE X AND Y OFFSETS AND CENTRAL ROTATION FROM THE SPACECRAFT POSITION AND POINTING AND CORRECT FOR IT BASED ON IMAGE REGISTRATION. FOR THE ROSETTA MISSION WE WILL USE THE RELATIVE OFFSET AND ROTATION WE DERIVED FROM OSIRIS-NAC IMAGES TO UPDATE THE CK KERNELS. FOR OTHER MISSIONS WE WILL USE THE OFFSETS AND ROTATION TO CORRECT THE SPICE DATA (CK AND/OR SPK) FOR SPACECRAFT AND COMET DATA USING BUNDLE ADJUSTMENT PROCESSES. THE BACKPLANE DATA AND UPDATED SPICE DATA WILL BE ARCHIVED TO THE PDS SMALL BODIES NODE (SBN) AND PDS NAIF FOR SCIENTIFIC ANALYSES BY THE BROAD COMMUNITY. SIGNIFICANCE: THE PRECISELY REGISTERED BACKPLANE DATA WILL GREATLY ACCELERATE THE SCIENTIFIC ANALYSIS THAT REQUIRES MEASUREMENTS OF GEOMETRY INCLUDING PHOTOMETRY SPECTROSCOPY GEOMORPHOLOGY AND PHOTOGRAMMETRY ETC. THE IMPROVED SPICE KERNELS WILL BE BENEFICIAL FOR ALL SCIENCES THAT REQUIRE ACCURATE LOCATIONS AND POINTINGS OF THE SPACECRAFT SUCH AS MASS (DENSITY) ESTIMATES SHAPE MODEL IMPROVEMENTS AND MEASUREMENTS OF THE ORBIT WOBBLING OF THE COMETS AND CREATION OF CARTOGRAPHIC MAPS. THE ROSETTA DATA ARCHIVE HAS JUST BEEN COMPLETED IN THE PDS AND MANY SCIENTISTS NEED THE GEOMETRY DATA FOR THEIR ANALYSES. WITH THIS WORK WE ARE SAVING THEM THE EFFORTS TO CONFIGURE SPICE RENDER THE HUGE 44 MILLION FACETS SHAPE MODEL AND GO THROUGH A LARGE AMOUNT OF REDUNDANT AND TEDIOUS WORK FOR SPATIAL REGISTRATION. WITH THE RIGHT TEAM AND THE RIGHT TOOL WE ENSURE THE ARCHIVAL OF THE BACKPLANE DATA WITH THE BEST GEOMETRY ACCURACY BASED ON BEST CURRENTLY AVAILABLE SHAPE MODEL AND THE TESTED CONTROLLED REGISTRATION QUALITY (SUB-PIXEL). FOR OTHER PREVIOUS COMET MISSIONS THE ISIS3 SUPPORTS AND UPDATED SPICE WILL HELP THE COMMUNITY WITH ACCESS TO IMPROVED GEOMETRIC DATA AND ENABLE MANY NEW RESEARCH OPPORTUNITIES. WE ALSO SUBSTANTIALLY SIMPLIFY THE PROCESS OF REVISITING THE DATASETS FROM HISTORICAL COMETARY MISSIONS. RELEVANCE TO PDART: THE PROPOSED WORK IS RELEVANT TO THE PLANETARY DATA ARCHIVING RESTORATION AND TOOLS (PDART) PROGRAM AS WE WILL RESTORE AND ARCHIVE DATASETS FOR USE BY THE COMMUNITY; WE WILL PRODUCE NEW DATA PRODUCTS TO BE SUBMITTED TO THE PDS THEREBY INCREASING THE AMOUNT AND QUALITY OF DATA PRODUCTS THAT ENHANCE FUTURE SCIENTIFIC INVESTIGATIONS. THE PROPOSED ARCHIVE HOLDS RELEVANCE FOR ALL THE COMET MISSIONS AS WELL AS A FUTURE COMET MISSION. THE DATASETS WOULD BOOST SCIENCE AND FUTURE PROPOSALS RELATED TO ROSETTA AND OTHER COMET MISSION DATA AND PUSH MORE REVISITING STUDY ON THE HISTORICAL MISSION DATA. PROMPT AVAILABILITY OF THIS DATA MADE POSSIBLE BY THIS PROPOSAL PROVIDES EFFICIENT AND ACCURATE ANALYSIS OF COMET DATA.

COMPARING ICE-ATMOSPHERE INTERACTION ON MARS PLUTO AND TRITON - PSI

WE PROPOSE THAT THIS CIRCULARIZATION RESULTS FROM SUBLIMATIVE ORBITAL PERTURBATIONS A VAPORIZATION-DRIVEN PROCESS ANALOGOUS TO THE YARKOVSKY EFFECT.

THE CHANG E 2 MRM COLLECTED THE FIRST EVER GLOBAL MAPS OF THE MOON AT 3 7.8 19 AND 37 GHZ OVER THE ENTIRE LUNAR DIURNAL CYCLE. THIS IS A UNIQUE DATA SET IN A NEW FREQUENCY RANGE THAT IS ABSENT FROM NASAS LUNAR RECONNAISSANCE.

UNDERSTANDING THE EVOLUTION OF THE MARTIAN CRYOSPHERE IS OF FUNDAMENTAL CLIMATOLOGICAL SIGNIFICANCE DUE TO THE POTENTIAL RAMIFICATIONS OF ITS VOLATILITY. MARSIS (MARS ADVANCED RADAR FOR SUBSURFACE AND IONOSPHERE SOUNDING) AND SHARAD (SHALLOW RADAR)

21-NFDAP21_2-0003 TIMESCALES FOR BOULDER EVOLUTION FROM THERMAL FATIGUE AND IMPACTS ON ASTEROID (101955) BENNU

MAPPING WATER IN THE OUTER ASTEROID BELT

INVESTIGATING CENTAUR SURFACE COLORS: CONNECTING SURFACE TRANSFORMATION TO THERMAL AND DYNAMICAL HISTORY

THERE IS ABUNDANT GEOMORPHIC EVIDENCE OF A LARGE ANCIENT INVENTORY OF SURFACE WATER ON MARS, BUT HOW MUCH REMAINS EXTANT AND WHERE IT CURRENTLY RESID

THIS PROPOSAL IS DIRECTLY RELEVANT TO THE MDAP PROGRAM WHICH SOLICITS PROPOSALS FOR SCIENTIFIC ANALYSIS OF DATA FROM HIRISE CTX CRISM MCS TES AND THEMIS.

21-PDART21-0014 TOOLS FOR ADVANCED DYNAMICAL CHARACTERIZATION OF SOLAR SYSTEM SMALL BODIES

"VOLATILE-RICH AEOLIAN DEPOSITS: A FIELD-BASED ANALOG STUDY"SUMMARY: AEOLIAN DUNES ON MARS MAY CONTAIN SIGNIFICANT VOLATILE RESERVOIRS OF ICE SNOW

IMPACT MELT PONDS FLOWS AND VENEERS ARE FOUND AROUND DOZENS OF COPERNICAN-AGED IMPACT STRUCTURES ON THE MOON. MELT AND EJECTA ARE EMPLACED CONTEMPORANEOUSLY AND SHOULD RECORD THE PRIMARY FLUX OF INNER SOLAR SYSTEM PROJECTILES BUT RECENT OBSERVATIONS HAVE SHOWN THAT: (1) SMALL-DIAMETER (<500 M) CRATER SIZE-FREQUENCY DISTRIBUTION (CSFDS) DIFFER BETWEEN MELT FEATURES AND ADJACENT CONTINUOUS EJECTA ASSOCIATED WITH THE SAME IMPACT CRATERING EVENT; (2)GHOST CRATERS BURIED BY IMPACT MELT SUGGEST THAT EJECTA BLANKETS ARE CRATERED IMMEDIATELY FOLLOWING EMPLACEMENT AND SOME CRATERS FORMED ON MELT UNITS POSSESS UNUSUAL SHAPES INCLUDING IRREGULAR CIRCULAR CRATERS WITH SPLASH-LIKE MORPHOLOGIES (POSSIBLY FORMED BY SECONDARY IMPACTS INTO VISCOUS MELT PONDS). BOTH OBSERVATIONS FAVOR THE HYPOTHESIS THAT SMALL-DIAMETER CRATERS ARE FORMED ON CONTINUOUS EJECTA DEPOSITS BY LATE-ARRIVING EJECTA FRAGMENTS FROM THE PARENT CRATER AND ARE EMPLACED PENECONTEMPORANEOUSLY WITH THE IMPACT MELT FACIES. THESE CRATERS ARE REFERRED TO AS SELF-SECONDARY CRATERS (SSCS). DETAILED STUDY OF THE ABUNDANCE DISTRIBUTION AND MORPHOLOGY OF SSCS MAY HELP TO IMPROVE OUR UNDERSTANDING FIRST OF LATE-STAGE EJECTA PROCESSES AND THE TIMING OF EVENTS SHAPING THE CONTINUOUS EJECTA BLANKET AND SECOND OF CRATER SIZE-FREQUENCY DISCREPANCIES BETWEEN MELT AND EJECTA FACIES AND THEIR POSSIBLE EFFECT ON THE LUNAR CRATER CHRONOLOGY. ALTHOUGH SSC EXISTENCE HAS BEEN WIDELY PROPOSED RECENTLY NOT ONLY ON THE MOON BUT ALSO ON MERCURY VESTA AND ICY SATELLITES THE MECHANISM OF THEIR FORMATION IS STILL NOT CLEAR; EXISTING HYPOTHESES HAVE YET TO BE SHOWN FEASIBLE BY MEANS OF NUMERICAL MODELS. EMPLACEMENT OF IMPACT MELTS HAS BEEN A SUBJECT OF LONG-STANDING DEBATE AND DETAILED ANALYSIS OF IMPACT CRATERS ON MELT UNITS GIVES US A NEW INSTRUMENT WHICH MAY HELP TO RESOLVE ISSUES OF TIMING AND EMPLACEMENT.

SCIENCE GOALS AND OBJECTIVES: ONE OF THE KEY DRIVERS OF THE MARS EXPLORATION PROGRAM IS THE SEARCH FOR EVIDENCE OF PAST OR PRESENT LIFE. IN THIS CONTEXT THE MOST RELEVANT MARTIAN ENVIRONMENTS TO INVESTIGATE ARE THOSE ASSOCIATED WITH LIQUID WATER.

HARMONIC ANALYSIS OF THE MARTIAN NITRIC OXIDE NIGHTGLOW

DEVELOPMENT AND CLIMATE CHANGE IN HIGH MOUNTAIN ASIA (HMA) ARE AFFECTING NATURAL HAZARDS. HMA IS VULNERABLE DUE TO THE EXPOSURE OF LARGE POPULATIONS AND BECAUSE OF HIGH SEISMIC AND EARTH SURFACE PROCESS ACTIVITY. WE WILL EXPLORE LINKS BETWEEN MOUNTAIN HAZARDS AND GLACIERS SNOWFIELDS GLACIAL LAKES AND UNSTABLE MOUNTAIN SLOPES AND ROCK DEBRIS IN GLACIERIZED NEPAL BHUTAN AND ADJOINING CHINA- A HMA REGION OF ABUNDANT GLACIAL LAKES AND FLOODS IN THE KOSHI AND GANDAKI BASINS (NEPAL) TO 200 KM DOWNSTREAM. WE WILL INVESTIGATE OVER THE SATELLITE ERA (SINCE LANDSAT 5) THE MASS MOVEMENT ENVIRONMENT OF GLACIAL LAKES LAKES EFFECTS ON GLACIER DYNAMICS AND TIMESCALES FROM GLACIER LAKE INCEPTION THROUGH GROWTH TO GLACIER LAKE OUTBURST FLOODS (GLOFS); COMPARE GLOFS WITH OTHER MOUNTAIN FLOOD TYPES: TRIGGERS TIMESCALES PEAK DISCHARGES AND DOWNSTREAM REACH.

PASSING STARS AND THE ORBITAL EVOLUTION OF OUR PLANETS

THE CHAOTIC TERRAINS OF MERCURY: UNVEILING THE HISTORY OF PLANETARY VOLATILE RETENTION AND LOSS IN THE INNERMOST SOLAR SYSTEM

OBJECTIVES: THIS PROJECT WILL ARCHIVE GASKELL SHAPE MODELS FOR THE SATURNIAN SATELLITES LISTED BELOW. TO DATE THERE ARE NO GASKELL SHAPE MODELS FOR RHEA IAPETUS OR ENCELADEUS WITHIN THE PLANETARY DATA SYSTEM (PDS) ARCHIVE. CURRENT MODELS FOR MIMAS

A SYSTEMATIC LARGE-SCALE SURVEY OF THE OVERLOOKED POPULATION OF SMALL OBJECTS BETWEEN THE ORBITS OF THE OUTER PLANETS.

SCIENTIFIC/TECHNICAL/MANAGEMENT MARS HAS A MASSIVE UP TO 1 KM-THICK CO2 ICE DEPOSIT BURIED BENEATH A ~10 M-THICK LAYER OF H2O ICE AT ITS SOUTH POLE. IF RELEASED THE BURIED CO2 ICE COULD DOUBLE MARS ATMOSPHERIC PRESSURE AND SIGNIFICANTLY ALTER MARS CLIMATE. THE BURIED CO2 ICE DEPOSIT ARISES FROM DEPOSITION OF ATMOSPHERIC CO2 AT TIMES OF LOW OBLIQUITY (LESS POLAR SUNLIGHT) THAT IS SUBSEQUENTLY BURIED BY A LAYER OF H2O ICE. THE MANNER AND FREQUENCY IN WHICH THE BURIED CO2 IS RELEASED INTO THE ATMOSPHERE IS AN OPEN QUESTION WITH PROFOUND IMPLICATIONS FOR MARS CLIMATE. ONE HYPOTHESIS PROPOSES THAT THE H2O ICE LAYER IS PERMEABLE TO CO2 GAS FLOW SUCH THAT THE BURIED CO2 FREELY AND GRADUALLY EQUILIBRATES WITH THE ATMOSPHERE AS MARS OBLIQUITY EVOLVES. AN ALTERNATIVE HYPOTHESIS PROPOSES THAT THE H2O LAYER PHYSICALLY AND THERMALLY SEQUESTERS THE BURIED CO2 FROM THE ATMOSPHERE SUCH THAT THE BURIED CO2 IS RELEASED ONLY RARELY WHEN THE H2O LAYER IS ABLATED AT TIMES OF CRITICALLY HIGH OBLIQUITY. IMPORTANTLY MARS MEAN PRESSURE THROUGHOUT ALL OF THE AMAZONIAN WOULD BE SIGNIFICANTLY LOWER IF H2O ICE LAYERS TYPICALLY SEQUESTER A PORTION OF MARS CO2 INVENTORY AS BURIED CO2 ICE. THUS DETERMINING WHETHER H2O LAYERS SEQUESTER THE BURIED CO2 HAS SIGNIFICANT CONSEQUENCES FOR UNDERSTANDING AMAZONIAN MARS CLIMATE HABITABILITY AND SURFACE GEOLOGIC PROCESSES. EACH OF THE TWO HYPOTHESES PREDICTS DIFFERENT MORPHOLOGIC DEVELOPMENT AND SEASONAL TEMPERATURE BEHAVIOR OF THE H2O ICE LAYER. THEREFORE WE WILL ANALYZE THE MORPHOLOGIC AND THERMAL CHARACTERISTICS OF THE H2O ICE LAYER IN ORDER TO DETERMINE WHETHER THE H2O ICE LAYER SEQUESTERS THE BURIED CO2. METHODOLOGY TO ACHIEVE OUR GOAL WE WILL: 1. USE CONTEXT CAMERA (CTX) AND HIGH-RESOLUTION IMAGING SCIENCE EXPERIMENT (HIRISE) IMAGES AND DIGITAL TERRAIN MODELS TO MAP THE MORPHOLOGY AND STRUCTURE OF THE TOPMOST H2O LAYER. 2. USE CTX TO OBSERVE THE SPATIOTEMPORAL EXPOSURE OF THE H2O LAYER THROUGH OVERLYING SEASONAL CO2 FROST AND HOLES IN THE RSPC COUPLED WITH THERMAL EMISSION IMAGING SYSTEM (THEMIS) DATA TO MAP THE SEASONAL TEMPERATURE CYCLE OF THE EXPOSED H2O REGIONS. 3. QUANTITATIVELY MODEL THE MORPHOLOGICAL DEVELOPMENT OF THE H2O LAYER AND HEAT TRANSFER THROUGH THE H2O LAYER MATCHED TO OBSERVATION TO DETERMINE WHETHER CO2 SUBLIMES THROUGH THE H2O LAYER. 4. MODEL SINTERING RATES OF THE H2O LAYER BASED ON THE OBSERVED THERMAL ENVIRONMENT TO DETERMINE WHETHER THE H2O LAYER WILL BECOME IMPERMEABLE TO CO2 GAS FLOW. RELEVANCE TO MARS DATA ANALYSIS PROGRAM (MDAP) ROSES 2020 CALL C.9 (MARS DATA ANALYSIS) STATES THAT THE OBJECTIVE OF THE MARS DATA ANALYSIS PROGRAM (MDAP) IS TO ENHANCE THE SCIENTIFIC RETURN FROM MISSIONS TO MARS CONDUCTED BY NASA AND OTHER SPACE AGENCIES [ INCLUDING] MARS ODYSSEY (MO) [AND] MARS RECONNAISSANCE ORBITER (MRO). OUR PROPOSED WORK WILL EXTENSIVELY USE OBSERVATIONS FROM THE HIRISE AND CTX INSTRUMENTS ONBOARD MRO AND THE THEMIS INSTRUMENT ONBOARD MO THEREBY ENHANCING THEIR SCIENTIFIC RETURN. ROSES 2020 CALL C.9 ALSO STATES THAT TASKS RESPONSIVE TO THIS CALL INCLUDE 1) DATA ANALYSIS TASKS [AND] 2) NONDATA-ANALYSIS TASKS THAT ARE NECESSARY TO ANALYZE OR INTERPRET THE DATA THESE TASKS MAY INCORPORATE THEORY MODELING LABORATORY STUDIES CORRELATIVE ANALYSES AND/OR OTHER RESEARCH AS LONG AS THE PRIMARY FOCUS OF THE WORK IS DATA ANALYSIS. OUR RESEARCH PLAN IS TO OBSERVE THE MORPHOLOGY AND TEMPERATURE CYCLE OF THE TOPMOST H2O LAYER OF MARS MCID AND THEN INTERPRET OUR OBSERVATIONS USING NUMERICAL MODELING. THE PROPOSED WORK INVOLVES 80% EFFORT FOR DATA ANALYSIS TASKS AND 20% SUPPORTING MODELING WORK AND IS THEREFORE RESPONSIVE TO MDAP RATHER THAN SOLAR SYSTEM WORKINGS BECAUSE ROSES 2020 CALL C.3 (SOLAR SYSTEM WORKINGS) STATES THAT "SOLAR SYSTEM WORKINGS DOES NOT ACCEPT PROPOSALS

THE PROPOSED INVESTIGATION WILL PROVIDE NEW CONSTRAINTS ON THE GEOLOGIC EVOLUTION OF THE LARGEST VOLCANIC PROVINCE ON THE MARTIANSURFACE THROUGH DETAILED MAPPING OF ITS SOUTHERN EXTENT IN DAEDALIA PLANUM. THE STYLES TIMING AND SPATIAL EXTENT OF THARSIS VOLCANISMWILL BE EXAMINED THROUGH A SYSTEMATIC MAPPING INVESTIGATION OF THE LAVA FLOW FIELDS TO THE SOUTH OF ARSIA MONS THAT FORM DAEDALIAPLANUM AND EMBAY THE HIGHLANDS OF TERRA SIRENUM TO THE SOUTH. THIS RESEARCH WILL INCLUDE PRODUCTION OF:A) ONE FORMAL USGS GEOLOGIC MAP PUBLICATION A 1:1M-SCALE GEOLOGIC MAP OF SIX MTM QUADRANGLES (-30137 -30132 -30127 -35137 -35132 AND -35127) IN DAEDALIA PLANUM COVERING THE FRESH CRATER ZUMBA AND ITS EXTENSIVE RAYS THE SURROUNDING LAVA FLOW FIELDS SMOOTH AND RIDGED PLAINS AND THE HIGHLANDS OF TERRA SIRENUM TO THE SOUTH ANDB) AS A DIGITAL SUPPLEMENT TO THE GEOLOGIC MAP A DETAILED LAVA FLOW FIELD MAP PROVIDING REPRESENTATIONS OF FLOW LOBE MARGINS CHARACTERIZATION OF DIFFERENT FLOW TYPES DELINEATION OF CHANNEL AND LEVEE SYSTEMS AND FLOW SURFACE TEXTURES AND STRUCTURES AS WELL ASDOCUMENTATION OF RELATIVE AGE RELATIONSHIPS BETWEEN ADJACENT FLOWS. FLOW FIELD MAPPING WILL BE COMPILED AT 1:100 000 SCALE.GEOLOGIC MAPPING WILL BE BASED PRIMARILY ON THEMIS DAYTIME THERMAL INFRARED (TIR) IMAGES SUPPORTED BY VARIOUS OTHER IMAGINGDATASETS AND THE DETAILED LAVA FLOW FIELD MAPS WILL BE GENERATED USING CTX AND THEMIS VIS COVERAGE. THIS PROJECT WILL UTILIZEGEOGRAPHIC INFORMATION SYSTEMS (GIS) SOFTWARE AND ANALYSIS TOOLS FOR THE PRODUCTION OF BOTH HARD COPY AND DIGITAL MAP PRODUCTS.

CHARACTERIZING THE NATURE OF SURFACE MATERIALS ON MARS IS ESSENTIAL FOR DETERMINING THE PAST AND PRESENT CLIMATE AND FOR ASSESSING FUTURE LANDING SITES. IN PARTICULAR SEDIMENTARY SURFACE MATERIALS MAY CONTAIN A RECORD OF HABITABILITY THE WATER CYCLE AND VARIABILITY ATMOSPHERIC CIRCULATION AND GEOLOGIC SURFACE PROCESSES. THE MATERIALS MAY BE INVESTIGATED BY A DIVERSE SUITE OF ORBITAL INSTRUMENTS AND A GREATER VARIETY SHOULD LEAD TO BETTER CHARACTERIZATION. CRITICAL TO THE CHARACTERIZATION OF SURFACE MATERIALS IS UNDERSTANDING THEIR MINERALOGICAL AND PHYSICAL PROPERTIES INCLUDING THEIR COMPOSITION AND DISTRIBUTION. WHEREAS MATERIALS ARE SPREAD NON-UNIFORMLY OVER THE MARTIAN SURFACE MANY DEPOSITS EXIST IN LOCATIONS THAT ARE DIFFICULT TO MEASURE WITH ONE OR MORE INSTRUMENTS IMPEDING FULL CHARACTERIZATION. IN RARE CASES MANY ORBITING INSTRUMENTS ARE ABLE TO TRAIN ON A SINGLE DEPOSIT OR MULTIPLE DEPOSITS IN THEIR ENTIRETY. WE HAVE LOCATED SEVERAL OF THESE DEPOSITS NEAR THE RIM OF VALLES MARINERIS (VM) AND NEIGHBORING CHASMATA THAT MAY BE CHARACTERIZED BY OPTICAL IMAGERY SPECTROSCOPY THERMAL BEHAVIOR AND NOW SOUNDING RADAR. OUR OBJECTIVE IS TO CONSTRAIN THE CHEMICAL AND PHYSICAL PROPERTIES OF SEDIMENTARY DEPOSITS ON THE VALLES MARINERIS RIM AND TO TEST THE VARIOUS HYPOTHESES OF THEIR ORIGIN. MULTIDISCIPLINARY APPROACHES SUCH AS THIS ARE DIFFICULT ON MARS EITHER BECAUSE SURFACE CHARACTERISTICS MAKE THE APPLICATION OF RADAR IMPOSSIBLE OR BECAUSE OF A LACK OF EXPOSURE LIMITING ACCESS WITH OTHER INSTRUMENTS. THUS THE VALLES MARINERIS PLATEAU DEPOSITS MAY SERVE AS AN IDEAL TEST LOCATION FOR UNDERSTANDING ALTERED SEDIMENTARY DEPOSITS ON MARS. CENTRAL TO OUR INVESTIGATION IS COMBINING MULTIDISCIPLINARY TECHNIQUES THAT CHARACTERIZE LAYERED DEPOSITS IN VARIOUS WAYS. IN LIGHT OF THAT WE WILL USE DATA FROM SHARAD HIRISE CTX CRISM THEMIS TES AND HRSC. AS AN ENSEMBLE THESE INSTRUMENTS PROVIDE VIEWS OF THE LLD THAT ARE MORE COMPLETE THAN IN PREVIOUS STUDIES. RECENT INCREASES IN COVERAGE WITH HIGH RESOLUTION IMAGERY DIGITAL TERRAIN MODELS (DTMS) AND SPECTRAL IMAGES WILL ENHANCE THE RETURN. IN SUPPORT OF MANY GOALS OF THE MARS DATA ANALYSIS PROGRAM (MDAP) AND THE MARS EXPLORATION PROGRAM ANALYSIS GROUP (MEPAG) WE WILL COMBINE DATASETS FROM SEVERAL INSTRUMENTS AND MISSIONS TO DETERMINE THE PHYSICAL AND COMPOSITIONAL CHARACTERISTICS OF THE LLD AND TO TEST THE OPEN HYPOTHESES OF LLD FORMATION: (1) LACUSTRINE SEDIMENTARY DEPOSITION (2) VOLCANIC DEPOSITION OR (3) AEOLIAN/ AIRFALL DEPOSITION [WEITZ ET AL. 2010 AND REFERENCES THEREIN]. FURTHERMORE WE WILL LOOK FOR EVIDENCE THAT THE LLD HAVE A COMMON SOURCE OR ALTERATION SEQUENCE AND TEST SCENARIOS OF LLD DEPOSITION OCCURRING BEFORE AND AFTER VM FORMATION AND GROWTH. PRODUCTS AND RESULTS WE WILL GENERATE TO TEST HYPOTHESES INCLUDE: MAPS OF FULL EXTENT THICKNESS AND VOLUME OF LLD OVER ENTIRE REGION WITH A FULL 3D RECONSTRUCTION; MAPS OF SPECTRAL COMPONENTS AND ALTERATION MINERALS IN A STRATIGRAPHIC CONTEXT; EXTRACTED GEOPHYSICAL AND THERMOPHYSICAL PROPERTIES FOR EACH LOCATION; CONSTRAINTS ON THE RELATIVE TIMING AND DURATION OF DEPOSITION AND ALTERATION; CONSTRAINTS ON THE HYDROLOGIC AND TECTONIC SETTINGS DURING DEPOSITION; AND CONSTRAINTS ON THE POROSITY AND DENSITY OF LLD.

RECENT IN SITU OBSERVATIONS OF COMETS HAVE HIGHLIGHTED THE IMPORTANCE OF VOLATILES OTHER THAN WATER IN DRIVING COMET ACTIVITY EVEN AT SMALL HELIOCENTRIC DISTANCES. CO2 AND CO HAVE BEEN SHOWN TO BE PARTICULARLY IMPORTANT. ROSETTA OBSERVATIONS ARE SUGGESTING NEW IDEAS ABOUT THE PRIMARY DRIVERS OF COMET ACTIVITY AT LARGE HELIOCENTRIC DISTANCES. THESE DEVELOPMENTS ARE DRIVING A PARADIGM SHIFT IN COMET STUDIES WHICH CALLS FOR THE REANALYSIS OF ALL COMET OBSERVATIONS. BY ARCHIVING WITH THE PDS A SIGNIFICANT AND UNIQUE COLLECTION OF WIDE-FIELD SPACE-BASED COMET OBSERVATIONS OUR EFFORT PROVIDES DATA CRITICAL TO ANSWERING THIS CALL. THE MIDCOURSE SPACE EXPERIMENT (MSX) THE GALAXY EVOLUTION EXPLORER (GALEX) AND THE SWIFT ULTRAVIOLET/OPTICAL TELESCOPE (SWIFT/ UVOT) ARE NON-PLANETARY SCIENCE DIVISION SPACE TELESCOPES WHICH HAVE OBSERVED MORE THAN TWO DOZEN COMET APPARITIONS SINCE 1996. THREE WERE CONTEMPORANEOUS WITH SPACECRAFT FLYBYS AND FOUR WERE OBSERVED ON TWO APPARITIONS EACH. COMETS OF ALL DYNAMICAL CLASSES HAVE BEEN OBSERVED MOST OVER A RANGE OF HELIOCENTRIC DISTANCES THE LARGEST OF WHICH BEING 0.8 -- 5 AU. UNIQUE FEATURES OF THE MSX GALEX AND SWIFT/UVOT OBSERVATIONS INCLUDE THEIR WIDE FIELDS OF VIEW (17 ARCMIN -- 10 DEGREES) AND THEIR SENSITIVITY TO UV EMISSIONS. IN FACT FOR EMISSION LONGWARD OF H-LYMAN ALPHA THESE SPACECRAFT HAVE COLLECTED ALMOST ALL OF THE AVAILABLE WIDE-FIELD UV DATA! THE WIDE-FIELD FAR-UV CAPABILITIES MSX AND GALEX MAKE POSSIBLE THE STUDY OF ATOMIC END-MEMBERS H O C AND S WHICH HAVE VERY LONG LIFETIMES. SCIENTIFIC FRUIT HAS ALREADY BEGUN IN THIS DIRECTION WITH A SENSITIVE MEASUREMENT OF THE IONIZATION LIFETIME OF CARBON BY MORGENTHALER ET AL. (2011). SWIFT IS AN ACTIVE ASTROPHYSICS MISSION AND IS STILL ADDING TO ITS LIST OF 19 COMETS OBSERVED 9 OF WHICH WILL BE ARCHIVED WITH THE SUPPORT OF OUR PROPOSED PROJECT. SWIFT'S IMAGING AND SPECTRO-IMAGING CAPABILITIES IN THE UV AND VISIBLE ENABLE IT TO STUDY THE SUITE OF MOLECULAR EMISSION DIAGNOSTIC OF FRAGMENTS OF VOLATILE SPECIES: CS OH CN C3 AND C2. SCIENCE RESULTS FROM SWIFT/UVOT OBSERVATIONS HAVE ALREADY BEGUN TO FLOW (E.G. BODEWITS ET AL. 2011 2014 2015). OUR PROPOSED EFFORTS WILL SUPPORT ARCHIVING OF MSX GALEX AND SWIFT/UVOT DATA IN THE PLANETARY DATA SYSTEM (PDS) IN A FORMAT THAT IS ACCESSIBLE TO COMET SCIENTISTS. THE MSX DATA COVERING 1000A -- 9000A WITH A VARIETY OF IMAGING AND LONG-SLIT DETECTORS AND IMAGERS HAS NEVER BEEN PUBLICLY ARCHIVED. THE GALEX AND SWIFT DATA ARE PUBLICLY ARCHIVED BUT THE DATA WERE PROCESSED WITH THE ASSUMPTION THAT THE COMETS WERE FIXED TARGETS. PI MORGENTHALER AND CO-I BODEWITS HAVE DEVELOPED THE NECESSARY ALGORITHMS TO ACCOMMODATE MOVING TARGETS AND WITH THE SUPPORT OF OUR PROPOSED EFFORT WILL APPLY THEM AND ARCHIVE THE RESULTING PRODUCTS IN THE PDS. WE WILL ALSO ARCHIVE A UNIQUE SET OF GROUND-BASED OBSERVATIONS OF C/1996 B2 (HYAKUTAKE) AND C/1995 O1 (HALE-BOPP) WHICH COMPLEMENT SPACE-BASED OBSERVATIONS. THE DATA INCLUDE A RICH SET OF SYNOPTIC OBSERVATIONS OF H2O+ IN HALE-BOPP WHICH HAVE NEVER BEEN PUBLISHED AND VELOCITY RESOLVED H-ALPHA OBSERVATIONS OF HALE-BOPP WHICH ENABLE THE TESTING OF THE HYDROGEN COMA MODEL USED TO INTERPRET THE SOHO/SWAN WHICH HAS OBSERVED 56 COMETS SINCE 1996. ARCHIVING THESE DATA WILL "INCREASE THE AMOUNT AND QUALITY OF DIGITAL INFORMATION AND DATA PRODUCTS AVAILABLE FOR PLANETARY SCIENCE RESEARCH AND EXPLORATION...." AND IS THEREFORE HIGHLY RELEVANT TO THE PDART.

THE MARTIAN GEOLOGIC RECORD PROVIDES COMPELLING EVIDENCE FOR AN EARLY CLIMATE THAT SUPPORTED LIQUID WATER ON OR NEAR THE SURFACE YET

FUNDAMENTAL TO UNDERSTANDING OF THE GEOLOGIC EVOLUTION OF THE MARTIAN CRUST, AND THE PROCESSES THAT LEAD TO ITS FORMATION, IS THE CHARACTERIZATION OF

DERIVING THE ROTATIONAL STATE OF COMET 103P/HARTLEY 2 TO INTERPRET EPOXI DATA WE WILL DETERMINE THE ROTATIONAL STATE OF THE NUCLEUS OF COMET 103P/HAR

GIVEN THE RECENT OPTICAL PHOTOMETRIC CALIBRATION OF FIELD STARS OVER THE ENTIRE NIGHT SKY FROM -30 DEGREES TO +90 DEGREES IN DECLINATION BY THE PAN-STARRS1 (PS1) SURVEY WE PROPOSE TO CREATE A CATALOG OF CALIBRATED ASTROMETRY PHOTOMETRY AND PSF MEASUREMENTS OF SERENDIPITOUSLY OBSERVED SMALL SOLAR SYSTEM OBJECTS IN PUBLIC ARCHIVAL IMAGE DATA FROM VARIOUS FACILITIES (INCLUDING PS1 ITSELF THE SLOAN DIGITAL SKY SURVEY OR SDSS AND OTHER LARGE TELESCOPES). WE WILL EXTRACT AND CALIBRATE DETECTIONS OF KNOWN MINOR PLANETS MEASURING AN ESTIMATED ~4X10^7 SERENDIPITOUS OBSERVATIONS OF THESE OBJECTS ALL OBTAINED BY LARGE (2.5M-8M) TELESCOPES WHICH WE WILL MAKE PUBLICLY AVAILABLE VIA NASA'S PLANETARY DATA SYSTEM (PDS) AND THE MINOR PLANET CENTER (MPC). WE WILL UTILIZE TRAIL-FITTING CODE ORIGINALLY DEVELOPED FOR PS1 IN ORDER TO OBTAIN ACCURATE ASTROMETRY AND PHOTOMETRY FOR TRAILED OBJECTS IN LONG-EXPOSURE IMAGES. PSF MEASUREMENTS WILL ALSO BE MADE TO ENABLE SEARCHES FOR PREVIOUSLY UNKNOWN COMET-LIKE ACTIVITY AMONG OUR OBJECTS. THESE RESULTS WILL BE MADE PUBLICLY AVAILABLE VIA PDS AND ALSO VIA AN ONLINE SEARCH TOOL HOSTED BY THE PLANETARY SCIENCE INSTITUTE THAT WILL ALLOW USERS TO SEARCH FOR A PARTICULAR OBJECT LIST OF OBJECTS OR OBJECTS OR OBSERVATIONS MEETING CERTAIN CRITERIA AND OBTAIN A HISTORICAL SERENDIPITOUS OBSERVATIONAL RECORD OF THAT/THOSE OBJECT(S) INCLUDING ASTROMETRY PHOTOMETRY PSF MEASUREMENTS ASSOCIATED METADATA JPEG PREVIEW IMAGERY AND PROCESSED FITS FILES FOR EACH DETECTION. OUR OBJECTIVE IS TO CREATE AN EASILY RECONFIGURABLE DATA REDUCTION PIPELINE FOR THIS WORK. AS SUCH THOUGH WE WILL SPEND SIGNIFICANT TIME DEVELOPING PIPELINE CODE FOR THE FIRST DATA ARCHIVES TO BE PROCESSED THIS OVERHEAD SHOULD DECLINE SIGNIFICANTLY FOR SUBSEQUENT DATA ARCHIVES ALLOWING US TO EVENTUALLY ADD ADDITIONAL ARCHIVES WITH MINIMAL ADDITIONAL EFFORT. WE ALSO PLAN TO PERIODICALLY UPDATE OUR DATABASE AS ORBITS OF MORE ASTEROIDS BECOME SUFFICIENTLY WELL-DETERMINED FOR THEIR POSITIONS TO BE ACCURATELY PREDICTED AND AS NEW DATA FROM OUR EXISTING SUITE OF PROCESSED DATA ARCHIVES REACH THE END OF THEIR PROPRIETARY PERIODS AND BECOME PUBLICLY AVAILABLE. BESIDES IMPROVING THE QUALITY AND USABILITY OF THE 1.6X10^7 ASTEROID MEASUREMENTS IN THE PS1 DATABASE AND EXPANDING UPON THE CURRENT SDSS MOVING OBJECT CATALOG (SDSSMOC; LAST UPDATED IN 2007) THIS PROJECT WILL EXPLOIT THE VAST QUANTITY OF PUBLICLY AVAILABLE ARCHIVAL OPTICAL IMAGING DATA FROM LARGE TELESCOPES THAT WERE ORIGINALLY OBTAINED FOR NON-SOLAR SYSTEM SCIENCE AND HAVE THEREFORE NEVER BEEN SEARCHED FOR SOLAR SYSTEM OBJECTS. WE EXPECT TO EXTRACT DATA FOR ~2.5X10^7 NEW ASTEROID DETECTIONS FROM NON- PS1 SOURCES. MANY OF THESE WILL BE FROM TELESCOPES WITH APERTURES ~8 M IN SIZE (I.E. THE SIZE OF THE PLANNED LARGE SYNOPTIC SURVEY TELESCOPE OR LSST OR LARGER) WITH IMPLICATIONS FOR A WIDE RANGE OF SMALL SOLAR SYSTEM BODY SCIENCE. AS SUCH THIS PROJECT (AND POTENTIAL FUTURE UPDATES) HAS THE POTENTIAL TO HAVE A SIGNIFICANT IMPACT ON THE FIELD YEARS AHEAD OF THE START OF THE LSST SURVEY. THIS PROGRAM WILL GENERATE HIGHER-ORDER DATA PRODUCTS FROM CURRENTLY EXISTING ASTRONOMICAL OBSERVATIONS MOST OF WHICH WERE NOT INITIALLY INTENDED FOR USE FOR SOLAR SYSTEM SCIENCE RESEARCH AND AS SUCH IS WELL-SUITED FOR THE PDART PROGRAM. IT WILL INCREASE THE AMOUNT OF DATA PRODUCTS AVAILABLE FOR PLANETARY SCIENCE RESEARCH AND PRODUCE TOOLS THAT WILL ENABLE AND ENHANCE FUTURE SCIENTIFIC INVESTIGATIONS AS DESCRIBED IN THE PDART PROGRAM SOLICITATION. ALL DATA PRODUCTS FROM THIS PROGRAM WILL BE MADE PUBLICLY AVAILABLE VIA THE SMALL BODY NODE OF PDS WHILE ALL PIPELINE CODE SEARCH TOOL SOURCE CODE AND DOCUMENTATION WILL BE MADE PUBLICLY AVAILABLE VIA GITHUB.

VOLCANISM IS A DOMINANT PROCESS IN THE GEOLOGIC HISTORY OF MARS AND UNDERSTANDING THE GEOLOGIC EVOLUTION OF THE MAJOR MARTIAN VOLCANIC CENTERS IS CRI

TESTING ALTERNATIVE HYPOTHESES TO OLIVINE ON VESTA WITH MULTIPLE DATA FROM THE DAWN MISSION IMPLICATIONS ON ITS INTERNAL STRUCTURE ORIGIN AND EVOLUTION

SHARAD, THE SHALLOW RADAR INSTRUMENT ON THE MARS RECONNAISSANCE ORBITER MRO, PROVIDES THE FIRST LARGE VOLUMES OF CLOSELY SAMPLED SUBSURFACE SOUNDING

ON ROVING SAMPLE-RETURN OR CACHING MISSIONS, TWO CENTRAL TENSION WILL BE CHOOSING THE SAMPLES TO BE COLLECTED AND STORED (OR POTENTIALLY DISCARDED IN

ARCHIVING AND DISTRIBUTION OF HIGH-QUALITY CONTEXT CAMERA (CTX) DIGITAL TERRAIN MODELS FOR THE MARS RESEARCH COMMUNITY

GOALS AND OBJECTIVES. THE CASSINI MISSION PROVIDED US WITH 13+ YEARS OF OBSERVATION OF THE SATELLITES AND RINGS OF SATURN. TO DATE ONLY A SMALL SUBSET OF THIS HIGH-QUALITY DATA HAS BEEN ANALYZED IN DEPTH PRODUCING UNPRECEDENTED RESULTS THAT HAVE IMPROVED OUR UNDERSTANDING OF THE GIANT PLANET S SYSTEM. THE OBJECTIVE OF THE PROJECT WE ARE PRESENTING IS TO IMPROVE ACCESS TO THE DATA COLLECTED BY THE CASSINI ULTRAVIOLET IMAGING SPECTROGRAH (UVIS) BY THE PLANETARY COMMUNITY INCLUDING THE YOUNGEST GENERATION OF UPCOMING SCIENTISTS.

PHYLLOSILICATES DETECTED ON MARS USING VISIBLE/NEAR INFRARED (VNIR) SPECTROSCOPY CLEARLY POINT TO A HISTORY OF AQUEOUS ALTERATION WITH OBVIOUS RELEVA

THIS PROPOSAL SEEKS TO PRODUCE A USGS GEOLOGIC MAP OF CENTRAL NOCTIS LABYRINTHUS, IN ORDER TO EXPLORE AND CHARACTERIZE THE PITS, TROUGHS, AND PLATEAU

DAWN SHOWED THAT CERES GLOBAL REGOLITH CONTAINS ABUNDANT HYDROGEN IN THE FORM OF AQUEOUSLY ALTERED MINERALS SUBSURFACE WATER ICE AND POSSIBLY ORGANIC MATTER. THE SURFACE IS DOTTED WITH BRIGHT MATERIALS RICH IN SALTS AND HYDRATED MINERALS

MUTUAL EVENTS, A SERIES OF OCCULTATIONS AND ECLIPSES, OCCUR AS THE COMPONENTS OF A BINARY SYSTEM PASS IN FRONT AND BEHIND EACH OTHER AS VIEWED FROM T

WE WILL RE-VISIT THE MOON USING DATA ACQUIRED BY THE KOREA PATHFINDER LUNAR ORBITER (KPLO) GAMMA RAY SPECTROMETER (GRS) TO BETTER CHARACTERIZE SUBSURFACE GEOCHEMISTRY AS WELL AS IDENTIFY AND ASSESS POTENTIALLY USEFUL MINERALS FOR IN SITU RESOURCE

EXPLAINING THE APOLLO HEAT FLOW EXPERIMENT DRIFT THE PRIMARY OBJECTIVE OF THIS STUDY IS TO EXPLAIN A SECULAR TEMPERATURE DRIFT THAT HAS LED SOME OF

WE PROPOSE TO DEVELOP A SUITE OF TOOLS TO SIMULATE ANALYZE AND HELP INTERPRET COMA FEATURES PRESENT IN IMAGES OF COMETS. THESE SOFTWARE TOOLS WILL ASSIST SCIENTISTS TO CHARACTERIZE COMA PROPERTIES AND BY EXTENSION THE NUCLEI OF COMETS. A WIDE RANGE

21-LDAP21_2-0023 MAPPING OF SURFACE AND SUBSURFACE COLD TRAPS FOR ICE AND SUPERVOLATILES

REMOTE MEASUREMENT OF LUNAR HEAT FLOW FROM EARTH BASED RADIO ASTRONOMYSCIENTIFIC OBJECTIVES: THE PRIMARY OBJECTIVE OF THIS STUDY IS TO BETTER CONSTRAIN THE GEOTHERMAL HEAT FLUX FROM THE LUNAR INTERIOR USING VLA PASSIVE RADIO OBSERVATIONS OF THE LUNAR NEARSIDE. CURRENTLY WE HAVE ONLY TWO VALUES OF LUNAR HEAT FLOW FROM THE APOLLO 15 AND 17 MISSIONS WITH A POTENTIAL 3RD UPPER LIMIT MEASUREMENT FROM DIVINER LUNAR RADIOMETER (DIVINER) MEASUREMENTS NEAR THE LUNAR SOUTH POLE [SIEGLER ET AL. 2014 PAIGE ET AL. 2016]. USING C L AND P BAND (~6 21 AND 90CM WAVELENGTH) PASSIVE RADIO MEASUREMENTS OF THE LUNAR NEARSIDE WE CAN POTENTIALLY CONNECT THESE DATA TO CONSTRAIN THE LUNAR NEAR SIDE AT ~100KM RESOLUTION. AS IN THE APOLLO HEAT FLOW EXPERIMENTS (HFE) [E.G. LANGSETH ET AL. 1976] AND THE UPCOMING INSIGHT MISSION MEASUREMENTS OF THE TEMPERATURE GRADIENT AT DEPTH CAN BE USED TO CHARACTERIZE THE GEOTHERMAL HEAT PRODUCTION OF A PLANET. PASSIVE RADIO-WAVELENGTH MEASUREMENTS HAVE BEEN LONG SUGGESTED [E.G. KEIHM ET AL. 1975] AS A METHOD FOR CONSTRAINING THERMAL EMISSION (AND THEREFORE THE TEMPERATURE GRADIENT) FROM SEVERAL METERS BELOW THE SURFACE. HOWEVER A MAJOR SOURCE OF ERROR ON SUCH A MEASUREMENT IS THE EMISSION FROM THE NEAR SURFACE WHICH VARIES DIURNALLY WITHIN THE UPPER METER. SUCH LIMITATIONS HAVE LED TO LITTLE MORE BEING DONE ON THE TOPIC THAN FULL-DISC OBSERVATIONS IN THE 1960 S AND 70 S. WITH THE VLA AND ARECIBO WE CAN INCREASE THE RESOLUTION BY A FACTOR OF 30 POTENTIALLY MAPPING NEARSIDE HEAT FLOW TO 100KM RESOLUTION. NEW DATA FROM THE DIVINER AND CHANG E 1 AND 2 PASSIVE MICROWAVE RADIOMETERS NOW ALLOWS DETAILED CONSTRAINT ON THIS NEAR SURFACE EMISSION. THESE INSTRUMENTS HAVE REVOLUTIONIZED OUT UNDERSTANDING OF INFRARED AND MICROWAVE BRIGHTNESS TEMPERATURES OF THE UPPER ~1M OF THE LUNAR SURFACE (ASSUMING ~10 WAVELENGTHS PENETRATION). COMBINED WITH THERMAL MODELS DESIGNED TO REPRODUCE DIVINER TEMPERATURES WE SHOULD NOW BE ABLE TO CHARACTERIZE THIS NEAR SURFACE EMISSION PRECISELY ENOUGH TO CONSTRAIN EMISSION FROM DEPTH ALONE. METHODOLOGY: L-BAND(~21CM) AND P-BAND(~90CM) MEASUREMENTS WILL BE USED TO BACK OUT PHYSICAL TEMPERATURE AS A FUNCTION OF DEPTH ON THE MOON IN THE UPPER ~10M. L-BAND WILL COLLECT THERMAL EMISSION WITHIN THE UPPER ~2M P-BAND WITHIN THE UPPER ~9M. FOR A SYNTHESIS IMAGING INSTRUMENT LIKE THE VLA A SPATIAL DYNAMIC RANGE OF ~30-40 BEAMS IS TYPICAL MEANING THAT WE NEED A SPATIAL RESOLUTION OF ~45 . THIS CAN BE ACHIEVED AT P-BAND IN THE C-CONFIGURATION AND AT L-BAND IN THE D-CONFIGURATION. THIS WILL YIELD A PHYSICAL RESOLUTION OF ~100 KM ON THE SURFACE OF THE MOON. VLA IS NOT ABLE TO MAKE FULL LUNAR MAPS AT SHORTER WAVELENGTHS LEADING TO A DESIRE TO MAP C-BAND (~6CM) DATA WITH ARECIBO WHICH COINCIDENTALLY WILL ALSO BE ~30-35 BEAM SPOTS ACROSS THE MOON RESULTING IN A COMPARABLE MAP TO THE VLA LONG WAVELENGTH DATA. THIS WILL REQUIRE TWO SEPARATE OBSERVING CAMPAIGNS AT THE VLA AS THESE CONFIGURATIONS ARE CHANGED EVERY 4 MONTHS AND ONE CAMPAIGN AT ARECIBO. EACH CAMPAIGN WILL IDEALLY INVOLVE MEASUREMENTS AT 3 PHASES WITHIN THE LUNAR MONTH TO AID IN CHARACTERIZATION OF THE DIURNAL COMPONENT OF THERMAL EMISSION. MODELS OF SUBSURFACE TEMPERATURES AND HEAT FLUX WILL BE USED TO PRODUCE FORWARD MODELS OF THERMAL FLUX CONSISTENT WITH THE TELESCOPE(AND EXISTING DIVINER AND CHANG E) OBSERVATIONS. RELEVANCE TO THE NASA SOLAR SYSTEM OBSERVATIONS PROGRAM: SSO SOLICITS OBSERVATIONS AT ALL WAVELENGTHS INCLUDING RADIO THAT CONTRIBUTE TO THE UNDERSTANDING OF THE NATURE AND EVOLUTION OF THE SOLAR SYSTEM BODIES. CONSTRAINING THE INTERNAL HEAT PRODUCTION OF THE MOON WAS A DESIRED GOAL OF THE NASA PLANETARY DECADAL SURVEY AND SUCH A MEASUREMENT MAY BE A VALUABLE PRECURSOR TO THE PROPOSED LUNAR GEOPHYSICAL NETWORK LISTED IN THAT DOCUMENT.

WE PROPOSE TO QUANTITATIVELY EVALUATE ONE SPECIFIC MECHANISM FOR THE FORMATION OF LIQUID WATER ON PRESENT-DAY MARS THAT WE CONSIDER PARTICULARLY PROMISING: MELTING OF SEASONAL WATER FROST IN ALCOVES. IN AREAS WITHIN ALCOVES THAT ARE SEASONALLY SHADOWED WATER FROST WILLACCUMULATE AND WHEN THE SUN RISES AGAIN TEMPERATURE INCREASES RAPIDLY AND MAY MELT THE FROST. WE WILL USE HIRISE-STEREO DERIVED DIGITAL ELEVATION MODELS (DEMS) AND THREE-DIMENSIONAL MODELING OF SHADOWS SURFACE TEMPERATURE NEAR-SURFACE TEMPERATURES AND SUBLIMATION IN RSLALCOVES TO TEST THIS HYPOTHESIS. THE GOAL IS TO QUANTITATIVELY ASSESS THE FULL CYCLE OF FROSTACCUMULATION WARMING AND MELTING IN THESE LOCAL ENVIRONMENTS. THE INVESTIGATION WILL ANSWERTHE FOLLOWING PROFOUND QUESTION: CAN LIQUID WATER FORM BY MELTING OF SEASONAL FROST IN ALCOVES AT PRESENT-DAY MARS CONDITIONS? THE MODEL RESULTS WILL BE COMPARED TO A SUITE OF OBSERVATIONAL CONSTRAINTS. WE WILL TAKE THE MODEL SURFACE TEMPERATURE OUTPUT AND COMPARE IT TO 1) MEASURED RSL GROWTH/RETREAT TIMESCALES (AT WHAT TEMPERATURES ARE THE RSL CHANGING?) AND TO 2) FREEZING POINT DEPRESSIONCALCULATIONS FOR CHLORIDE PERCHLORATE AND SULFATE SOLUTIONS AND/OR BRINES. THE RESULTS OF THIS PROJECT WILL YIELD A MORE DETAILED PICTURE OF THE THERMAL STATE OF RSL AND AS A CONSEQUENCE WHAT FLUIDS THEY COULD BE COMPOSED OF. THIS WILL HELP ESTABLISH IF THEY ARE "SPECIAL REGIONS" OR ARE TOO SALTY TO SUPPORT LIFE AS WE KNOW IT (RUMMEL ET AL. 2014). THE PROPOSED RESEARCH FALLS WITHIN THE SCOPE OF THE HABITABLE WORLDS PROGRAM AS IT IDENTIFIES ANDCHARACTERIZES THE DISTRIBUTION OF POTENTIALLY HABITABLE ENVIRONMENTS ON MARS. THE "ASTROBIOLOGICAL POTENTIAL OF PAST OR PRESENT ENVIRONMENTS ON OR IN THE MARTIAN SURFACE ORSUBSURFACE" IS SPECIFICALLY MENTIONED IN THE PROGRAM CALL. ALTHOUGH PRIMARILY A SCIENCE DRIVEN INVESTIGATION THE PROJECT WILL ALSO GENERATE HIGHER-ORDER DATA PRODUCTS FROM NASA MISSIONS TO MARS (HIRISE DEMS) AND IT WILL LEAD TO FURTHER DEVELOPMENT AND DISSEMINATION OF SOFTWARE TOOLS.

COLLABORATIVE RESEARCH: FORMATION, STABILITY, AND DETECTION OF AMORPHOUS FERRIC SULFATE SALTS ON MARS

CATHERINE WEITZ/PLANETARY SCIENCE INSTITUTEGEOLOGIC MAPPING OF A PROPOSED MARS SCIENCE LABORATORY LANDING SITE IN SOUTHWESTERN MELAS CHASMATHE OB

THE ANALYSIS OF INTERPRETATION OF THE DEEP IMPACT EVENTTHIS IS A PROPOSAL TO USE THEORY MODELING E

THE PROPOSED WORK FOCUSES ON UNDERSTANDING THE EFFECT OF THERMAL CYCLING ON ICE AND ROCK IN PLANETARY ENVIRONMENTS BY DEVELOPING A MODEL RELATING THEIR THERMOMECHANICAL RESPONSE TO INDUCED DAMAGE AND CHANGES IN THEIR BULK PROPERTIES.

CLIMATE MODEL (GCM) MOLA TOPOGRAPHY A MODEL OF THE THERMAL EVOLUTION OF THE CRUST AND AN ADVANCED MODEL OF REGIONAL AND GLOBAL SUBPERMAFROST GROUNDWATER FLOW (BASED ON THE LATEST UNSTRUCTURED GRID (USG) IMPLEMENTATION OF THE US GEOLOGICAL SURVEY S GROUNDWATER MODELING SOFTWARE MODFLOW) TO INVESTIGATE THE EFFECTS OF A COLD EARLY CLIMATE ON THE EVOLUTION OF THE MARTIAN HYDROSPHERE THE FIRST ATTEMPT TO SIMULATE THE COMPLETE HYDROLOGIC CYCLE OF A COLD EARLY MARS. THIS IS WORK THAT IS BEING PURSUED IN COLLABORATION WITH CO-I ROBIN WORDSWORTH (HARVARD UNIVERSITY). THIS REVISED PROPOSAL IS BEING SUBMITTED BECAUSE OF MY TRANSITION FROM THE LUNAR AND PLANETARY INSTITUTE (LPI) TO THE PLANETARY SCIENCE INSTITUTE (PSI) AND INCLUDES A DISCUSSION OF THE TASKS I INTEND TO PURSUE AT PSI IN THE REMAINING TWO YEARS OF THIS GRANT (SECTION 2.1) AS WELL AS THE PROGRESS THAT WAS MADE AT LPI DURING THE GRANT S FIRST YEAR (SECTION 2.3). THIS PROPOSAL ALSO CONTAINS A REVISED BUDGET FOR YEAR S 2&3 (SECTION VII) THAT INCLUDES A CARRY-OVER OF UNSPENT FUNDS FROM THE FIRST YEAR AT LPI.

BALLISTIC TRANSPORT PROCESSES ON COMET NUCLEI MAY DRAMATICALLY ALTER THEIR SURFACE ACTIVITY AND GEOMORPHOLOGY. COMET 103P/HARTLEY 2 HAS A SMALL BILOBATE NUCLEUS WITH A HYPERACTIVE REGION AT THE TIP OF ITS SMALL LOBE AND TERRAINS OF VARYING DEGREES

SULFUR PLAYS A DOMINANT ROLE IN GEOCHEMICAL CYCLING ON MARS, PAST AND PRESENT. THEORETICAL, CHEMICAL, AND SPECTROSCOPIC EVIDENCE SUGGEST THAT ABUNDAN

INVESTIGATIONS OF TRANSVERSE AEOLIAN RIDGES ON MARSWE PROPOSE A FOUR-YEAR STUDY TO CONTINUE OUR RECENT WORK TO EXPLORE THE AGE, SEDIMENT SOURCE, AN

SCIENTIFIC OBJECTIVES: OSIRIS-REX CAN BE THOUGHT OF AS A THERMAL EXPERIMENT. THE SAMPLES RETURNED FROM ASTEROID BENNU WILL PRESERVE A UNIQUE INVENTORY OF SOLAR SYSTEM VOLATILE BUILDING BLOCKS CONTROLLED BY THE TEMPERATURE HISTORY OF ITS SURFACE AND INTERIOR. THERMAL REMOTE SENSING OF ITS SURFACE WILL CONSTRAIN COMPOSITION AND PHYSICAL MATURITY OF THE SURFACE AND MATERIALS WE WILL RETURN. TEMPERATURES CONTROL BENNU'S ORBITAL EVOLUTION. THE PRIMARY OBJECTIVE OF THIS OSIRIS-REX PARTICIPATING SCIENTIST PROJECT IS TO ADVANCE THE SCIENTIFIC ANALYSIS OF BENNU WITH THERMAL MODELING. USING 3D THERMAL MODELING TOOLS AND EXPERIENCE WITH THERMAL INFRARED IMAGERY AND LASER REFLECTANCE DATA FROM THE MOON MERCURY AND ITOKAWA WE WILL INVESTIGATE AND AID CURRENTLY PLANNED INVESTIGATIONS BY ADDRESSING: 1) STABILITY OF SURFACE AND INTERIOR VOLATILES INCLUDING POSSIBLE VOLATILE OUTGASSING 2) SURFACE AND SUBSURFACE THERMAL PROPERTIES INCLUDING SURFACE ROCK SIZE AND FRACTION AND SAMPLE SITE SELECTION AND 3) YARKOVSKY AND YORP ACCELERATIONS. THIS MODEL HAS HERITAGE IN THE LRO DIVINER LUNAR THERMAL MODEL (PAIGE ET AL. 2010; SIEGLER ET AL. 2014 2016) AND MESSENGER THERMAL MODEL (PAIGE ET AL. 2013). ON MERCURY AND THE MOON THIS MODEL HAS BEEN USED TO ANALYZE THERMAL PROPERTIES OF THE LUNAR SUBSURFACE AND VOLATILE STABILITY IN SHADOWED REGIONS NEAR THE POLES. IT HAS ALSO BEEN DEMONSTRATED FOR SMALLER 3D OBJECTS SUCH AS ASTEROID ITOKAWA AND HAS BEEN APPLIED TO EXAMINING THE YARKOVSKY EFFECT DUE TO ASYMMETRIC HEATING ON AIRLESS BODIES (ADLER ET AL. 2013 LPSC). WE WILL WORK WITH EXISTING TEAM THERMAL MODELS (CHOI ET AL. 2014) TO CREATE A UNIFIED MODEL FRAMEWORK. WE SEE THIS MODEL AS AN IDEAL SUPPORTING APPLICATION FOR THE OSIRIS-REX INSTRUMENT PACKAGE IN SEVERAL KEY WAYS: IT WILL UTILIZE SHAPE MODEL DATA FROM OLA AND OCAMS TO PRODUCE A GLOBAL THERMAL MAP OF SURFACE AND SUBSURFACE TEMPERATURES. THIS WILL ALLOW FOR MAPPING OF EXPECTED SURFACE THERMAL INERTIA AND IDENTIFICATION OF REGIONS OF POSSIBLE VOLATILE STABILITY. WE WILL WORK WITH OTES TO PROVIDE AREAS WHERE ANOMALOUS THERMAL PROPERTIES HAVE BEEN DETECTED. OTES WILL PROVIDE SURFACE TEMPERATURES BUT THE MODEL WILL ALLOW FOR A FULL THERMAL HISTORY LINKING SEPARATE MEASUREMENTS IN TIME. IT CAN ACT AS A BASELINE THERMAL CORRECTION FOR OVIRS OBSERVATIONS IF COINCIDENT OTES MEASUREMENTS ARE UNAVAILABLE. WE WILL WORK WITH TEAM MEMBERS STUDYING THE YARKOVSKY EFFECT AND HOW THEIR STUDIES MIGHT UTILIZE OUR MODEL RESULTS.

THIS PROPOSAL REQUESTS FUNDS FOR A NEW FOUR-YEAR INVESTIGATION TO EVALUATE THE GEOLOGIC AND HYDROLOGIC HISTORIES OF AN AREA ALONG THE EASTERN RIM OF

INVESTIGATIONS OF TERRESTRIAL AND PLANETARY LAVA FLOWS THE PROPOSED INVESTIGATION IS A STUDY OF LAVA FLOW MORPHOLOGY AND EMPLACEMENT PROCESSES UTIL

IO'S VOLCANIC ACTIVITY HELPS IT TO MAINTAIN A TENUOUS ATMOSPHERE. IN A CLASSIC "CHICKEN AND EGG" PROBLEM, IONS IN IO'S ATMOSPHERE ARE PICKED UP BY JU

SCOTT C. MEST IS A SENIOR SCIENTIST AT THE PLANETARY SCIENCE INSTITUTE (PSI) AND IS AN EXPERT IN GEOLOGIC MAPPING OF PLANETARY BODIES IN THE SOLAR SYSTEM INCLUDING THE MOON MARS VESTA AND CERES. DR. MEST WILL LEAD THE EFFORTS FOR ALL TASKS RELATED TO THE APOLLO 16 MISSION INCLUDING DIGITIZING THE PRE-MISSION MAPS (0.08 FTE YEAR 1) AND CREATING UPDATED USGS SIM MAPS FOR APOLLO 16 (0.15 0.23 0.23 FTE IN YEARS 1-3). CO-I MEST IS REQUIRED TO ATTEND AND PRESENT RESULTS IN YEARS 1 2 AND 3 AT THE ANNUAL PLANETARY GEOLOGIC MAPPERS MEETING (0.02 FTE EACH YEAR). THE MEETING IS NORMALLY HELD AT THE USGS FACILITY IN FLAGSTAFF AZ. THERE IS NO CONFERENCE FEE FOR THIS MEETING. THE AUTO RENTAL IS NECESSARY TO TRAVEL FROM PHOENIX AIRPORT TO FLAGSTAFF. HE WILL PRESENT RESULTS OF THE PROJECT WITH PI GARRY AT LPSC MEETING IN YEAR 3 ONLY ONCE ALL THE MAPS ARE COMPLETE (0.02 FTE IN YEAR 3). R. AILEEN YINGST IS A SENIOR SCIENTIST AT THE PLANETARY SCIENCE INSTITUTE (PSI) AND IS AN EXPERT IN GEOLOGIC MAPPING OF PLANETARY BODIES IN THE SOLAR SYSTEM INCLUDING THE MOON MARS AND VESTA. SHE WILL LEAD EFFORTS RELATED TO MAPPING THE APOLLO 17 MISSION DATA. THIS WILL INCLUDE: 1. DIGITIZE THE PRE-MISSION AND POST-MISSION MAP OF THE APOLLO 17 LANDING SITE (TASK 1: 0.08 FTE YEAR 1) 2. CREATE UPDATED USGS SIM MAPS FOR APOLLO 17 (TASK 2: 0.15 0.23 0.23 FTE YEARS 1-3) 3. PRESENT RESULTS AT PLANETARY MAPPERS AND LUNAR AND PLANETARY SCIENCE CONFERENCE MEETINGS (0.02 0.02 0.04 FTE).

OBSERVATIONAL CHARACTERIZATION OF ACTIVE MAIN-BELT COMETS AND MAIN-BELT COMET NUCLEI WE PROPOSE A MULTI-YEAR OPTICAL OBSERVATIONAL CAMPAIGN TO CHARAC

ALTHOUGH THERE ARE A NUMBER OF FLUVIAL LANDFORMS PRESERVED IN INVERTED RELIEF ON MARS, FURTHER STUDY IS NEEDED TO UNDERSTAND THE SEQUENCE OF EVENTS A

SCIENTIFIC OBJECTIVES PIT CRATERS ARE A UBIQUITOUS SURFACE FEATURE ON MANY ASTEROIDS VISITED BY SPACECRAFT. PIT CRATERS PRESENT AS LINEAR CHAINS OF SIMILARLY SIZED OFTEN OVERLAPPING CRATERS AND ARE FREQUENTLY ASSOCIATED WITH VISIBLE RIDGES OR

PLANETARY IMPACT EJECTA AND THE PHYSICO-CHEMICAL EVOLUTION OF EXPANSION PLUMES: A MULTIDISCIPLINARY APPROACHWE PROPOSE A MULTIDISCIPLINARY PROJECT T

THE PROPOSED INVESTIGATION INCLUDES DETAILED MORPHOLOGIC AND TOPOGRAPHIC ANALYSES OF A SERIES OF VOLCANIC FEATURES ON THE SURFACE OF MARS USING HIRIS

MULTICOMPONENT CHEMICAL SYSTEMS IN MULTIPLE PHASES ARE UBIQUITOUS IN CELESTIAL BODIES. THE PROPERTIES AND BEHAVIOR OF THE SYSTEMS ARE OFTEN KEYS TO P

STEPPED FANS ARE RELATIVELY RARE ON BOTH EARTH AND MARS, AND THEIR FORMATION MECHANISMS ARE POORLY UNDERSTOOD, YET THESE LANDFORMS HAVE THE POTENTIAL

THE PURPOSE OF OUR PROPOSED WORK EFFORT IS TO TEST THE HYPOTHESIS THAT IN SITU SEGREGATION AND RESULTANT FROST HEAVE HAVE CONTRIBUTED SUBSTANTIALLY TO OBSERVED EXCESS ICE IN THE UPPER METER OF THE MARTIAN REGOLITH. WE WILL FOCUS ON NUMERICAL SIMULATIONS OF THE DEVELOPMENT OF ICE LENSES WITH THE GOAL OF ESTIMATING THE VOLUME OF EXCESS ICE THAT CAN BE PRODUCED IN THIS FORM DURING THE PAST 1-4 MA OF MARTIAN HISTORY IN TWO SPECIFIC REGIONS WHERE THE ORIGIN OF EXCESS ICE IS DEBATED: THE PHOENIX LANDING SITE AND MID-LATITUDE FRESH CRATER SITES IN UTOPIA PLANITIA. OBSERVATIONS OF EXCESS ICE IN THESE LOCATIONS ARE DISTINCT FROM ONE ANOTHER. ASSESSING THE CONTRIBUTION OF FROST HEAVE AT EACH LOCATION WILL SHED LIGHT ON THE RELATIVE IMPORTANCE OF ALL THREE HYPOTHESES FOR EXCESS ICE PRODUCTION IN DIFFERENT GEOGRAPHIC REGIONS OF MARS.

UNDERSTANDING THE FORMATION AND EVAOLUTION OF LOBATE DEBRIS APRONS IS OF CRITICAL IMPORTANCE TO MARTIAN CLIMATOLOGY BECAUSE THEY LIKELY REPRESENT THE

DERIVATION OF SUSPENDED SEDIMENT LOADS OF GLACIER-FED ANDEAN LAKES RESERVOIRS AND RIVERS: APPLICATIONS FOR HAZARDS AND WATER QUALITY.

TIDAL STRESSES AND HEATING PRODUCED BY ENCELADUS' ORBITAL AND ROTATIONAL DYNAMICS PLAY AN IMPORTANT ROLE IN THE FORMATION OF THE LARGE FRACTURES IN T

WE PROPOSE TO STUDY THE ROLE OF WAVE DYNAMICS ON THE ORIGIN AND EVOLUTION OF HOT JUPITERS. THIS WORK WILL ADDRESS HOW ANGULAR MOMENTUM TRANSPORT BY TIDALLY AND CONVECTIVELY DRIVEN WAVES AFFECTS THE ORBITAL EVOLUTION AND OBSERVATIONAL INFERENCES OF HOT JUPITERS. WE WILL USE TWO (2D) AND THREE (3D) DIMENSIONAL NONLINEAR HYDRODYNAMIC SIMULATIONS TO UNDERSTAND: 1) ANGULAR MOMENTUM TRANSPORT BY CONVECTIVELY DRIVEN WAVES WITHIN STARS AND HOW THESE WAVES AFFECT STELLAR ROTATIONAL EVOLUTION 2) THE INTERACTION OF TIDALLY-INDUCED WAVES WITH CONVECTIVELY-GENERATED WAVES AND HOW THEIR MUTUAL DISSIPATION AFFECTS THE ORBITAL EVOLUTION OF HOT JUPITERS AND 3) HOW THIS COMBINED ANGULAR MOMENTUM TRANSPORT AFFECTS THE OBSERVATIONAL INFERENCES OF THE EVOLUTION OF PLANETARY ORBITAL PROPERTIES. SPECIFICALLY THESE STUDIES WILL SHED LIGHT ON THE OBSERVED DICHOTOMY BETWEEN THE OBLIQUITY OF PLANETS AROUND HOT STARS VERSUS THOSE AROUND COOL STARS AND WILL PROVIDE AN ESTIMATE FOR THE TIDAL DISSIPATION FUNCTION Q FOR EXOPLANETS' HOST STARS. IN ORDER TO TEST OUR MODELS WE WILL MAKE OBSERVATIONAL PREDICTIONS WHICH MAY BE CHECKED WITH EXISTING DATA FROM NASA'S KEPLER MISSION AND FORTHCOMING SEARCHES FROM THE TESS MISSION AS WELL AS GROUND-BASED FOLLOW-UP RADIAL VELOCITY OBSERVATIONS.

COLLABORATIVE RESEARCH: A COORDINATE-FREE FRAMEWORK FOR IMPROVING EDDY PARAMETERIZATIONS -THIS PROJECT IS TO CREATE AND APPLY A NEW THEORETICAL FRAMEWORK FOR DEVELOPING AND ASSESSING PARAMETERIZATIONS OF EDDY TRANSPORT IN NUMERICAL MODELS. THE FRAMEWORK CONSTITUTES A SET OF PRINCIPLES LINKING PHYSICAL MEANING TO PARAMETERIZATION FORM, INCLUDING EXTANT AS WELL AS YET-UNFORMULATED VARIATIONS. THIS WORK WILL PROVIDE AN AVENUE FOR THE CROSS-EVALUATION OF EXISTING OR PROPOSED PARAMETERIZATIONS FROM FIRST PRINCIPLES. TWO SIGNIFICANT SOFTWARE PACKAGES THAT WILL RESULT FROM THIS WORK ARE (I) SYMBOLIC ALGEBRA SOFTWARE FOR IMPLEMENTING EDDY PARAMETERIZATIONS IN AN ARBITARY MODEL COORDINATE SYSTEM AND CHOICE OF DISCRETIZATION, AND (II) NUMERICAL CODE FOR ERROR DIAGNOSTICS IN MODEL IMPLEMENTATION. THE EXPLICIT, STOCHASTIC, COORDINATE-INDEPENDENT (ESC) FRAMEWORK WILL INCORPORATE: (I) EXPLICIT AND RIGOROUS DEFINITIONS FOR FILTERING AND AVERAGING OPERATIONS; (II) A FLEXIBLE APPROACH TO STOCHASTIC MODELING THAT RELAXES THE UNREALISTIC CONSTRAINTS IMPLICIT IN EXISTING PARAMETERIZATIONS ON EDDY PATH SMOOTHNESS AND DEPENDENCE ON LOCAL CONDITIONS; AND (III) THE USE OF COORDINATE-INDEPENDENT REPRESENTATIONS TO EXPRESS THE PHYSICAL ESSENCE OF PARAMETERIZATIONS FREE FROM CHOICE OF MODEL GEOMETRY. THIS WORK WILL CLARIFY THE LINK BETWEEN PARAMETERIZATION FORMS AND CONSERVED PROPERTIES (ENERGY, ENSTROPHY, ETC.); SPEED THE IDENTIFICATION AND ASSESSMENT OF DISCRETIZATION ERRORS IN MULTIPLE MODEL SYSTEMS; UNIQUELY IDENTIFY THE ADVECTIVE AND DIFFUSIVE COMPONENTS OF PARAMETERIZED FLUXES ACROSS IMPLEMENTATIONS; AND ACCOUNT FOR THE IMPACT OF THE OBSERVED RANGE OF HIGH-FREQUENCY TRAJECTORY BEHAVIOR ON PARAMETERIZATION STRUCTURE. THIS AWARD REFLECTS NSF'S STATUTORY MISSION AND HAS BEEN DEEMED WORTHY OF SUPPORT THROUGH EVALUATION USING THE FOUNDATION'S INTELLECTUAL MERIT AND BROADER IMPACTS REVIEW CRITERIA.

THE PRIMARY OBJECTIVE OF THIS WORK IS TO CHARACTERIZE THE EXTENT, COMPOSITION, ERUPTION STYLE, AND GEOLOGIC SETTING OF LUNAR DARK MANTLE DEPOSITS (DM

RELAXATION OF SMALL CRATERS AT PHOENIX LANDING SITE LATITUDES TESTING THE THIN PERMAFROST LAYER AND RAPID RELAXATION RATES HYPOTHESES. THE OBJECTIVE

WE PROPOSE TO EVALUATE THE GLOBAL GEOLOGY OF CERES WHERE IMPORTANT SPATIAL AND TEMPORAL RELATIONSHIPS BETWEEN GEOLOGIC AND ICE-DRIVEN PROCESSES ARE L

STRONG EVIDENCE SUGGESTS THAT LIQUID WATER MUST HAVE PLAYED AN IMPORTANT ROLE IN THE EVOLUTION AND CURRENT STATE OF CERES, THE LARGEST ASTEROID AND O

UNDERSTANDING FREE NORMAL MODES AND IRREGULAR STRUCTURES ON THE EDGES OF SATURN'S RINGS THE PURPOSE OF THIS PROPOSAL IS TO INVESTIGATE A NUMBER OF QU

TWO MAIN SOURCES HELP PRODUCE THE AIRGLOW THAT THE CASSINI-ULTRAVIOLET IMAGING SPECTROGRAPH (UVIS) INSTRUMENT OBSERVED IN TITAN S UPPER ATMOSPHERE. THE SOLAR XUV RADIATION IS THE MAIN SOURCE OF DAYGLOW WHILE MAGNETOSPHERIC PARTICLE PRECIPITATION PRINCIPALLY ACT ON THE NIGHTSIDE OF THE SATELLITE. ONE OF THE QUESTIONS THAT MIGHT STAY UNANSWERED AFTER THE END OF THE CASSINI MISSION CONCERNS THE ROLE AND QUANTIFICATION OF THE MAGNETOSPHERIC PARTICLE PRECIPITATION AND OTHER MINOR SOURCES SUCH AS MICROMETEORITE PRECIPITATION AND/OR COSMIC GALACTIC RAY. THE CASSINI-UVIS DATASET CONTAINS MORE THAN 10 000 OBSERVATIONS OF TITAN REALIZED WITH THE FAR-UV (FUV) AND EXTREME-UV (EUV) CHANNELS OF THE INSTRUMENTS AND DATA WERE CONTINUOUSLY ACQUIRED DURING THE 126 TITAN FLYBYS THAT THE CASSINI MISSION ACCOMPLISHED. THUS AT THE END OF THE MISSION WE HAVE AVAILABLE ALMOST 13 YEARS OF TITAN OBSERVATION IN THE UV WHICH REPRESENTS A LITTLE LESS THAN THE HALF OF A SATURN YEAR. TITAN HAS BEEN OBSERVED DURING VARIOUS SOLAR WIND AND MAGNETOSPHERIC CONDITIONS BUT TO DATE STILL VERY LITTLE OF THE UVIS DATA SET HAS BEEN ANALYZED AND EXPLORED. TREMENDOUS AMOUNT OF INFORMATION IS WAITING TO BE EXTRACTED. THE BEST EXAMPLE OF THIS SITUATION IS THE T32 FLYBY ON JUNE 13 2007 WHERE TITAN HAS BEEN OBSERVED BY UVIS AS WELL AS BY ALL IN-SITU INSTRUMENTS ONBOARD THE CASSINI SPACECRAFT. WHILE RESULTS CONCERNING THE T32 MAGNETOSPHERIC ENVIRONMENT HAVE BEEN LONG PUBLISHED BY ALL IN-SITU INSTRUMENT TEAMS NOBODY LOOKED AT THE UVIS DATA ON THIS PARTICULAR DAY UNTIL RECENTLY. ABSTRACTS AND PAPER PUBLISHED BY ROYER ET AL. DEMONSTRATED THAT ON T32 THE UVIS INSTRUMENT OBSERVED AN INTENSE RESPONSE FROM TITAN IONOSPHERE TO AN ELECTRON BURST OBSERVED BY THE CASSINI PLASMA SPECTROMETER (CAPS) IN-SITU INSTRUMENT. THIS PROJECT PRESENTED HERE INTENDS TO CORRELATE FURTHER REMOTE-SENSING AND IN-SITU OBSERVATIONS OF TITAN IN ORDER TO BETTER UNDERSTAND TITAN IONOSPHERIC RESPONSE TO ITS ENVIRONMENT AND WILL ENSURE THAT THE FULL POTENTIAL OF THE UVIS DATASET WILL BE USED. INVESTIGATION ON ATMOSPHERIC ESCAPE WILL ALSO BE PERFORMED. APPROACH AND METHODOLOGY THE WORK WILL PRIMARILY RELY ON THE TITAN UVIS LIBRARY WHICH CONSISTS IN A DATABASE OF UVIS DETECTOR IMAGES ALLOWING FOR A RAPID DETERMINATION OF THE PRESENCE OR NOT OF AN AIRGLOW IN TITAN S UPPER ATMOSPHERE. THE PROJECT WILL ALSO INCORPORATE ALL CAPS PUBLICLY AVAILABLE DATA. ON MOST OCCASIONS IN-SITU AS WELL AS REMOTE SENSING INSTRUMENTS SIMULTANEOUSLY MONITOR THE SATURNIAN ENVIRONMENT. USING PATTERN RECOGNITION ALGORITHMS WE WILL SEARCH FOR ENHANCED AIRGLOW IN THE UVIS DATA AND HIGH ELECTRON ENERGIES IN THE CAPS DATASET. IN ADDITION THE RELATIONSHIP BETWEEN THE SATURN LOCAL TIME AND TITAN AIRGLOW CHARACTERISTICS WILL BE EXPLORED. CAPS DATA WILL BE USED TO CORRELATE THE ELECTRON FLUX AND POTENTIAL PRESENCE OF IONS IN THE VICINITY OF THE SPACECRAFT WITH THE AIRGLOW CHARACTERISTICS AND THE AIRGLOW PATTERNS DETECTED BY UVIS. SCOPE OF THE PROGRAM AS STATED IN THE FULL ROSES 2018 THIS CDAP PROGRAM SOLICITS RESEARCH PROPOSALS TO CONDUCT SCIENTIFIC INVESTIGATIONS UTILIZING DATA OBTAINED BY THE CASSINI MISSION . WE WILL CONDUCT A SCIENTIFIC INVESTIGATION AS MANDATED AND WILL COMBINED DATA FROM TWO INSTRUMENTS (UVIS AND CAPS) ONBOARD THE CASSINI SPACECRAFT. OUR APPROACH IS NOVEL IN THE SENSE THAT IN-SITU AND REMOTE SENSING INSTRUMENTS ARE RARELY PART OF A SAME STUDY. THE GOAL OF THIS PROJECT IS THE PROVIDE A BETTER UNDERSTANDING OF THE INTERACTIONS BETWEEN TITAN S UPPER ATMOSPHERE AND ITS DIRECT MAGNETOSPHERIC ENVIRONMENT.

GEOPHYSICAL CHARACTERIZATION OF SURFACE AND NEAR-SURFACE STRUCTURE ON VENUS WITH VENSAR

THIS PROPOSAL DIRECTLY ADDRESSES THE GOALS OF THE EMERGING WORLDS PROGRAM AS DESCRIBED IN APPENDIX C.2 OF ROSES 2017. THE WORK WILL ENHANCE THE FUNDAMENTAL SCIENCE QUESTION OF HOW THE SOLAR SYSTEM FORMED AND EVOLVED.

ONE OF THE MOST EXCITING DISCOVERIES BROUGHT ABOUT DURING THE LAST HALF A CENTURY OF SOLAR SYSTEM EXPLORATION IS THAT MARS WAS A HYDROLOGICALLY ACTIVE EARTH-LIKE PLANET. PARTICULARLY SIGNIFICANT IS THE FINDING THAT AN OCEAN PROBABLY OCCUPIED THE MARTIAN NORTHERN PLAINS ~3.4 GA. THIS HYPOTHESIS HAS BEEN THE SUBJECT OF DEBATE AND SCRUTINY FOR NEARLY HALF A CENTURY. PART OF THE CONTROVERSY STEMMED FROM THE OBSERVATION THAT THE PROPOSED PALEO-OCEANIC BASIN LACKS AN APPRECIABLE CONTINUITY OF PALEO-SHORELINE FEATURES. A RECENT INVESTIGATION SUGGESTS THAT THE EMPLACEMENT AND LONG-TERM PRESERVATION OF MEGATSUNAMI DEPOSITS OVER THE PLANET S ANCIENT COASTAL ENVIRONMENTS COVERED THE PALEOSHORELINES HENCE EXPLAINING THEIR ABSENCE (HTTPS://WWW.NATURE.COM/ARTICLES/SREP25106). THIS INVESTIGATION DOCUMENTS TWO POSSIBLE MEGATSUNAMI DEPOSITS A YOUNGER ONE WHICH SHOWS EVIDENCE OF BACKWASH CHANNELS OVER DEBRIS LOBATE FRONTS. AN OLDER ONE LACKING EVIDENCE OF BACKFLOW AND SHOWING DOMINANTLY ICY COMPOSITIONS PERHAPS BECAUSE THE WAVES FROZE DURING THEIR RUN-UP INTO THE HIGHLANDS. THE OLDER AND A YOUNGER MEGATSUNAMI RESPECTIVELY EXTENDED FROM PALEOSHORELINES AT THE -3 800 M AND -4 100 M ELEVATIONS. A FUNDAMENTAL INTERPRETATION IN THE ARTICLE IS THAT MARS EXPERIENCED GLOBAL PALEOCLIMATIC COOLING DURING THE OCEANIC REGRESSION PHASE. THE EVOLUTION OF THE OCEAN S COASTAL ENVIRONMENTS WHICH IS RELEVANT TO THE UNDERSTANDING OF MARS PALEOCLIMATIC EVOLUTION AND POTENTIAL HABITABILITY REMAINS MOSTLY UNKNOWN. HERE WE PROPOSE TO MAP THE DISTRIBUTION OF ALL POTENTIAL TSUNAMI-RELATED LANDFORMS THROUGHOUT THE ENTIRE NORTHERN PLAINS AND THE INTERIOR LOWER FLANKS OF ELYSIUM MONS. WE WILL USE OUR MAPPING TO ESTABLISH SPATIAL AND TEMPORAL RELATIONSHIPS THAT WILL ALLOW US TO INVESTIGATE THE EVOLUTION OF THE NORTHERN OCEAN AND ADD DETAIL TO THE RODRIGUEZ ET AL. (2016) PALEOCLIMATIC RECONSTRUCTION. WAVE HEIGHT AND OTHER HYDRODYNAMIC CHARACTERISTICS WILL BE DETERMINED USING NUMERICAL SIMULATIONS WHICH ALSO GENERATE COASTAL INUNDATION DISTANCES AND BACKWASH PATTERNS. WE WILL COMPARE THESE SIMULATION OUTPUTS TO THE MAPPING RESULTS TO FIND THE BEST MATCHING CASES AND PROVIDE REASONABLE GEOLOGIC RECONSTRUCTIONS OF THE TSUNAMI EVENTS. WE WILL USE OUR MAPPING OF MEGATSUNAMI FEATURES FOR PALEOSHORELINE RECONSTRUCTION WHICH WILL ALLOW US TO INVESTIGATE THE COASTAL PALEOENVIRONMENTS FORMED DURING OCEANIC REGRESSION. THESE RESULTS WILL ALLOW US TO ASSESS THE MARTIAN OCEAN S LONGEVITY AND THE PALEOCLIMATIC CONDITIONS UNDER WHICH IT EXISTED. THESE RESULTS ARE RELEVANT TO CURRENT PALEOCLIMATIC MODELING EFFORTS AND THE SEARCH FOR GEOLOGIC MATERIALS THAT MIGHT RETAIN FORMER LIFE EVIDENCE. TO THIS END WE WILL IDENTIFY ASTROBIOLOGICALLY SIGNIFICANT TSUNAMI DEPOSITS BY COMBINING OUR MAPPING AND NUMERICAL SIMULATIONS TO ESTABLISH THE DISTRIBUTION OF TSUNAMI DEPOSITS THAT ARE MOSTLY COMPOSED OF ERODED OCEAN FLOOR MATERIALS. THIS PROPOSAL ADVANCES THE MDAP OBJECTIVE "TO ENHANCE THE SCIENTIFIC RETURN FROM MISSIONS TO MARS CONDUCTED BY NASA AND OTHER SPACE AGENCIES". THE METHODOLOGY PROPOSED IS DOMINATED BY THE ANALYSIS AND INTERPRETATION OF RELEASED MARS SPACECRAFT DATA SPECIFICALLY FROM THE NASA MARS GLOBAL SURVEYOR MARS ODYSSEY AND MARS RECONNAISSANCE ORBITER MISSIONS AS WELL AS ESA MARS EXPRESS. OUR PROPOSED INVESTIGATION WILL PROVIDE INSIGHTS INTO THE HISTORY OF TSUNAMI-DRIVEN COASTAL RESURFACING IN EARLY MARS OCEANS. OUR ANALYSIS OF SURFACE GEOMORPHOLOGIC FEATURES WITHIN THE PROPOSED TSUNAMI DEPOSITS WILL IMPROVE OUR UNDERSTANDING OF CLIMATE CHANGE IN THE PLANET S EARLY HISTORY AND IDENTIFY AREAS OF ASTROBIOLOGICAL INTEREST FOR FUTURE MARS MISSIONS. THUS IT IS IN DIRECT SUPPORT OF THE GOALS OUTLINED BY MDAP AND THE DECADAL SURVEY PARTICULARLY THOSE RELATING TO GEOLOGICAL PROCESSES THE DISTRIBUTION OF WATER SURFACE-ATMOSPHERE INTERACTIONS HABITABILITY AND CLIMATE.

22-PDAR22-0001 A GEOLOGIC MAP OF ARAM CHAOS: A COMMUNITY RESOURCE TO FACILITATE FUTURE SCIENTIFIC INVESTIGATIONS ON MARS

CARBON DIOXIDE LEVITATION: A NEW GEOMORPHIC PROCESS SUBLIMATION OF MARS' SEASONAL CO2 ICE CAP CAUSES GEOMORPHOLOGIC CHANGES ON THE SURFACE OF MARS IN

THE SOLAR SYSTEM IS HOME TO THE ONLY KNOWN INHABITED PLANET, AND THE HISTORY OF ITS PLANETS PROVIDES INSIGHTS INTO PLANETARY HABITABILITY. OUR SOLAR

ONE OF THE REMARKABLE DISCOVERIES BY THE DAWN MISSION AT CERES ARE PERENNIALLY SHADOWED REGIONS (PSRS) AND BRIGHT (ICE) DEPOSITS WITHIN THEM. THE PSRS CAN BE DELINEATED BY COMPUTATIONAL RAY-TRACING BASED ON AVAILABLE TOPOGRAPHIC MODELS AND AS THE

CONSTRAINING THE AQUEOUS HISTORY OF MERIDIANI PLANUM THROUGH INVESTIGATION OF SMALL-SCALE VALLEY NETWORKS AND LACUSTRINE DEPOSITS--A WINDOW INTO ANCI

IMPACT CRATERING ON MARS: HYDROTHERMAL SYSTEMS, EJECTA, AND RAMPARTS

"ANALYSIS AND CHARACTERIZATION OF PHOSPHATES USING MULTIPLE SPECTRAL TECHNIQUES" PHOSPHATE MINERALS OCCUR ON MARS AS EVIDENCED BY THEIR PRESENCE IN M

RADAR INVESTIGATIONS HAVE REVEALED THAT CARBON DIOXIDE ICE DEPOSITS EXIST AT THE SOUTH POLAR LAYERED DEPOSITS (SPLD) OF MARS. THE CO2 IS SPREAD ACROSS MULTIPLE UNITS EACH MADE UP OF TWO OR THREE LAYERS SEPARATED BY WATER ICE BOUNDING LAYERS. THEY MEASURE UP TO 1 KM THICK AND ARE COVERED BY THIN LAYERS OF WATER AND CO2. MEASUREMENTS OF SURFACE TOPOGRAPHY ALONG WITH SURFACE FEATURES THAT RESEMBLE CREVASSES SUPPORT THE INTERPRETATION THAT THESE DEPOSITS HAVE UNDERGONE OR CURRENTLY UNDERGO VISCOUS FLOW IN THE FORM OF DRY ICE GLACIERS. GLACIAL MODELING IS AN EFFECTIVE WAY TO CONSTRAIN FLOW RATES BASAL FRICTION GEOTHERMAL FLUX AND MORE (POTENTIALLY DEPOSITIONAL AND THUS CLIMATIC HISTORY) BUT THE CURRENT STATE OF THE LITERATURE DOES NOT PROVIDE THE NECESSARY INPUTS FOR CO2 ICE RHEOLOGY OR FOR THE PHYSICAL STATE OF THE GLACIERS THEMSELVES ESPECIALLY RELATED TO THE BOUNDING LAYERS. IN ORDER TO SUCCESSFULLY MODEL THE GLACIERS IN 3D THOSE MEASUREMENTS MUST BE MADE. SCIENTIFIC GOALS: WE AIM TO BETTER CONSTRAIN THE FLOW OF CO2 ICE IN MARTIAN CONDITIONS WITH LABORATORY STUDIES OF CO2 ICE RHEOLOGY. THE EVENTUAL AIM IS TO DETERMINE WHEN THE ICE FLOWED AND FOR HOW LONG. THIS IN TURN WILL HELP CONSTRAIN THE PERIODS OF DEPOSITION OF CO2 ICE REVEALING IMPORTANT EVENTS IN THE RECENT CLIMATIC HISTORY OF MARS.

WE PROPOSE TO CONDUCT A SYSTEMATIC SURVEY OF CRISM DATA IN THE CIRCUM-HELLAS REGION, WITH EMPHASIS ON THE BETTER-PRESERVED NW HELLAS IN ORDER TO IDEN

WE PROPOSE TO CARRY OUT A COMPREHENSIVE ANALYSIS OF GAS AND DUST FEATURES IN THE COMA OF THE NASA EPOXI MISSION TARGET, COMET 103P/HARTLEY 2. OUR GRO

THE STABILITY OF MAGNETIC FLUX ROPES: BRIDGING OBSERVATIONS AND EXPERIMENTS WITH SIMULATIONS

THE PRIMARY OBJECTIVE OF THIS FOUR-YEAR STUDY IS TO DEVELOP A GREATER UNDERSTANDING OF THE GEOLOGIC HISTORY OF THE PORTION OF XANTHE TERRA SURROUNDIN

THE OVERALL OBJECTIVE OF THIS PROPOSAL IS TO CONSTRAIN THE EXTENT AND CAUSES OF SEDIMENTARY DEPOSITION AND AQUEOUS ALTERATION IN COPRATES CHASMA AND

SUBSURFACE MIGRATION OF WATER VAPOR ON AIRLESS BODIES

EXECUTE A BALANCED SCIENCE PROGRAM BASED ON DISCIPLINE-SPECIFIC GUIDANCE FROM THE NATIONAL ACADEMIES OF SCIENCES ENGINEERING AND MEDICINE ADMINISTRATION PRIORITIES AND DIRECTION FROM CONGRESS. PARTICIPATE AS A KEY PARTNER AND ENABLER IN THE AGENC

TOWARD A REALISTIC MODEL OF THE FORMATION OF TERRESTRIAL PLANETS AND WATER DELIVERY

IN OCTOBER 2008 A SMALL ASTEROID WITH AN F-TYPE REFLECTANCE SPECTRUM 2008 TC3 EXPLODED OVER THE NUBIAN DESERT AND DEPOSITED MATERIAL IN A STREWN FIELD IN NORTHERN SUDAN. SEARCHES TO-DATE HAVE LED TO COLLECTION OF>600 STONES THOUGHT TO BE DERIVED FROM 2008 TC3. THESE MATERIALS ARE NAMED ALMAHATA SITTA (AHS) AND REPRESENT THE FIRST RECOVERED METEORITE FROM A SPECTRALLY OBSERVED ASTEROID. THE DISCOVERY TRACKING SPECTRAL ANALYSIS AND RECOVERY OF MATERIAL FROM 2008 TC3/AHS WAS A REMARKABLE SERIES OF EVENTS AND A TESTAMENT TO THE BENEFITS OF CROSS-DISCIPLINARY AND INTERNATIONAL COOPERATION. BUT THE LIST OF REMARKABLE THINGS ABOUT THIS OBJECT DOES NOT END THERE. THE FIRST AHS SAMPLES STUDIED SHOWED AN ANOMALOUS TYPE OF MATERIAL BELONGING TO THE CLASS OF UREILITE METERORITES.UREILITES ARE ONE OF THE LEAST UNDERSTOOD CLASSES OF PRIMITIVE ACHONDRITES AND ARGUABLY ONE OF THE MOST IMPORTANT FOR UNDERSTANDING EARLY SOLAR SYSTEM PROCESSES THAT BRIDGE THE CHONDRITE-TO-ACHONDRITE TRANSITION. THUS THE ADVENT OF A NEW TYPE OF UREILITE POTENTIALLYPROVIDING NEW INFORMATION IN THE FORM OF FRESH UNWEATHERED MATERIAL IS CERTAINLY WELCOME. ENSUING STUDIES OF MORE SAMPLES SHOWED A GREAT DIVERSITY OF UREILITE MATERIALS LEADING TO CLASSIFICATION OF AHS AS AN ANOMALOUS POLYMICT UREILITE. EVEN MORE REMARKABLY HOWEVER ~20-30% OF THE RECOVERED CLASTS WERE FOUND TO BE NON-UREILITIC INSTEAD REPRESENTING A VARIETY OF DIFFERENT CHONDRITE TYPES.THUS 2008 TC3/AHS APPEARS TO BE A NEW TYPE OF BRECCIA UNLIKE ANY METEORITE KNOWN TO DATE. NEVERTHELESS THERE ARE STRONG INDICATIONS THAT 2008 TC3/AHS "NORMAL" POLYMICT UREILITES AND MAIN GROUP UREILITES SHARE A COMMONLINEAGE. WE HYPOTHESIZE THAT THE IMMEDIATE PARENT OF 2008 TC3/AHS WAS ALSO THE IMMEDIATE PARENT OF ALL UREILITIC MATERIAL THAT HAS BEEN SAMPLED IN RECENT TIMES BY METEORITES ON EARTH AND THAT USING 2008 TC3/AHS AS A STARTING POINT WE CAN TRACE THE HISTORY OF THISMATERIAL BACK THROUGH MANY STAGES OF SOLAR SYSTEM HISTORY TO ACCRETION OF THE ORIGINAL UREILITE PARENT BODY. THE GOAL OF THE PROPOSED RESEARCH IS TO BRING OUR COMBINED EXPERTISE IN UREILITE PETROLOGY AND GEOCHEMISTRY ACCRETION MODELING ASTEROID DYNAMICS AND CRATERING AND REGOLITH EVOLUTION TO BEAR ON 4 MAJOR STAGES IN THE HISTORY OF UREILITIC MATERIAL IN THE SOLAR SYSTEM: 1) ACCRETION AND EARLY DIFFERENTIATION; 2) PARENT BODY BREAKUP AND FORMATION OF OFFSPRING BODIES; 3) DYNAMICAL EVOLUTION OF UREILITIC ASTEROIDS; AND 4) DEVELOPMENT OF A COMPLEX REGOLITH ON THE 2008 TC3 PARENT.

THE SCIENTIFIC OBJECTIVES OF THIS PROPOSAL ARE: 1) UNDERSTAND THE GENERAL PHYSICAL PROPERTIES OF THE KEY GEOLOGICAL TERRAINS ON FOUR JUPITER FAMILY C

CONSTRAINING THE RELATIVE TIMING AND DURATION OF THESE AQUEOUS PERIODS BASED ON THE GEOLOGIC RECORD IS OF FUNDAMENTAL IMPORTANCE TO AN ACCURATE CHARACTERIZATION OF PAST CLIMATE CONDITIONS ON MARS. WHILE PAST RESEARCH HAS FOCUSED ON FLUVIAL LANDFORMS MAINLY VALLEY NETWORKS ALLUVIAL FANS ARE LANDFORMS THAT CAN PROVIDE INSIGHT INTO THIS CRITICAL QUESTION BECAUSE THEIR FLOW PROCESSES HAVE DISCRIMINABLE DIFFERENCES IN THE RESULTING DEPOSITS THAT CAN BE DIRECTLY TIED TO WATER VOLUME AND DURATION. DOCUMENTING THE DETAILED STRATIGRAPHIC CONTEXT OF ALLUVIAL FAN DEPOSITS GLOBALLY WILL IMPROVE OUR UNDERSTANDING OF THE RELATIVE TIMING OF CLIMATIC CONDITIONS. EXAMINATION OF THE GLOBAL RECORD OF ALLUVIAL FANS PROVIDES A TEST BETWEEN THE WARM WET AND THE COLD DRY CLIMATE HYPOTHESES AND WILL PROVIDE CLIMATE MODELERS WITH HARD CONSTRAINTS ON THE TIMING MAGNITUDE AND DURATION OF WARM-WET CONDITIONS. THE SYNTHESIS OF ORBITAL DATA (IMAGE TOPOGRAPHIC AND COMPOSITIONAL) WITH HYDRAULIC MODELING IN THIS INTERDISCIPLINARY INVESTIGATION IS CONSISTENT WITH THE SCIENTIFIC OBJECTIVES OF THE MARS DATA ANALYSIS PROGRAM (MDAP). IN ADDITION THIS INVESTIGATION ADDRESSES MULTIPLE MEPAG (2015) SCIENCE GOALS INCLUDING II.C2 (FIND AND INTERPRET PHYSICAL AND CHEMICAL RECORDS OF PAST CLIMATES AND FACTORS THAT AFFECT CLIMATE) AND III.A1 (IDENTIFY AND CHARACTERIZE PAST AND PRESENT GEOLOGIC ENVIRONMENTS AND PROCESSES RELEVANT TO THE CRUST). CONSTRAINING THE PALEO-HYDROLOGIC CONDITIONS AND TIMESCALES OF AQUEOUS ACTIVITY ASSOCIATED WITH ALLUVIAL FAN FORMATION AT SITES AROUND THE GLOBE CONTRIBUTES TO A BETTER UNDERSTANDING PAST CLIMATE CONDITIONS AND HABITABLE REGIONS. LARGE ALLUVIAL FANS IN MARTIAN HIGHLAND CRATERS HAVE BEEN INTERPRETED AS EVIDENCE OF A LATE-STAGE PERIOD OF FLUVIAL ACTIVITY BETWEEN EARLY HESPERIAN AND EARLY AMAZONIAN (3.7 TO 3.3 GYR). THUS LARGE ALLUVIAL FANS DOCUMENT DEPOSITIONAL CONDITIONS FOR A CRITICAL WINDOW IN MARS CLIMATE HISTORY WITH PROFOUND IMPLICATIONS FOR UNDERSTANDING THE PRESENCE LOCATION AND PERSISTENCE OF SURFACE HABITABLE ENVIRONMENTS. THE PROPOSED INVESTIGATION WILL CONDUCT MAPPING OF APPROXIMATELY 30 ALLUVIAL FAN SITES AROUND THE GLOBE TO DOCUMENT FLOW PROCESS AND STRATIGRAPHIC CONTEXT. HIGH RESOLUTION IMAGES FROM THE CTX HIRISE AND MOC INSTRUMENTS WILL BE USED TO DIFFERENTIATE SEDIMENT-GRAVITY FLOW DEPOSITS FROM FLUID-GRAVITY DEPOSITS AS WELL AS THE SUPERPOSITION RELATIONSHIPS BETWEEN DEPOSITS TO DEVELOP AN EVOLUTIONARY SEQUENCE. THE MINERALOGY IN FAN DEPOSITS DETERMINED IN SPECTRAL DATA WILL SHED INSIGHT ON FLOW RHEOLOGY AND COMPOSITION. HYDRAULIC MODELING OF FAN FLOWS WILL BE BASED ON THE GEOMORPHIC ANALYSIS UNDERPINNED BY TOPOGRAPHIC DATA FROM MOLA AND ELEVATION MODELS CONSTRUCTED FROM STEREO IMAGE PAIRS. ULTIMATELY THE EVOLUTIONARY SEQUENCE OF ALLUVIAL FANS WILL BE DETERMINED THROUGH THE COMBINED GEOLOGIC MAPPING AND MODELLING RESULTS.

OBSERVATIONS OF CURRENT AND PAST NASA COMETARY MISSION TARGETS\NWE WILL CARRY OUT GROUND BASED OPTIC

21-MSLPSP21_2-0038 UNDERSTANDING MG-SULFATE DISTRIBUTION HYDRATION STATE AND CRYSTALLINITY IN MT. SHARP

DUSTY RINGS IN THE SOLAR SYSTEM ARE BELIEVED TO MAINTAINED BY THE ONGOING COLLISIONS OF HIGH-SPEED DUST GRAINS INTO `RING-MOONS&#039; EMBEDDED WITHIN

SEVERAL LINES OF EVIDENCE INDICATE THAT CERES IS A WATER-RICH WORLD. ON THEORETICAL GROUNDS, SHALLOW ICE IS PREDICTED TO BE PRESENT AT DEPTHS OF 10-1

OBSERVATIONAL DATA OVER THE LAST DECADE UNAMBIGUOUSLY DEMONSTRATE THAT COMETS UNDERGO ROTATIONAL CHANGES AT TIMESCALES SMALLER THAN A SINGLE ORBIT, I

ASTEROID FAMILIES ARE GROUPINGS OF ASTEROIDS IN ORBITAL ELEMENT SPACE THAT FORMED FROM A SINGLE PARENT BODY AT SOME POINT IN THE PAST. THE THEMIS FAMILY HAS ATTRACTED PARTICULAR INTEREST IN RECENT YEARS. THREE CURRENTLY-KNOWN MAIN-BELT COMETS (MBCS) WHOSE ACTIVITY MAY BE DRIVEN BY THE SUBLIMATION OF VOLATILE ICE ARE THEMIS FAMILY MEMBERS. DETECTIONS OF SURFACE ICE ON TWO LARGE MEMBERS OF THE FAMILY HAVE ALSO BEEN REPORTED. SINCE ASTEROID FAMILY MEMBERS ARE BELIEVED TO BE COMPOSITIONALLY SIMILAR THESE FINDINGS INDICATE THAT ICE COULD BE WIDESPREAD WITHIN THE FAMILY. WE SEEK TO UNDERSTAND HOW ICE-BEARING OBJECTS FROM THE THEMIS FAMILY MIGHT BE DISTRIBUTED AND TRANSPORTED THROUGHOUT THE MAIN BELT AND TO THE NEAR-EARTH OBJECT POPULATION. THESE DYNAMICAL STUDIES WILL THEN BE COUPLED WITH THEORETICAL THERMAL MODELING TO UNDERSTAND THE FATE OF ICE IN THESE OBJECTS. TWO OF THE MBCS IN THE THEMIS FAMILY BELONG TO YOUNG (<10 MYR) SUB-FAMILIES. THIS IS INTRIGUING SINCE THE RECENT FORMATION OF SUBFAMILIES COULD BE A PLAUSIBLE MEANS FOR PRODUCING "FRESH" FRAGMENTS WHERE ICE LIES AT OR JUST BELOW THE SURFACE MAKING MBC-LIKE ACTIVITY MUCH MORE LIKELY. WE WILL CONDUCT A SYSTEMATIC SEARCH FOR MORE THEMIS SUB-FAMILIES. ANY NEW SUB-FAMILY WILL BE STUDIED TO ASCERTAIN ITS AGE AND PHYSICAL CHARACTERISTICS. WE WILL ALSO INSPECT AVAILABLE ARCHIVAL IMAGES OF NEW SUB-FAMILY MEMBERS TO SEARCH FOR PREVIOUSLY UNRECOGNIZED ACTIVITY IN AN EFFORT TO IDENTIFY NEW MBCS. WE WILL ALSO INVESTIGATE THE LONG-TERM DYNAMICAL EVOLUTION OF ASTEROIDS FROM THE THEMIS FAMILY WITH A PARTICULAR FOCUS ON IDENTIFYING PATHWAYS BY WHICH MEMBERS CAN EXIT THE FAMILY VIA RESONANCES OR NON-GRAVITATIONAL EFFECTS AND ASCERTAINING THE PROBABLE ABUNDANCE AND DYNAMICAL PROPERTIES OF SUCH OBJECTS. IT HAS BEEN SUGGESTED THAT A FOURTH MBC COULD HAVE ONCE BEEN A THEMIS MEMBER DESPITE ITS CURRENTLY HIGH ECCENTRICITY. WE WILL INVESTIGATE THIS HYPOTHESIS USING NUMERICAL INTEGRATIONS OF MEMBERS OF THE THEMIS FAMILY INCLUDING BOTH GRAVITATIONAL AND NON-GRAVITATIONAL FORCES TO DETERMINE WHETHER OTHER MAIN-BELT ASTEROIDS OR EVEN NEAR-EARTH OBJECTS COULD BE FORMER THEMIS FAMILY MEMBERS. USING THESE DYNAMICAL RESULTS WE WILL DEVELOP THERMAL MODELS OF ICE DEPLETION IN THEMIS ASTEROIDS AS THEY EITHER REMAIN IN THE MAIN BELT ACCOUNTING FOR BOTH THERMAL AND COLLISIONAL PROCESSES OR TRANSITION FROM THE MAIN BELT TO NEAR-EARTH SPACE ACCOUNTING FOR CHANGING ENVIRONMENTAL CONDITIONS AS THEY EVOLVE. IN PARTICULAR WE ARE INTERESTED IN DETERMINING IF ICE COULD STILL PERSIST IN NEOS WITH OUTER ASTEROID BELT ORIGINS. WE WILL BUILD ON EXISTING THERMAL AND ICE EVOLUTION MODELS OF THE NEAR-SURFACE AND COUPLE THEM WITH A 3D MODEL FOR THE INTERIOR OF THE BODY. THIS HIGHLY INTERDISCIPLINARY WORK IS RELEVANT TO NASA S SOLAR SYSTEM WORKINGS PROGRAM IN NUMEROUS WAYS. WE WILL STUDY GRAVITATIONAL AND NON-GRAVITATIONAL EFFECTS ON ASTEROIDS WITHIN AND WITHOUT AN ASTEROID FAMILY AND HOW THEY AFFECT ORBITAL CHARACTERISTICS AND STABILITY. WE WILL ALSO SEARCH FOR YOUNG SUB-FAMILIES WITHIN THE THEMIS FAMILY WHOSE FORMATION EVENTS ARE POSSIBLE SOURCES OF INTERPLANETARY DUST ANOTHER TOPIC OF INTEREST FOR THE SSW PROGRAM AND STUDY THE LONG-TERM DYNAMICAL EVOLUTION OF BOTH THE MAIN FAMILY AND ITS SUB-FAMILIES. AS PART OF OUR EFFORTS TO PHYSICALLY CHARACTERIZE YOUNG ASTEROID FAMILIES WE WILL ALSO ANALYZE AND INTERPRET EXISTING OBSERVATIONS OF SOLAR SYSTEM OBJECTS. FINALLY WE WILL INVESTIGATE THE PHYSICAL EVOLUTION OF VOLATILE MATERIAL (PARTICULARLY WATER ICE) IN THE INTERIORS OF MINOR BODIES VIA THEORETICAL MODELING WHICH ALIGNS WITH THE SSW PROGRAM GOAL TO STUDY THE INTERNAL STRUCTURE OF SOLAR SYSTEM OBJECTS AND UNDERSTAND THE PHYSICAL PROCESSES THAT OCCUR WITHIN THESE STRUCTURES AND IS ALSO ALIGNED WITH NASA S STRATEGIC INTEREST IN ASTEROID RESOURCE EXPLOITATION.

THE NASA PLANETARY DATA SYSTEM (PDS) IS A MAJOR ARCHIVE OF DATA PRODUCTS FROM PLANETARY SCIENCE RESEARCH SPONSORED BY NASA'S SCIENCE MISSION DIRECTOR

REFLECTANCE SPECTRA (BRIGHTNESS VARIATIONS AS A FUNCTION OF WAVELENGTH) CONTAIN INFORMATION PERTAINING TO COMPOSITION (IDENTIFICATION OF MINERALS) C

RE-EXAMINATION OF THE MARTIAN LACUSTRINE HISTORY

THE PROPOSED INVESTIGATION IS A GEOLOGIC MAPPING STUDY OF PARTS OF TERRA SABAEA AND TYRRHENA TERRA, NORTH OF THE HELLAS BASIN. THE PROJECT INCLUDES (

ROCK BREAKDOWN ON EARTH AND MARS: FURTHER INVESTIGATIONS USING A COMBINED FIELD AND EXPERIMENTAL APP

THE PRIMARY GOAL OF THIS PROPOSED STUDY IS TO PROVIDE IMPORTANT CONSTRAINTS ON THE SURFACE HYDRAULIC FLOW EROSIONAL AND DEPOSITIONAL PROCESSES THAT FORMED THE MARTIAN OUTFLOW CHANNELS. WE PROPOSE TO MORE FULLY ESTABLISH AND DESCRIBE THE ROLE WATER PLAYED IN OUTFLOW CHANNEL FORMATION AND EVOLUTION BY ANALYZING HIGH RESOLUTION IMAGES TO CHARACTERIZE THE EROSIONAL AND DEPOSITIONAL MORPHOLOGY OF FIVE SOUTHERN CIRCUM-CHRYSE OUTFLOW CHANNELS. WE WILL ALSO PERFORM HYDRAULIC MODELLING OF THESE OUTFLOW CHANNELS USING A NEW TWO-DIMENSIONAL APPROACH THAT INCORPORATES UNSTEADY COMPUTATIONAL FLUID DYNAMICS. OUR RESULTS WILL PROVIDE IMPORTANT DATA TOWARDS RECONSTRUCTING THE NATURE OF THE PALEOFLOODS THAT FORMED THE OUTFLOW CHANNELS. THIS INFORMATION WILL ALSO CONTRIBUTE TOWARD AN IMPROVED UNDERSTANDING OF THE GLOBAL HYDROLOGIC CYCLE OF MARS.

EO14042 WE SEEK TO DERIVE FROM LOLA DATA LUNAR SURFACE SLOPES AND ROUGHNESS AS A FUNCTION OF SCALE AND TO STUDY THE INFLUENCE OF THESE MEASUREMENTS ON SURFACE TEMPERATURE

THE ABUNDANCE AND DISTRIBUTION OF WATER ICE IN THE LUNAR POLAR REGIONS REMAINS ONE OF THE MOST IMPORTANT AND UNANSWERED QUESTIONS IN LUNAR SCIENCE. CLASSICAL THEORY SUGGESTS ICE SHOULD RESIDE WITHIN COLD TRAPS BUT THE OBSERVATIONAL EVIDENCE POINTS TOWARD A MORE COMPLEX SITUATION. NEVERTHELESS CLASSIC COLD TRAPPING THEORY IS CONSISTENT WITH OBSERVATIONS OF ICE IN PERMANENTLY SHADOWED CRATERS ON MERCURY AND CERES. THE EXTENT OF COLD TRAPS IS COMMONLY DEFINED BY A PEAK TEMPERATURE THRESHOLD WHEREAS IT IS FUNDAMENTALLY DEFINED BY SUBLIMATION RATE. HERE WE PROPOSE TO MAP LUNAR COLD TRAPS FOR THE FIRST TIME BASED ON TIME-INTEGRATED SUBLIMATION RATES INSTEAD OF PEAK TEMPERATURE. THE SAME APPROACH WILL BE USED TO MORE ACCURATELY MAP THE STABILITY OF BURIED ICE AND THERMAL PUMPING TWO PROPOSED ALTERNATIVE ICE STORAGE MECHANISMS. FINALLY WE WILL COMPARE THESE RESULTS WITH SEVERAL OBSERVATIONAL CONSTRAINTS. DELIVERABLES INCLUDE: 1) THE MOST ACCURATE MAP OF COLD TRAPS (POTENTIAL SUBLIMATION RATE) EVER PRODUCED 2) NEW SOFTWARE TECHNOLOGY FOR READ-LIMITED DATA PROCESSING AND 3) A QUANTITATIVE ASSESSMENT OF SPATIAL COINCIDENCE OR DEVIATION BETWEEN ICE RESERVOIRS PREDICTED BY THREE THEORIES VERSUS OBSERVATIONAL CONSTRAINTS. THIS DETAILED QUANTIFICATION OF ICE STORAGE MECHANISMS WILL PROVIDE CRUCIAL INSIGHT INTO THE SCIENCE OF LUNAR VOLATILES.