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38,696 grants matching “als”
Targeting the EPhA4 in motor neuron disease: a structure-based approach
$453,229Maurizio Pellecchia · University Of California Riverside · R01 · FY2019 · NS
Entry Into Comprehensive Methadone Treatment Via Interim Maintenance
$453,102Robert P Schwartz · Friends Research Institute, Inc. · R01 · FY2009 · DA
Improving parenting capacity to promote safe driving for adolescents with ADHD
$453,083Gregory A Fabiano · State University Of New York At Buffalo · R01 · FY2014 · HD
A CRITICAL ISSUE IN DEALING WITH NEAR-EARTH OBJECTS (NEO) ACCORDING TO NEOO PROGRAM GOALS AND THE PLANETARY DEFENSE COORDINATION OFFICE (PDCO) IS TO IDENTIFY POTENTIAL IMPACTORS THAT MAY STRIKE THE EARTH. GIVEN THIS PRIORITY IT IS DISTURBING THAT WE DO NOT YET HAVE AN ACCURATE MODEL OF THE ORBITS AND PHYSICAL PROPERTIES OF NEO IMPACTORS. AT BEST WE HAVE VAGUE APPROXIMATIONS FOR IMPACTOR TRAJECTORIES VELOCITIES SIZES STRENGTHS AND COMPOSITIONS. WITH AN ACCURATE MODEL WE CAN POTENTIALLY OPTIMIZE OUR GROUND- AND SPACEBASED SEARCH STRATEGIES TO FIND IMPACTORS EVALUATE THE EFFECTIVENESS OF STATE OF THE ART SURVEYS LIKE NEOCAM SENTINEL AND LSST AND DEVELOP COST EFFECTIVE EARLY WARNING SYSTEMS FOR CHELYBINSK-LIKE AND LARGER EVENTS. THE KEY PROBLEMS WITH COMPUTING AN ACCURATE IMPACTOR MODEL ARE AS FOLLOWS: 1. IMPACT PROBABILITY PROBLEMS: NEARLY ALL SYNTHETIC IMPACTORS ARE GENERATED BY RUNNING OBSERVED/MODEL NEOS THROUGH STATISTICAL OPIK -LIKE CODES WHERE IMPACT PROBABILITIES ARE DETERMINED USING GEOMETRICAL ARGUMENTS (E.G. OPIK 1951; BOTTKE ET AL. 1994; VERES ET AL. 2009). AS WE WILL SHOW HOWEVER OPIK CODES PRODUCE INACCURATE NEO IMPACTORS. THEY ASSUME THAT OVER ~1E4 YEARS THE SEMIMAJOR AXIS A ECCENTRICITY E AND INCLINATION I OF NEOS ARE UNCHANGING AND THEIR ORBIT ANGLES PRECESS UNIFORMLY. RECENT STUDIES HOWEVER SHOW THESE ASSUMPTIONS ARE FREQUENTLY VIOLATED; OVER THESE TIMESCALES PLANETARY PERTURBATIONS CAN PRODUCE NON-UNIFORM ORBIT ANGLES (E.G. JEONGAHN AND MALHOTRA 2014) AND BIG E I SWINGS (E.G. VOKROULICKY ET AL. 2012; POKORNY AND VOKROUHLICKY 2013). 2. MANY NEOS DISRUPT NEAR THE SUN. IN CONSTRUCTING A NEW NEO MODEL GRANVIK ET AL. (2016) SHOWED THAT PRIMITIVE OBJECTS BETWEEN ~100 M AND FEW KM DISRUPT WHEN THEY GET WITHIN ~0.05-0.2 AU OF THE SUN. WE ARGUE HERE THIS MAY BE TOO CONSERVATIVE; METER-SIZED BOLIDES AND LUNAR CRATERS INDICATE THAT MANY SMALL NEOS REGARDLESS OF COMPOSITION DISRUPT WITHIN ~0.17 AU OF THE SUN. NO IMPACTOR MODEL HAS YET ACCOUNTED FOR THIS EFFECT. 3. NO COLOR-ALBEDO-TAXONOMY MODEL FOR IMPACTORS. AT THIS TIME NO QUANTITATIVE MODEL OF THE LIKELY NATURE OF POTENTIAL IMPACTORS EXISTS. THIS LIMITS OUR ABILITY TO APPRAISE THE RANGE OF POTENTIAL EFFECTS PRODUCED BY THEIR BLASTS ANOTHER KEY GOAL OF NEOO AND THE PDCO. GIVEN THESE LIMITATIONS WE PROPOSE TO DEVELOP THE MOST ACCURATE NEO IMPACTOR MODEL EVER USING DIRECT NUMERICAL INTEGRATION METHODS AS WELL AS THE INSIGHTS PROVIDED BY THE NEW NEO MODEL OF GRANVIK ET AL. (2016). OUR PROPOSED TASKS ARE AS FOLLOWS: TASK 1. USING SUPERCOMPUTERS AND INITIAL CONDITIONS FROM GRANVIK ET AL. (2016) WE WILL INITIATE A LARGE NUMERICAL CAMPAIGN TO GENERATE 5E4-5E5 SYNTHETIC IMPACTORS WITH WELL-DEFINED ORBITS OVER THE NEXT THREE YEARS. THIS WILL REQUIRE US TO INTEGRATE THE ORBITS OF ~5E5-5E6 ASTEROIDS FOR ~200 MYR. IN ADDITION USING NEW CODES WRITTEN FOR THIS PROPOSAL WE WILL ALSO COMPUTE THE LOCATION IMPACT TRAJECTORIES AND COLLISION VELOCITIES FOR THE IMPACTORS. TASK 2. THE INTERNAL STRUCTURE DENSITY AND STRENGTHS OF IMPACTORS CORRELATE WITH THEIR OBSERVABLE PROPERTIES (E.G. LOW ALBEDO CCOMPLEX ASTEROIDS LIKELY SIMILAR TO CARBONACEOUS CHONDRITES). ACCORDINGLY TO PREDICT IMPACTOR PHYSICAL PROPERTIES WE WILL DEVELOP AN ALBEDO-COLOR-TAXONOMY MODEL FOR IMPACTORS BASED ON THEIR ORBITS. HERE WE WILL TAKE ADVANTAGE OF THE METHODS AND MODEL OF GRANVIK ET AL. (2016) AS WELL AS SEVERAL RICH DATASETS CONTAINING MAIN BELT AND NEO ALBEDOS (WISE/NEOWISE) COLORS (SDSS) AND TAXONOMIC CLASSES (E.G. PDS NODE). TASK 3. USING AN ESTABLISHED NEO SURVEY SIMULATOR (VERES ET AL. 2009) WE WILL EXAMINE THE EFFICIENCY OF EXISTING AND PROSPECTIVE SURVEYS AT DETECTING OUR SYNTHETIC IMPACTORS. OUR WORK WILL DETERMINE WHAT SURVEY STRATEGIES/PROPERTIES ARE NEEDED TO MEET NEOO/PDCO GOALS.
$453,062Southwest Research Institute · · FY2020 · National Aeronautics and Space Administration
Synaptic plasticity onto Dopamine neurons shapes fear learning
$453,021Antonello Bonci · National Institute On Drug Abuse · ZIA · FY2016 · DA
RESEARCH METHODS CORE
$452,980Nicholas Ialongo · Johns Hopkins University · P30 · FY2010 · MH
SOCIAL SKILLS TRAINING FOR MEDICATED ADHD CHILDREN
$452,962University Of California Los Angeles · R01 · FY2002 · MH
Neuropathology Core
$452,897Allan I Levey · Emory University · P30 · FY2025 · AG
Regulation Of Sugar Transport And Metabolism In Oral Bacteria
$452,857John M Thompson · Dental & Craniofacial Research · Z01 · FY2007 · DE
INTRODUCTION. ALTHOUGH LUNAR MAGNETIC ANOMALIES (LMAS) WERE DISCOVERED IN THE SEVENTIES BY THE APOLLO MISSIONS THEIR INTERACTIONS WITH THE SOLAR WIND PLASMA FLOW AND THEIR POSSIBLE CONNECTION WITH LUNAR SWIRLS REMAIN POORLY UNDERSTOOD. THE SUBJECT IS HIGHLY INTRIGUING BECAUSE OF THE IMPLICATIONS FOR THE MOON S GEOLOGICAL HISTORY AND POSSIBLE FUTURE LUNAR EXPLORATION OPPORTUNITIES. TWO MAJOR OBSTACLES HAVE BLOCKED THE PATH TO BETTER UNDERSTANDING THE NATURE OF THE SOLAR WIND PLASMA INTERACTION WITH LMAS: 1) OUR LACK OF OBSERVATIONS OF THE LMA STRUCTURE AND STRENGTH WITHIN A FEW KM OF THE LUNAR SURFACE; AND 2) THE LIMITATIONS OF COMPUTATIONAL RESOURCES TO RESOLVE BOTH THE ELECTRON AND ION KINETIC PHYSICS WHILE MODELING SUFFICIENTLY LARGE SPATIAL SCALES. WITH THE DEVELOPMENT OF IMPLICIT PARTICLE-IN-CELL TECHNIQUES THE LATTER HURDLE HAS RECENTLY BEEN SUCCESSFULLY SURPASSED [DECA ET AL. PRL 2014] OPENING NEW FRONTIERS TO CONSOLIDATE MULTI-SCALE AND MULTI-PHYSICS SIMULATIONS WITH THE AVAILABLE LOW-ORBIT LUNAR OBSERVATIONS. SCIENCE GOALS OBJECTIVES AND METHODOLOGY. WE PROPOSE TO SYSTEMATICALLY MINE THE VAST AMOUNT OF MEASUREMENTS FROM THE ARTEMIS AND KAGUYA (SELENE) MISSIONS. BUILDING ON PREVIOUS SUCCESSFUL STUDIES WE FOCUS ON THE ION AND ELECTRON DISTRIBUTIONS OBSERVED FOR A WIDE RANGE OF WEAK TO STRONG LMAS AND COMPARE THE BACK-STREAMING POPULATIONS WITH THE PREDICTIONS FROM REALISTIC FULL-KINETIC PARTICLE-IN-CELL SIMULATIONS. MOST RECENTLY TSUNAKAWA AND COLLABORATORS (JGR 2015) APPLIED A SURFACE VECTOR MAPPING (SVM) METHOD TO CONSTRUCT GLOBAL MAPS OF THE LMA STRUCTURE CLOSE TO THE SURFACE WHICH HAS BEEN SUCCESSFULLY INTEGRATED WITH OUR COMPUTATIONAL MODEL IPIC3D [DECA ET AL. UNDER REVIEW]. ANALYZING DATA FROM KAGUYA S PLASMA ENERGY ANGLE AND COMPOSITION EXPERIMENT (MAPPACE) INTERTWINED WITH THE ARTEMIS PARTICLE MEASUREMENTS WE WILL LOOK FOR PRECISE CORRELATIONS BETWEEN THE OBSERVED PARTICLE DISTRIBUTIONS/FLUXES AND THE MAGNETIC FIELD MAPS. WE WILL CONSTRUCT A RELIABLE CORRELATION MODEL BETWEEN THE OBSERVED BACK-STREAMING POPULATIONS AND THE UNDERLYING MAGNETIC FIELD TOPOLOGY TAKING INTO ACCOUNT THE UPSTREAM SOLAR WIND CONDITIONS. THIS WORK WILL PROVIDE A DEFINITIVE ANSWER TO THE QUESTION OF WHICH KINETIC PROCESSES DOMINATE THE SOLAR WIND INTERACTION WITH LMAS. RELEVANCE. UP TO THE PRESENT ONLY THE CORRELATIONS WITH THE STRONGEST LMAS SUCH AS THE REINER GAMMA AND GERASIMOVICH ANOMALIES HAVE BEEN STUDIED IN DETAIL [E.G. FATEMI ET AL. JGR 2015 POPPE ET AL. ICARUS 2016 DECA ET AL. UNDER REVIEW]. THE PROPOSED SYSTEMATIC ANALYSIS OF A GREAT NUMBER OF LMAS WILL SHED LIGHT ON THE GLOBAL VARIABILITY AND STRUCTURE OF THE LUNAR NEAR-SURFACE PLASMA ENVIRONMENT AROUND THESE SMALL-SCALE STRUCTURES. WE WILL IDENTIFY CORRELATIONS BETWEEN THE OBSERVED PLASMA POPULATIONS AND THE POSITION OF THE LMAS ON THE LUNAR SURFACE AND/OR THE POSITION OF THE MOON ALONG ITS ORBIT. AN ADDITIONAL GOAL OF THIS WORK IS TO HELP DISTINGUISH BETWEEN THE COMPETING THEORIES FOR THE FORMATION OF LUNAR SWIRLS AND DETERMINE WHETHER THEY COULD BE THE RESULT OF DIRECT SOLAR WIND INTERACTION WITH LMAS. A BETTER UNDERSTANDING OF THE KINETIC INTERACTION WITH SMALL-SCALE MAGNETIC STRUCTURES ON THE MOON WILL ALSO BENEFIT THE ANALYSIS OF MARTIAN MAGNETIC ANOMALIES AND MERCURY S SMALL MAGNETOSPHERE.
$452,816The Regents Of The University Of Colorado · · FY2020 · National Aeronautics and Space Administration
Inositol Lipid Regulation of Membrane Fusion & Fission
$452,791Lois S Weisman · University Of Michigan At Ann Arbor · R01 · FY2015 · GM
Understanding the structural basis of replication initiation in AAV
$452,765Frederick Dyda · National Institute Of Diabetes And Digestive And Kidney Diseases · ZIA · FY2012 · DK
Structure and function of eukaryotic DNA transposases
$452,765Frederick Dyda · National Institute Of Diabetes And Digestive And Kidney Diseases · ZIA · FY2012 · DK
Structure and function of novel prokaryotic DNA transposases
$452,765Frederick Dyda · National Institute Of Diabetes And Digestive And Kidney Diseases · ZIA · FY2012 · DK
GENETIC ANALYSIS OF ZEBRAFISH EMBRYO DEVELOPMENT
$452,720Paul Liu · National Human Genome Research Institute · ZIA · FY2010 · HG
Integrin-targeted siRNA delivery for therapeutic gene silencing in blood cancers
$452,691Motomu Shimaoka · Immune Disease Institute, Inc. · R01 · FY2010 · CA
Control of Mammalian Craniofacial Morphogenesis by the ESCRT Machinery
$452,681Licia Selleri · University Of California, San Francisco · R01 · FY2024 · DE
METABOLIC REGULATION IN LEUKEMIA-INITIATING CELLS
$452,662Daisuke Nakada · Baylor College Of Medicine · R01 · FY2023 · CA
METABOLIC REGULATION IN LEUKEMIA-INITIATING CELLS
$452,662Daisuke Nakada · Baylor College Of Medicine · R01 · FY2022 · CA
Role of Afadin in 3D epithelial plexus morphogenesis and beta cell mass
$452,661Ondine B Cleaver · Ut Southwestern Medical Center · R01 · FY2020 · DK
SYNTHETIC PEPTIDE VACCINES FOR DENTAL CARIES
$452,616Forsyth Institute · R01 · FY2000 · DE
IGF::OT::IGF RD CORONERY ARTERY RISK DEVELOPMENT IN YOUNG ADULTS (CARDIA) UMN FI
$452,595Pamela Shreiner · University Of Minnesota · N01 · FY2013 · HL
AFTER MORE THAN 2 YEARS OF OPERATIONS IN THE VICINITY OF COMET 67P/CHURYUMOV-GERASIMENKO ESA S HIGHLY SUCCESSFUL EXPLORATORY SPACE MISSION ROSETTA CAME TO ITS CONCLUSION IN SEPTEMBER 2016. ROSETTA CARRIED ONBOARD A COMPREHENSIVE SUITE OF FIVE PLASMA INSTRUMENTS DESIGNED TO OBSERVE THE FORMATION AND EVOLUTION OF THE VARIOUS PLASMA INTERACTION REGIONS AS THE COMET TRAVELED ALONG ITS ELLIPTICAL ORBIT [CARR ET AL. SPACE SCI. REV. (2007)]. WHILE SOME OBSERVATIONS WERE EXPECTED MANY OTHERS WERE A COMPLETE SURPRISE AND HAVE RAISED MORE QUESTIONS THAN THEY HAVE BROUGHT ANSWERS. IN PARTICULAR THE ROLE OF THE DIFFERENT ELECTRON POPULATIONS OF THE NEARCOMET ENVIRONMENT [ERIKSSON ET AL. ASTRON.&ASTROPH. (2017)] IN THE VARIOUS OBSERVED INSTABILITIES AND WAVES IS POORLY UNDERSTOOD. A COMETARY IONOSPHERE IS FORMED WHEN THE OUTGASSING NEUTRAL ATMOSPHERE BECOMES IONIZED THROUGH PHOTOIONIZATION CHARGE EXCHANGE WITH SOLAR WIND IONS AND IMPACT IONIZATION OF HIGH-ENERGY ELECTRONS [CRAVENS ET AL. J. GEOPHYS. RES. (1987); GALAND ET AL. MON. NOT. R. ASTRON. SOC. (2016)]. THROUGH MASS-LOADING OF THE SOLAR WIND [BIERMANN ET AL. SOLAR PHYS. (1967); SZEGO ET AL. SPACE SCI. REV. (2000)] AND A NONCONSTANT COLLISION CROSS-SECTION FROM THE COMET [CRAVENS ET AL. ADV. SPACE RES. (1989)] VARIOUS PLASMA INTERACTION BOUNDARIES DEVELOP EVOLVE AND HAVE BEEN OBSERVED BY THE ROSETTA SPACECRAFT IN THE COMETARY PLASMA ENVIRONMENT [MANDT ET AL. MON. NOT. R. ASTRON. SOC. (2016)]. OUR GOAL IS TWOFOLD. (1) TO CHARACTERIZE THE STABILITY OF A WEAK COMETARY IONOSPHERE AS THE PLASMA TRANSITIONS FROM A COLLISIONAL TO A COLLISIONLESS INTERACTION REGION [VIGREN&ERIKSSON ASTRONOM. J. (2017)]. INSIDE THE ELECTRON COLLISIONOPAUSE A PART OF THE ELECTRON POPULATION IS COOLED BY COLLISIONS WITH THE NEUTRAL GAS WHEREAS THE WARM POPULATION IS CONSTITUTED OF LOCALLY-PRODUCED ELECTRONS RELEASED IN THE IONIZATION PROCESS THAT HAVE RETAINED THEIR ENERGY [GILET ET AL. RADIO SCI. (2017)]. STRONG DENSITY GRADIENTS HAVE BEEN OBSERVED AT THE BOUNDARY BETWEEN THESE TWO ELECTRON REGIMES [HENRI ET AL. MON. NOT. R. ASTRON. SOC. (2017)] PROVIDING A SOURCE OF FREE ENERGY FOR INSTABILITIES TO DEVELOP [KARLSSON ET AL. GEOPHYS. RES. LETT. (2017)]. (2) TO ASSESS THE PHYSICAL PROCESSES THAT CAUSE THE GENERATION OF THE ANOMALOUSLY LARGE DENSITY OF ENERGETIC ELECTRONS CLOSE TO THE COMET. THE LATTER HAVE BEEN OBSERVED NEXT TO THE COLD AND WARM POPULATIONS WITH ENERGIES RANGING FROM 15 UP TO 200 EV [CLARK ET AL. ASTRON.&ASTROPH. (2015)] HIGH ENOUGH TO IONIZE THE COMETARY NEUTRALS AND SERVE AS A SIGNIFICANT SOURCE POPULATION FOR THE COMETARY IONOSPHERE [HERITIER ET AL. ASTRON.&ASTROPH. (2018)]. IN THE LITERATURE THEIR PRESENCE HAS BEEN EXPLAINED BY HEATING THROUGH WAVEPARTICLE INTERACTIONS [BROILES ET AL MON. NOT. R. ASTRON. SOC. (2016)] OR THROUGH THE ACCELERATION OF SOLAR WIND ELECTRONS BY A COMETARY AMBIPOLAR ELECTRIC FIELD [MADANIAN ET AL J. GEOPHYS. RES. (2016)]. ONLY A 3D FULLY KINETIC MODEL THAT INCLUDES BOTH ELECTRON AND ION COLLISIONS CAN ASSESS THE UNDERLYING PHYSICAL PROCESSES THAT DOMINATE THE COMET-PLASMA INTERACTION [DECA ET AL. PHYS. REV. LETT. (2017)]. THE KEY QUESTION WE FOCUS ON IS HOW THE OBSERVED WAVES COUPLE TO THE UNDERLYING PARTICLE DISTRIBUTIONS AND THE OVERALL (GLOBAL) PLASMA STRUCTURE OF A WEAKLY OUTGASSING COMET. THIS STUDY WILL BRING CLARITY TO DISENTANGLE THE RELATIVE CONTRIBUTIONS OF THE VARIOUS PHYSICAL PROCESSES DEDUCED FROM THE MEASUREMENTS. BEING ABLE TO COMBINE THE FINDINGS OF A SUITE OF PLASMA OBSERVATIONS WITH A COMPREHENSIVE SELF-CONSISTENT 3D MODEL HELPS TO BETTER PREDICT THE PLASMA STRUCTURE AROUND OTHER COMETS WHICH ON ITS TURN ALLOWS DEFINING MORE ACCURATELY THE PERSPECTIVES FOR FUTURE COMETARY MISSIONS AND THE BEHAVIOR OF MASS-LOADING PLASMA IN SPACE.
$452,500The Regents Of The University Of Colorado · · FY2020 · National Aeronautics and Space Administration
Probing the Proteinopathy Component of Light Chain Amyloidosis Pharmacologically
$452,500Jeffery W Kelly · Scripps Research Institute, The · R01 · FY2023 · HL
Genetic and Pharmacogenetic Modifiers of Cancer Risk and Intervention Outcomes
$452,492Mark H Greene · Division Of Cancer Epidemiology And Genetics · ZIA · FY2014 · CA