The Collier Report of U.S. Government Contracting

Sampling of Federal Government Funding Actions/Set Asides

In order by amount of set aside monies.

• $9,964 - Tuesday the 5th of June 2012
  Veterans Affairs Department
  688-WASHINGTON DC
  TUITION PAYMENT FOR NURSING ED

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• $91,000 - Friday the 10th of July 2015
  National Aeronautics And Space Administration
  NASA SHARED SERVICES CENTER
  WE PROPOSE TO STUDY THE HEATING AND THE ACCELERATION OF MULTI-ION PLASMA IN THE SOLAR WIND BY A TURBULENT SPECTRUM OF ALFV NIC FLUCTUATIONS USING 2D HYBRID NUMERICAL MODEL. THE CENTRAL SCIENCE QUESTION OF THE SOLAR WIND PLASMA HEATING AND ACCELERATION WILL BE ADDRESSED IN THE PROPOSED STUDY. THE MODELING EFFORT WILL BE GUIDED BY THE OBSERVED PROPERTIES OF THE SPECTRUM AND THE MEASURED PHYSICAL PARAMETERS OF THE SOLAR WIND PLASMA IN THE INNER CORONA AND THROUGHOUT THE HELIOSPHERE BY COMPUTATIONAL MODELS APPROPRIATE TO THE SMALL SCALE KINETIC CONDITIONS IN VARIOUS REGIONS. EXPANDING SOLAR WIND MODEL WILL BE INCORPORATED INTO THE CODE. IN PARTICULAR, WE PROPOSE TO DEVELOP TWO-DIMENSIONAL HYBRID MODELS OF SOLAR WIND PLASMA WITH PROTONS, HELIUM AND HEAVIER IONS, AND STUDY THE HEATING OF THE PLASMA BY RESONANT AND NON-RESONANT TURBULENT ALFV NIC WAVE SPECTRUM, AND BY ION BEAMS. IN A HYBRID MODEL THE PROTONS AND HEAVY IONS ARE TREATED KINETICALLY, WHILE THE ELECTRONS ARE INCLUDED AS NEUTRALIZING BACKGROUND FLUID. THIS WILL BE THE FIRST TWO-DIMENSIONAL HYBRID STUDY OF THE SOLAR WIND PLASMA THAT INCLUDES THE EFFECTS TURBULENT WAVE SPECTRUM GUIDED BY OBSERVATION. IN ADDITION, WE PROPOSE TO INVESTIGATE THE EFFECTS OF ION BEAMS AND INHOMOGENEITY OF THE BACKGROUND PLASMA DENSITY ON THE HEATING AND THE ACCELERATION OF THE SOLAR WIND. THE RESULTS OF THE MODEL WILL BE COMPARED TO PUBLISHED SPACECRAFT DATA AND WILL BE USEFUL FOR FUTURE MISSIONS, SUCH AS THE SOLAR PROBE. THE STUDY IS DIRECTLY RELEVANT TO THE GOALS OF NASA SOLAR AND HELISOPHERIC PROGRAM.

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• $8,010 - Friday the 13th of July 2012
  Department Of Navy
  NAVY MEDICINE PROFESSIONAL
  TUITION AND FEES

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• $66,654 - Friday the 10th of July 2015
  National Aeronautics And Space Administration
  NASA SHARED SERVICES CENTER
  THE OBJECTIVE OF THIS PROPOSAL IS TO ADDRESS SEVERAL KEY QUESTIONS ABOUT THE GEOLOGIC HISTORY OF MERCURY USING THE MESSENGER GEOCHEMISTRY SUITE OF INSTRUMENTS - XRS, GRNS, AND VIRS. EACH OF THESE INSTRUMENTS IS SENSITIVE TO DIAGNOSTIC ELEMENTS IN MERCURY'S SURFACE. MEASUREMENT OF ELEMENTS SUCH AS FE, CA, AL, K, TH, H, AND S WILL PROVIDE VALUABLE INFORMATION THAT WILL MAKE IT POSSIBLE TO SELECT BETWEEN COMPETING THEORIES OF MERCURY'S HIGH IRON/SILICATE RATIO, TO ESTABLISH THE ORIGIN OF THE SMOOTH AND INTERCRATER PLAINS, AND TO IDENTIFY THE SOURCE OF THE HIGH RADAR REFLECTIVE SIGNAL FROM DEPOSITS NEAR THE POLES. WHILE EACH OF THE GEOCHEMISTRY INSTRUMENTS IS INDEPENDENTLY CAPABLE OF ADDRESSING SOME OF THESE KEY SCIENCE QUESTIONS, THE SYNTHESIS OF DATA FROM ALL THREE WILL PROVIDE INSIGHT INTO THE GEOLOGIC HISTORY OF MERCURY THAT WOULD NOT BE OBTAINED OTHERWISE. IN FACT, EACH OF THE GEOCHEMISTRY INSTRUMENTS TO SOME EXTENT WILL DEPEND ON THE OTHERS FOR CROSS CALIBRATION AND NORMALIZATION. MY SPECIFIC CONTRIBUTION TO THIS EFFORT WILL BE DEVELOPMENT OF ANALYSIS TOOLS FOR THE XRS EXPERIMENT, MODELING OF PARTICLE TRANSPORT IN THE PLANET S SURFACE, AND MODELING OF DETECTOR RESPONSE FUNCTIONS. PRIMARY FOCUS WILL BE ON APPLICATION OF ANALYTIC MODELS OF X-RAY FLUORESCENCE AND SCATTERING, AND MONTE CARLO MODELING OF ELECTRON INDUCED X-RAY FLUORESCENCE. GRNS RELATED WORK MAY INCLUDE MONTE CARLO MODELING OF NEUTRON AND GAMMA-RAY TRANSPORT IN THE PLANET. THE TASKS DESCRIBED ABOVE ARE ESSENTIAL TO THE ANALYSIS OF XRS AND GRNS DATA. COMBINING THE RESULTS FROM THESE INSTRUMENTSWITH THE VIRS DATA WILL PROVIDE A BETTER UNDERSTANDING OF THE GEOLOGICAL EVOLUTION OF MERCURY AND HOW IT RELATES TO THE OTHER TERRESTRIAL PLANETS.

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• $49,519 - Friday the 10th of July 2015
  National Aeronautics And Space Administration
  NASA SHARED SERVICES CENTER
  WE PROPOSE TO STUDY THE HEATING AND THE ACCELERATION OF MULTI-ION PLASMA IN THE SOLAR WIND BY A TURBULENT SPECTRUM OF ALFV NIC FLUCTUATIONS USING 2D HYBRID NUMERICAL MODEL. THE CENTRAL SCIENCE QUESTION OF THE SOLAR WIND PLASMA HEATING AND ACCELERATION WILL BE ADDRESSED IN THE PROPOSED STUDY. THE MODELING EFFORT WILL BE GUIDED BY THE OBSERVED PROPERTIES OF THE SPECTRUM AND THE MEASURED PHYSICAL PARAMETERS OF THE SOLAR WIND PLASMA IN THE INNER CORONA AND THROUGHOUT THE HELIOSPHERE BY COMPUTATIONAL MODELS APPROPRIATE TO THE SMALL SCALE KINETIC CONDITIONS IN VARIOUS REGIONS. EXPANDING SOLAR WIND MODEL WILL BE INCORPORATED INTO THE CODE. IN PARTICULAR, WE PROPOSE TO DEVELOP TWO-DIMENSIONAL HYBRID MODELS OF SOLAR WIND PLASMA WITH PROTONS, HELIUM AND HEAVIER IONS, AND STUDY THE HEATING OF THE PLASMA BY RESONANT AND NON-RESONANT TURBULENT ALFV NIC WAVE SPECTRUM, AND BY ION BEAMS. IN A HYBRID MODEL THE PROTONS AND HEAVY IONS ARE TREATED KINETICALLY, WHILE THE ELECTRONS ARE INCLUDED AS NEUTRALIZING BACKGROUND FLUID. THIS WILL BE THE FIRST TWO-DIMENSIONAL HYBRID STUDY OF THE SOLAR WIND PLASMA THAT INCLUDES THE EFFECTS TURBULENT WAVE SPECTRUM GUIDED BY OBSERVATION. IN ADDITION, WE PROPOSE TO INVESTIGATE THE EFFECTS OF ION BEAMS AND INHOMOGENEITY OF THE BACKGROUND PLASMA DENSITY ON THE HEATING AND THE ACCELERATION OF THE SOLAR WIND. THE RESULTS OF THE MODEL WILL BE COMPARED TO PUBLISHED SPACECRAFT DATA AND WILL BE USEFUL FOR FUTURE MISSIONS, SUCH AS THE SOLAR PROBE. THE STUDY IS DIRECTLY RELEVANT TO THE GOALS OF NASA SOLAR AND HELISOPHERIC PROGRAM.

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• $40,000 - Friday the 10th of July 2015
  National Aeronautics And Space Administration
  NASA SHARED SERVICES CENTER
  THIS PROPOSED RESEARCH SEEKS TO PROVIDE NEW KNOWLEDGE AND UNDERSTANDING FROM AN ANALYSIS OF RADIO EMISSIONS FROM SOLAR TRANSIENTS USING DATA FROM RADIO RECEIVERS ON THE STEREO AND WIND SPACECRAFT. SINCE SHORTLY AFTER LAUNCH IN OCTOBER OF 2006, THE STEREO SPACECRAFT HAVE BEEN ORBITING THE SUN AT A DISTANCE OF 1 AU, TRAILING BEHIND AND AHEAD OF EARTH. DURING THE PERIOD OF PERFORMANCE OF THIS RESEARCH THE ANGULAR SEPARATION OF THE TWO STEREO SPACECRAFT WILL VARY FROM ABOUT 80 FROM THE WIND SPACECRAFT NEAR EARTH TO ABOUT 1400 FROM WIND, I.E., ON THE FAR SIDE OF THE SUN. THIS CONFIGURATION WILL PROVIDE A UNIQUE OPPORTUNITY TO STUDY IN DETAIL HOW TRANSIENT RADIO PHENOMENA ARE OBSERVED FROM THE OPPOSITE SIDE OF THE SUN. THIS RESEARCH EFFORT BUILDS ON PREVIOUS RESEARCH THAT WE HAVE PERFORMED USING THE RADIO AND OTHER DATA FROM THE STEREO AND WIND SPACECRAFT WHEN THEY WERE ALL ON THE NEAR SIDE OF THE SUN. WE WILL ANALYZE IN DETAIL, THE RADIO EMISSIONS ASSOCIATED WITH SOLAR TYPE III RADIO BURSTS, PRODUCED BY ELECTRON BEAMS FROM THE SUN, AND ASSOCIATED WITH SOLAR TYPE II RADIO EMISSIONS, PRODUCED BY CORONAL AND INTERPLANETARY SHOCKS. WE WILL USE THE UNIQUE DIRECTION FINDING CAPABILITIES ON THE STEREO AND WIND SPACECRAFT TO LOCATE THE RADIO SOURCES USING THREE SPACECRAFT TRIANGULATION TECHNIQUES. WE WILL ALSO ANALYZE THE DIFFERENCES IN THE TIME PROFILES OF THE RADIO BURSTS OBSERVED FROM THESE WIDELY SEPARATED SPACECRAFT. FINALLY, WE WILL ANALYZE THE TIMES OF ARRIVAL AT EACH OBSERVING SPACECRAFT, SEEKING TO BETTER UNDERSTAND ANY ANOMALOUS TIME DELAYS THAT MAY BE CAUSED BY PROPAGATION AND SCATTERING EFFECTS IN THE INTERPLANETARY MEDIUM.

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• $36,300 - Saturday the 1st of December 2012
  National Institutes Of Health
  NIH, NHLBI, DERA OA OFC ACQUISTIONS
  IGF::CL::IGF CLOSELY ASSOCIATED- CONTRACT FOR COMPUTER SOFTWARE PROGRAMMING SUPPORT FOR NHLBI CONFOCAL MICROSCOPY IMAGING SYSTEM AND IMAGE PROCESSING.

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• $35,420 - Wednesday the 27th of June 2012
  Department Of Navy
  NAVY MEDICINE PROFESSIONAL
  TUITION AND FEES

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• $35,260 - Wednesday the 4th of April 2012
  Department Of Navy
  NAVY MEDICINE PROFESSIONAL
  TUITION AND FEES

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• $31,543 - Monday the 26th of June 2017
  National Aeronautics And Space Administration
  NASA SHARED SERVICES CENTER
  WE PROPOSE TO INVESTIGATE THE PHYSICAL PROCESSES THAT DRIVE INCREASES IN EXTREME ULTRAVIOLET (EUV; 6-36 NM) IRRADIANCE DURING SOLAR FLARES. AS THIS EMISSION CAN HAVE A SIGNIFICANT EFFECT ON EARTH'S UPPER ATMOSPHERE (LEAN ET AL. 2009, QIAN ET AL. 2010), UNDERSTANDING ITS ORIGINS IS A MAJOR GOAL OF THE LIVING WITH A STAR PROGRAM. PREVIOUS STUDIES HAVE SHOWN THAT THESE INCREASES ARE GREATEST DURING A FLARE'S IMPULSIVE PHASE (WOODS ET AL. 2004; 2006), SUGGESTING THAT THEY ARE DRIVEN BY NONTHERMAL ELECTRONS, ALTHOUGH HARD X-RAY (HXR) OBSERVATIONS HAVE NEVER BEEN UTILIZED TO CONFIRM THIS. THE MAIN FOCUS OF THIS PROPOSAL IS THEREFORE TO EXPAND UPON PREVIOUS WORKS BY COMBINING OBSERVATIONS OF SOLAR FLARES FROM THE RAMATY HIGH ENERGY SOLAR SPECTROSCOPIC IMAGER (RHESSI), TO CHARACTERIZE THE NONTHERMAL ELECTRONS THROUGH HXR IMAGING SPECTROSCOPY, AND THE EUV VARIABILITY EXPERIMENT (EVE) ONBOARD THE SOLAR DYNAMICS OBSERVATORY (SDO) TO MEASURE THE ASSOCIATED INCREASE IN EUV IRRADIANCE. TO DEMONSTRATE HOW COORDINATED OBSERVATIONS WITH THESE TWO INSTRUMENTS CAN ADDRESS THIS ISSUE, THE PRELIMINARY ANALYSIS OF TWO LOW-M-CLASS FLARES IS PRESENTED. EVE OBSERVATIONS SHOW A SMALL INCREASE (~3%) IN THE TOTAL EUV EMISSION OF ONE FLARE (AN M1.2 ON 5 MAY 2010), AND A LARGER INCREASE OF ~11% IN THE OTHER (AN M2.9 ON 16 OCTOBER 2010). IN EACH CASE, IT IS SHOWN THAT CHROMOSPHERIC EMISSION (PRIMARILY THE HE II LINE AT 30.4 NM) DOMINATES THIS CHANGE IN EUV IRRADIANCE, AND THAT IT IS TEMPORALLY CORRELATED WITH THE POWER CONTAINED IN NONTHERMAL ELECTRONS AS DETERMINED FROM RHESSI OBSERVATIONS. THE RHESSI DATA SHOW THAT THE 16 OCTOBER 2010 FLARE HAD A CONSIDERABLY HARDER ELECTRON SPECTRUM (DELTA=4, AT ENERGIES UP TO 100 KEV), THAN THE 5 MAY 2010 EVENT WHICH HAD A SOFTER SPECTRAL INDEX (DELTA=6 UP TO ONLY 50 KEV). THESE PRELIMINARY FINDINGS SUPPORT, AND EXPAND UPON, PREVIOUS STUDIES OF FLARE EUV IRRADIANCE THAT ONLY SPECULATED THAT INCREASED IRRADIANCE IS DRIVEN BY ACCELERATED PARTICLES. JOINT RHESSI AND EVE OBSERVATIONS ARE THEN DIRECTLY COMPARABLE TO THE RADIATIVE HYDRODYNAMIC SIMULATIONS OF ALLRED ET AL. (2005), WHICH CAN MODEL THE RESPONSE OF THE HE II LINE TO A BEAM OF NONTHERMAL ELECTRONS. THE EVE SPECTRAL RANGE ALSO CONTAINS A NUMBER OF DENSITY SENSITIVE EMISSION LINES WITH FORMATION TEMPERATURES IN EXCESS OF 10 MK, YIELDING A POTENTIALLY POWERFUL AND, AS YET, UNUSED DIAGNOSTIC OF FLARE DENSITIES AT HIGH TEMPERATURES. THESE LINE RATIOS WERE TENTATIVELY APPLIED TO BOTH OF THE FLARES DESCRIBED ABOVE, AND CLEAR CHANGES IN THE VALUES OF THE LINE RATIOS WERE FOUND DURING THE TWO EVENTS. - THE FIRST TASK OF THIS PROPOSAL IS TO COMPLETE THE ANALYSES OF THE 5 MAY 2010 AND 16 OCTOBER 2010 EVENTS TO ESTABLISH THE RELATIONSHIP BETWEEN THE PROPERTIES OF THE ACCELERATED ELECTRONS AND THE INCREASE IN EUV IRRADIANCE. - SECONDLY, THE RESULTS OF THIS JOINT ANALYSIS WILL BE DIRECTLY COMPARED TO THE MODEL PREDICTIONS OF ALLRED ET AL. (2005) TO DETERMINE THE HEATING MECHANISM AND CONSTRAIN THE TOTAL ENERGETICS. - THE THIRD TASK INVOLVES INVESTIGATING THE DIAGNOSTIC POTENTIAL OF THE DENSITY SENSITIVE LINE RATIOS IN THE EVE SPECTRA TO DETERMINE THE PLASMA DENSITY DURING THE TWO FLARES. - FINALLY, WE WILL EXTEND THIS ANALYSIS TO THE 15 OTHER FLARES OF VARYING MAGNITUDES ALREADY JOINTLY OBSERVED BY BOTH RHESSI AND EVE, AND OTHERS DETECTED DURING THE RISE OF SOLAR CYCLE 24 TO PERFORM A STATISTICALLY SIGNIFICANT COMPARISON OF NONTHERMAL ELECTRON ENERGIES AND CHANGES IN EUV IRRADIANCE.

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