← LeaderboardsInvestigatorsiAttributed = a PI's even-split share of each grant — a $1M grant with 2 PIs counts $500K each.
Lockheed Martin Corporation
Gaithersburg
$200,858,003
Total funding
65
Grants
Funding over time
peak $95.2M · FY2008–22$100M$75M$50M$25M$0
'08
'09
'10
'11
'12
'13
'14
'15
'16
'17
'18
'19
'20
'21
'22
Funding mix
By agency
NSF$94,349,352 · 1
DOD$80,795,232 · 8
NASA$22,113,977 · 51
DOE$3,599,442 · 5
By mechanism
—$200,858,003 · 65
Investigators at Lockheed Martin Corporation
InvestigatorsiAttributed = a PI's even-split share of each grant — a $1M grant with 2 PIs counts $500K each.
Exposure= the full size of every grant they're on ($1M each).
Rising Stars
First grant in the last 5 yrs
Not enough data
Emerging Leaders
6–10 yrs in
Not enough data
All-Time
Most funded here, all years
Not enough data
Largest grants
Research and Operation Support for the United States Antarctic Program$94,349,352
· FY2011 · GEO
ADVANCED COMPOSITE CARGO AIRCRAFT (ACCA) FLIGHT DEMONSTRATOR$47,814,320
· FY2008 · Department of the Air Force
AFFORDABLE LASER INFRARED SURVIVABILITY SYSTEM (ALISS)$12,564,712
· FY2008 · Department of the Air Force
AIRBORNE MANNED UNMANNED SYSTEM TECHNOLOGY DEMONSTRATION$11,768,028
· FY2008 · Department of Defense
MACRO-SCALE ASSEMBLY&CHARACTERIZATION$3,425,762
· FY2019 · Department of the Army
AMUST D$2,940,415
· FY2008 · Department of the Army
ONE OF THE TOP QUESTIONS FOR NASA HELIOPHYSICS IS: WHAT CAUSES THE SUN TO VARY?. THE SOLAR MAGNETIC FIELD PLAYS A FUNDAMENTAL ROLE IN THIS VARIATION AND HENCE ITS MEASUREMENT MADE WITH MAGNETOGRAPHS IS ESSENTIAL.$1,754,283
· FY2020 · National Aeronautics and Space Administration
THE MULTI-AGENT ARCHITECTURE FOR COORDINATED, RESPONSIVE OBSERVATIONS$1,475,654
· FY2008 · National Aeronautics and Space Administration
EXPLORING OCEAN WORLDS REQUIRES ADAPTATION TO OBSTACLES NEVER SEEN BEFORE BY THE SYSTEM WHILE ALSO CONDUCTING SCIENCE OPERATIONS. ONE SOLUTION TO THIS PROBLEM IS UTILIZING REINFORCEMENT LEARNING TO LEARN STRATEGIES TO REACH A GOAL. ALTHOUGH$1,435,856
· FY2021 · National Aeronautics and Space Administration
MISSION SYSTEMS EFFECTIVENESS TRADES AND ANALYSIS$1,398,866
· FY2012 · Department of Defense
THE OFFEROR PROPOSES RESEARCH AND IF POSSIBLE IMPLEMENT THE MODERNIZATION OF SOLARSOFT SOFTWARE UPDATE DISTRIBUTION; PRESERVE ALGORITHMS FOR EMPLOYMENT BY FUTURE SOFTWARE ARCHITECTURES; IMPROVE THE PORTABILITY OF DOCUMENTATION; AND INTEGRATE SUPPORT FOR THE ANALYSIS OF MAJOR NEW SOLAR AND HELIOSPHERIC SCIENTIFIC DATA SETS (E.G. PARKER SOLAR PROBE DKIST AND SOLAR ORBITER) INTO SOLARSOFT.$1,225,766
· FY2020 · National Aeronautics and Space Administration
NEW AWARD - ADVANCED COMPOSITE OTEC COLD WATER PIPE PROJECT$1,193,110
· FY2008 · Department of Energy
WE AIM TO (A) INVESTIGATE THE PHYSICAL MECHANISMS DRIVING SOLAR ACTIVE REGION (AR) ERUPTIONS, (B) PROVIDE A CRITICAL EVALUATION OF THE VALIDITY OF RE$1,116,638
· FY2014 · National Aeronautics and Space Administration
THIS PROPOSAL AIMS AT BETTER LOCALIZATION OF THE SOURCE REGIONS OF THE SOLAR WIND OBSERVED IN NEAR-EARTH SPACE BY IMPROVING FULLSURFACE (SYNOPTIC) MAGNETIC MAPS COMMONLY USED TO COMPUTE MACROSCOPIC PROPERTIES OF THE SOLAR WIND. WE CONCENTRATE ON UPDATING THE MAGNETIC FIELD IN THE POLAR REGIONS. THE SOLAR WIND IS GENERALLY DIVIDED INTO TWO CATEGORIES FAST AND SLOW. WE OFTEN ASSOCIATE THE FAST SOLAR WIND WITH CORONAL HOLES DARK REGIONS IN EUV AND SOFT X-RAY IMAGES. IN COMPARISON THERE IS HARDLY ANY CONSENSUS AS TO THE ORIGIN OF THE SLOW SOLAR WIND. IT IS OF VITAL IMPORTANCE TO RELIABLY LOCATE THE SOURCE REGIONS IN ORDER TO TEST THE MODELS OF THE SOLAR WIND. KNOWING THE SOURCE REGIONS WILL ALSO HELP US UNDERSTAND VARIOUS PROPERTIES OF THE SOLAR WIND IN TERMS OF THE PROPERTIES OF THE SOURCE REGION. HOWEVER WITHOUT THE ACTUAL MEASUREMENT OF THE SOLAR WIND VERY CLOSE TO THE SUN WE CANNOT DIRECTLY LOCATE THE SOURCE REGIONS. INSTEAD WE HAVE TO DEPEND ON MODELS THAT SHOW WHERE ON THE SUN WE ARE MAGNETICALLY CONNECTED TO AND THUS EXPOSED TO THE SOLAR WIND. THESE MODELS GENERALLY REQUIRE THE RADIAL COMPONENT OF THE MAGNETIC FIELD OF THE FULL SOLAR SURFACE I.E. A SYNOPTIC MAGNETIC MAP AS BOUNDARY CONDITIONS. THIS IS NOT OBSERVATIONALLY AVAILABLE. PRESENTLY THE SOLAR MAGNETIC FIELD IS MEASURED EXCLUSIVELY FROM THE EARTH. ONLY LESS THAN ONE HALF OF THE SURFACE IS ADEQUATELY SAMPLED BY THESE MEASUREMENTS. WE MAY USE HELIOSEISMIC FARSIDE IMAGING COMBINED WITH STEREO EUV IMAGES TO DETECT STRONG MAGNETIC FIELD REGIONS ON THE BACKSIDE. MAGNETOGRAMS TAKEN SEVERAL DAYS BEFORE OR AFTER MAY TELL US WHETHER THERE WERE INDEED SUCH REGIONS ON THE BACKSIDE ASSUMING THAT THEY WOULD SURVIVE WITHOUT DRASTIC CHANGES FOR SEVERAL DAYS. HOWEVER THE POLAR REGIONS ARE INHERENTLY VERY HARD TO OBSERVE FROM THE ECLIPTIC AND THE HISTORICAL MEASUREMENTS OF MAGNETIC FIELD CLOSE TO THE POLES MAY HAVE LARGE UNCERTAINTIES. IT IS POSSIBLE THAT THESE UNCERTAINTIES MAY SERIOUSLY IMPACT OUR UNDERSTANDING OF THE MAGNETIC CONNECTION BETWEEN THE SUN AND EARTH. IN POLAR REGIONS THE RADIAL COMPONENT OF THE FIELD BECOMES ALMOST PERPENDICULAR TO THE LINE OF SIGHT AND HIGH-RESOLUTION AND HIGHSENSITIVITY VECTOR MEASUREMENTS BECOME ESSENTIAL. WE PROPOSE TO IMPROVE SYNOPTIC MAPS THAT SERVE AS THE LOWER BOUNDARY CONDITIONS FOR MODELS SIMPLE AND COMPLEX ALIKE BY INCORPORATING MEASUREMENTS OF THE VECTOR FIELD IN THE POLAR REGIONS BY THE HINODE SPECTRO-POLARIMETER (SP) AND SDO HELIOSEISMIC AND MAGNETIC IMAGER (HMI). TO DATE SP IS THE BEST RESOURCE FOR THE POLAR FIELD DUE TO ITS HIGH SPATIAL AND SPECTRAL RESOLUTION. INVERSIONS NOT INCLUDED IN THE PIPELINE WILL BE EXPLORED ON SP DATA TO ENSURE THE BEST RESULTS FOR THE POLAR REGIONS. HMI IS NEEDED NOT ONLY TO CORRECT FOR THE SP POINTING BUT ALSO TO ADDRESS THE TIME VARIABILITY OF THE POLAR FIELD. WE WILL CALIBRATE HMI DATA WITH SP AND USE THEIR RADIAL FIELD FOR UPDATING THE POLAR REGIONS IN THE SYNOPTIC MAPS FROM HMI LINE-OF-SIGHT MAGNEOTOGRAMS. USING THESE MAPS WE RUN BOTH THE POTENTIAL FIELD SOURCE SURFACE (PFSS) MODEL AND MAGNETOHYDRODYNAMIC (MHD) MODEL TO LOCATE THE MAGNETIC FOOTPOINT OF THE OBSERVER AT L1 AND ESTIMATE THE UNCERTAINTIES OF THE LOCATION. WE WILL SYSTEMATICALLY CONDUCT THIS STUDY FOR PERIODS SELECTED ON THE BASIS OF THE DIFFICULTY OF LOCATING THE SOURCE REGION OF THE SOLAR WIND. THE PROPOSED RESEARCH SHOULD BE AN IMPORTANT PART OF FST#2 AND WILL FORM THE BASIS OF OTHER PROJECTS IN THE TEAM WHOSE EMPHASIS MAY BE THE MECHANISMS OF HEATING AND ACCELERATION OF THE SOLAR WIND.$919,904
· FY2020 · National Aeronautics and Space Administration
TAS::89 0321::TAS OCEAN THERMAL ENERGY CONVERSION PIPE PIPE PLATFORM SUB-SYSTEM DYNAMIC INTERACTION VALIDATION (OPPSDIV)$914,082
· FY2010 · Department of Energy
IN THE NEXT DECADE NASA WILL DEVELOP LARGE SPACE-BASED OBSERVATORIES TO ANSWER FOR HUMANKIND THE FUNDAMENTAL ASTRONOMY QUESTION OF OUR AGE ARE WE ALONE IN THE UNIVERSE? THREE SUCH ENVISIONED MISSIONS ARCHITECTURES THE ORIGINS SPACE TELESCOPE (OST) THE HABITABLE EXOPLANET (HABEX) IMAGING MISSION AND THE LARGE ULTRAVIOLET/OPTICAL/INFRARED (LUVOIR) SURVEYOR ALL REQUIRE EXTREME LEVELS OF DYNAMIC STABILITY AND PRECISION POINTING AND WAVEFRONT ERROR PERFORMANCE OVER LONG OBSERVATION DURATIONS. ACHIEVING ULTRASTABILITY OF SEGMENTED OPTICAL SYSTEMS WITH INTEGRATED CORONAGRAPHS INVOLVES THE EXQUISITE INTEGRATION OF HIGH-PERFORMANCE SUBSYSTEMS INCLUDING ISOLATION REACTION-CANCELLING FAST STEERING MIRRORS WAVEFRONT SENSING AND CONTROL AND SEGMENT RELATIVE POSITION CONTROL TO NAME A FEW. THIS PRESENTS A SIGNIFICANT SYSTEMS ENGINEERING AND INTEGRATED DESIGN CHALLENGES INCLUDING REQUIREMENTS FLOWDOWN AND DEFINITION QUANTIFYING THE PERFORMANCE OF A LARGE DESIGN SPACE AND IDENTIFYING AREAS FOR FURTHER TECHNOLOGY DEVELOPMENT. WHILE PROGRESS HAS BEEN MADE IN COMPONENT TECHNOLOGY DEVELOPMENT FOR LARGE SEGMENTED OPTICS AND CORONAGRAPHS RIGOROUS ANCHORED END-TO-END SYSTEMS-LEVEL MODELS AND A SYSTEMATIC MODEL-BASED DESIGN APPROACH ARE NEEDED TO MEET THE SYSTEM DESIGN CHALLENGE. THE THREEFOLD OBJECTIVES OF THE PROPOSED RESEARCH PROVIDE NASA WITH A SOLUTION TO THIS END-TO-END SYSTEMS DESIGN CHALLENGE: (1) ANCHOR OBSERVATORY CONCEPTS AND ESTABLISH SPECIFICATIONS FOR KEY SENSING AND CONTROL ELEMENTS USING INTEGRATED MODELS TO QUANTIFY END-TOEND PERFORMANCE; (2) PERFORM TRADES TO ARRIVE AT OBSERVATORY ARCHITECTURE THAT INCREASE DESIGN ROBUSTNESS AND MEET SCIENCE RETURN OBJECTIVES; AND (3) PERFORM EARLY HIGH-BENEFIT TESTING AND FORMULATE A LONGER-TERM TECHNOLOGY MATURATION PLAN TO BRIDGE TECHNOLOGY GAPS RELATIVE TO THE CURRENT STATE OF THE ART. TWO SETS OF MODELS ARE ENVISIONED FOR LUVOIR AND HABEX THAT FULLY SPAN THE OPTICAL STABILITY PERFORMANCE ENVELOPE: A QUASI-STATIC MODEL WHERE ERRORS ARE PRINCIPALLY DRIVEN BY THERMAL DEFORMATION AND LONG-PERIOD FIGURE ERROR AND A DYNAMIC MODEL WHOSE ERRORS ARE DRIVEN BY DISTURBANCES THAT HAVE TIME-VARYING SIGNATURE SUCH AS THOSE ARISING FROM CONTROL-MOMENT-GYROSCOPE EXPORTED DISTURBANCES AND MECHANISM EXPORTED LOADS. WE WILL DEVELOP THESE MODELS FROM THE GROUND UP STARTING FROM COMPONENT MODELS PROVIDED BY NASA SUCH AS STRUCTURAL AND OPTICAL MODELS AND MATERIAL PROPERTIES. WE WILL ALSO ADDRESS THE UNIQUE THERMAL AND CRYOGENIC DESIGN CHALLENGES OF THE OST THROUGH TARGETED ANALYSIS AND MODELING WHERE POSSIBLE. WE WILL LEVERAGE SUBSTANTIAL LOCKHEED MARTIN RESEARCH AND DEVELOPMENT FUNDING THAT IS SPECIFICALLY IDENTIFIED AND ALLOCATED IN SUPPORT OF THIS RESEARCH AS WELL AS THE PRIOR WORKING RELATIONSHIPS THAT WE HAVE DEVELOPED IN OUR ACTIVE PARTICIPATION WITH NASA IN 2017 AS PART OF THE LARGE TELESCOPE COOPERATIVE RESEARCH CONTRACTS IN SUPPORT OF LUVOIR AND OST. LOCKHEED MARTIN SPACE BRINGS UNIQUE CAPABILITIES IN VIBRATION ISOLATION AND PICOMETER LEVEL STABILITY PIONEERED AT ITS ADVANCED TECHNOLOGY CENTER AND FOR THIS EFFORT WE HAVE PARTNERED WITH HARRIS UTC AND COHERENT-TINSLEY TO PROVIDE LEADING TECHNOLOGY IN OPTICAL MATERIALS MECHANISMS AND STRUCTURES. FINALLY LM SPACE IS COMMITTING SUBSTANTIAL INTERNAL RESEARCH AND DEVELOPMENT FUNDS IN CALENDAR YEARS 2018 AND 2019 IN SUPPORT OF THIS EFFORT IN ADDITION TO EXTANT TESTBED HARDWARE. BY LEVERAGING OUR OWN EXPERIENCE AND CAPABILITIES IN LARGE OPTICAL SYSTEMS AS WELL AS THAT OR PARTNERS IN THIS PROPOSED EFFORT WE ARE CONFIDENT THAT THE LOCKHEED MARTIN TEAM CAN PROVIDE NASA WITH VALUABLE DESIGN TOOLS AND TECHNOLOGY PLANS TO SUPPORT ITS LARGE SEGMENTED OPTICAL OBSERVATORY VISION FOR THE 2020 DECADAL SURVEY.$894,483
· FY2020 · National Aeronautics and Space Administration
CORONAL MASS EJECTIONS (CMES) AND LARGE SOLAR FLARES PRODUCE THE STRONGEST SPACE WEATHER DISTURBANCES, AND ARE DRIVEN BY THE RELEASE OF STORED MAGNET$868,281
· FY2014 · National Aeronautics and Space Administration
JOINT MULTI-ROLE TECHNOLOGY DEMONSTRATOR ARCHITECTURE IMPLEMENTATION PROCESS DEMONSTRATIONS$696,218
· FY2016 · Department of Defense
NUCLEAR ENERGY ENABLING TECHNOLOGIES - REACTOR MATERIALS$624,630
· FY2012 · Department of Energy
MAGNETIC FIELDS IN THE ATMOSPHERES OF SUN-LIKE STARS ARE THE BRIDGE BETWEEN THE DYNAMO ACTIVITY OCCURRING IN STELLAR INTERIORS AND THEIR OBSERVABLE CHARACTERISTICS. OBSERVATIONAL EVIDENCE OF MAGNETIC FIELDS AND MAGNETIC PROXIES SHOW THAT SUN-LIKE STARS SPAN THE GAMUT OF ACTIVITY LEVELS RANGING FROM EXTREMELY QUIET STARS TO HIGHLY VARIABLE STARS POSSESSING STARSPOTS OR STARSPOT GROUPS COVERING A LARGE FRACTION OF THE STELLAR SURFACE. FURTHERMORE COMPARATIVE STUDIES SHOW THE SUN IS FAR FROM A TYPICAL STAR. IN THIS PROJECT WE AIM TO ANSWER THE FOLLOWING SCIENCE QUESTIONS: WHAT CONSTRAINTS CAN MEASUREMENTS OF MAGNETIC SPOTS DIFFERENTIAL ROTATION AND FLARES ON OTHER STARS TEACH US ABOUT THE SOLAR DYNAMO? WHAT ARE THE LIMITS OF OBSERVATIONAL INFERENCE OF MAGNETIC FIELDS AND DIFFERENTIAL ROTATION ON OTHER STARS? WHAT ARE THE CORONAL MAGNETIC CONFIGURATIONS ASSOCIATED WITH SUPERFLARE EVENTS (AS OBSERVED FOR EXAMPLE IN WHITE LIGHT PHOTOMETRIC DATA IN KEPLER)? WHAT IS THE IMPORTANCE OF WELL-KNOWN PHYSICAL PROCESSES ON THE SUN (INCLUDING FLUX EMERGENCE DIFFERENTIAL ROTATION TURBULENT DIFFUSION) FOR MAGNETIC ACTIVITY ON OTHER STARS?$624,176
· FY2020 · National Aeronautics and Space Administration