TOTAL SOLAR ECLIPSES PROVIDE VALUABLE OPPORTUNITIES FOR SOLAR AND PLANETARY ASTROPHYSICS. OBJECTS NORMALLY OVERWHELMED BY THE SUN S GLARE BECOME OBSERVABLE ALLOWING MEASUREMENTS THAT ARE OTHERWISE IMPOSSIBLE. USING AIRCRAFT FLYING ALONG THE ECLIPSE TRACK AT HIGH ALTITUDE IT IS POSSIBLE TO EXTEND THE AVAILABLE OBSERVING TIME WHILE SIMULTANEOUSLY REDUCING CONFOUNDING EFFECTS FROM EARTH S ATMOSPHERE. WE PROPOSE TO OBSERVE THE 21 AUG 2017 ECLIPSE WITH NASA S WB-57 AIRCRAFT AT ~50 KFT USING THE EXISTING WB-57-COMPATIBLE DYNAMITE VISIBLE AND NEAR-INFRARED (NIR) TELESCOPES TO MAKE RARE SOLAR AND PLANETARY OBSERVATIONS. THIS STRATOSPHERIC ALTITUDE ELIMINATES OBSCURATION BY CLOUDS AND SIGNIFICANTLY REDUCES SEEING EFFECTS BY TURBULENCE. DYNAMITE IS A FULLY-GIMBALED STABILIZED PLATFORM WITH TWO 9-INCH COALIGNED TELESCOPES WITH IMAGING CAPABILITY UP TO 60 HZ IN BOTH VISIBLE AND NIR. FIELDS-OF-VIEW ARE ~1X1.8 DEG (VISIBLE) AND ~0.7X1.3 DEG (NIR) WITH PLATESCALES OF ~3 /PIX. POINTING STABILITY IS<~1 RMS AT 20 HZ. THE INSTRUMENT CAN ACCOMMODATE NARROWBAND FILTERS OR POLARIZERS WITH ONLY MINOR MODIFICATION. NO ADDITIONAL INSTRUMENT DEVELOPMENT IS REQUIRED. OUR OBSERVATIONS ENABLE FOUR MAIN SCIENCE GOALS: (1) CHARACTERIZING THE FINE-SCALE STRUCTURE OF THE SOLAR CORONA OUT TO THE MID-CORONA ABOVE THE CONVENTIONAL SOURCE SURFACE AT 2.5 RS; (2) EXPLORING SMALL-SCALE TRANSIENT MOTIONS INCLUDING POSSIBLE HIGH-FREQUENCY (30-300 MHZ) WAVES IN THE CORONA; (3) NIR OBSERVATIONS OF MERCURY; AND (4) A SEARCH FOR POSSIBLE VULCANOID ASTEROIDS. THE PRIMARY GOAL OF OUR CAMPAIGN WILL BE TO CAPTURE THESE HIGHLY UNIQUE DATA WHICH WILL ENABLE FUTURE IN-DEPTH STUDIES THAT ADDRESS THE ABOVE SCIENCE IN DETAIL. HOWEVER WE INCLUDE SUFFICIENT SCOPE TO PUBLISH A FIRST-RESULTS PAPER AND IDENTIFY KEY FINDINGS. OBSERVATIONS OF THE SOLAR CORONA ARE GENERALLY LIMITED BY BOTH STRAY-LIGHT CONSTRAINTS AND BY EITHER TELEMETRY CONSTRAINTS FOR SPACEBORNE INSTRUMENTS OR ATMOSPHERIC EFFECTS FOR GROUND-BASED INSTRUMENTS. OUR CAMPAIGN WILL PROVIDE HIGH-RESOLUTION IMAGES WITH NONE OF THESE LIMITATIONS OUT TO AT LEAST 6 SOLAR RADII. DYNAMITE S HIGH CADENCE OVERSAMPLES THE FREQUENCY RANGE OF INTEREST PERMITTING HIGHER SENSITIVITY AND BETTER ATMOSPHERIC REJECTION THAN WOULD BE AVAILABLE WITH DIRECT 1 HZ SAMPLING. WE WILL USE ADVANCED IMAGE PROCESSING TECHNIQUES AS WELL AS FOURIER AND WAVELET ANALYSIS TO SEARCH FOR SHORT-TIMESCALE DYNAMICS AND WAVE-RELATED PHENOMENA THAT COULD BE RELATED TO THE HEATING OF THE CORONA AND THE ACCELERATION OF OUTFLOWS RELATED TO THE SOLAR WIND. A TARGET OF PARTICULAR INTEREST WILL BE CORONAL FANS: STRUCTURES ASSOCIATED WITH BUNDLES OF ELONGATED OPEN MAGNETIC FIELD LINES VISIBLE OUT TO SEVERAL SOLAR RADII. THESE STRUCTURES HAVE BEEN REPORTED IN EUV OBSERVATIONS BUT HAVE NOT BEEN WELL CHARACTERIZED IN VISIBLE LIGHT. THERE IS EVIDENCE THAT THESE STRUCTURES ARE RELATED TO BOTH WAVE-DRIVEN HEATING AND OUTFLOWS. BETTER CHARACTERIZATION OF THESE STRUCTURES IS ONE GOAL OF OUR COLLABORATION WITH OUR EUROPEAN PARTNERS. FOR PLANETARY SCIENCE WE WILL OBSERVE MERCURY AND SEARCH FOR VULCANOIDS. SINCE MESSENGER DID NOT OBSERVE MERCURY IN THE NIR OUR DYNAMITE OBSERVATIONS WILL HELP TO CONSTRAIN THE RATE OF COOLING OF MERCURY S NIGHTSIDE SURFACE. VULCANOIDS ARE HYPOTHESIZED ASTEROIDS BETWEEN THE SUN AND MERCURY THAT CAN ONLY BE STUDIED DURING ECLIPSES OR AT TWILIGHT. OUR OBSERVATIONS WILL PROVIDE UNPRECEDENTED SENSITIVITY TO THESE POSSIBLE SMALL BODIES. OUR CAMPAIGN ALSO PROVIDES COMPLEMENTARY DATA FOR A SEPARATELY-FUNDED PROGRAM BY COLLABORATORS MAKING ECLIPSE OBSERVATIONS USING AN AIRBORNE NIR SPECTROMETER AND SLIT-JAW IMAGER AND PROVIDES DATA FOR PREFLIGHT RADIOMETRIC MODELING AND CALIBRATION OF THE ASPIICS CORONAGRAPH ON THE EUROPEAN FORMATION-FLYING PROBA3 MISSION. THIS WORK HAS OBVIOUS RELEVANCE TO AND D