THIS RESEARCH PROJECT WILL MEASURE THE INFRARED SPECTRUM OF THE SOLAR CORONA USING A FOURIER TRANSFORM INFRARED SPECTROMETER (FTIR). NO SPECTRAL SURVEY OF THE INFRARED CORONA HAS EVER BEEN PERFORMED YET SOME OF THE MOST MAGNETICALLY SENSITIVE SPECTRAL LINES ARE THEORETICALLY PREDICTED IN THIS REGION. ALL OF THE INFRARED CORONAL LINES ARE FORBIDDEN LINES OF MAGNETIC DIPOLE CHARACTER. WE DO NOT KNOW HOW INFRARED EMISSION LINE INTENSITIES ARE DISTRIBUTED IN THE CORONA NOR DO WE KNOW WAVELENGTHS ACCURATELY ENOUGH TO DETERMINE DETRIMENTAL EFFECTS OF TELLURIC ABSORPTION ON THESE PARTICULAR LINES. THE ABILITY TO MEASURE THE MAGNETIC FIELD OF THE CORONA IS IMPERATIVE IF WE ARE TO ACCURATELY DIAGNOSE THE SOURCES OF SPACE WEATHER AND ULTIMATELY UNDERSTAND THE HEATING MECHANISMS OF THE SOLAR CORONA. WE INTEND TO COMPLETE AND OPTIMIZE AN FTIR INSTRUMENT THAT WILL MEASURE THE CORONAL SPECTRUM FROM ~2-12 MICRONS DURING THE 2017 ECLIPSE. WE WILL DEPLOY THE INSTRUMENT ALONG THE PATH OF TOTALITY IN WYOMING AT ~2900 MASL AND MEASURE THE CORONA AS THE MOON PASSES ACROSS THE SOLAR DISK. THE PRINCIPAL SCIENCE GOALS AND OBJECTIVES OF THIS PROJECT ARE (1) TO IDENTIFY SPECTRAL LINES IDEALLY SUITED TO MEASURE CORONAL MAGNETIC FIELDS (2) TO FIND THE RANGE OF TEMPERATURES SPANNED BY THE LINES (IONS FROM 6 TO 14 TIMES IONIZED) (3) TO IDENTIFY THE TYPICAL RANGE OF FEATURES SAMPLED BY THE LINES (ACTIVE REGIONS SOURCE REGIONS OF FAST AND SLOW SOLAR WIND) AND (4) TO DETERMINE WHERE CORONAL LINES LIE RELATIVE TO TELLURIC ABSORPTION FEATURES. THE DATA TO BE USED IN THIS PROJECT ARE MODERATE RESOLUTION (R=10000) INFRARED SPECTRA. OUR EFFORT WILL INCLUDE CALIBRATION OF THE WAVELENGTH SCALE. WE WILL IDENTIFY THE SPECTRAL FEATURES OF THESE SPECTRA AND COMPARE THE LINE INTENSITIES AND WAVELENGTHS WITH THEORETICAL PREDICTIONS. IN ADDITION WE WILL IDENTIFY WHERE THE LINES OF SOLAR ORIGIN LIE IN RELATION TO THE TELLURIC ABSORPTION FEATURES. WE WILL USE COMPLEMENTARY DATA FROM INSTRUMENTS ABOARD NASA SPACECRAFT TO PROVIDE SPATIAL CONTEXT FOR OUR RESULTS. THIS RESEARCH IS OF DIRECT RELEVANCE TO THE GOAL OF CONNECTING THE 2017 ECLIPSE TO THE STUDY OF THE SUN-EARTH SYSTEM. MEASURING THE IR SOLAR CORONA IS ONLY POSSIBLE IN THE EVENT OF AN ECLIPSE OR WITH A CORONAGRAPH. THE ECLIPSE OFFERS A UNIQUE OPPORTUNITY BY MAKING THE LOW CORONA (OTHERWISE OBSCURED BY THE OCCULTING DISK OF A CORONAGRAPH) VISIBLE. THESE OBSERVATIONS WILL LEAD TO THE IDENTIFICATION OF MAGNETICALLY SENSITIVE EMISSION LINES THAT CAN ULTIMATELY BE USED TO DIAGNOSE THE MAGNETIC FIELD OF THE SOLAR CORONA. MEASURING THIS MAGNETIC FIELD IS OF FUNDAMENTAL IMPORTANCE IN THE UNDERSTANDING OF THE SUN AND HOW IT INFLUENCES THE EARTH.