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SS73 17 was an innocuous Mira-type symbiotic star until Integral and Swiftdiscovered its bright hard X-ray emission, adding it to the small class of"hard X-ray emitting symbiotics." Suzaku observations in 2006 then showed itemits three bright iron lines as well, with little to no emission in the 0.3-2keV bandpass. We present here followup observations with the Chandra HETG andSuzaku that confirm the earlier detection of strong emission lines of Fe Kalphafluorescence, Fe XXV and Fe XXVI but also show significantly more soft X-rayemission. The high resolution spectrum also shows emission lines of otherhighly ionized ions as Si XIV and possibly S XVI. In addition, a reanalysis ofthe 2006 Suzaku data using the latest calibration shows that the hard (15-50keV) X-ray emission is brighter than previously thought and remains constant inboth the 2006 and 2008 data.  The G ratio calculated from the Fe XXV lines shows that these lines arethermal, not photoionized, in origin. With the exception of the hard X-rayemission, the spectra from both epochs can be fit using thermal radiationassuming a differential emission measure based on a cooling flow model combinedwith a full and partial absorber. We show that acceptable fits can be obtainedfor all the data in the 1-10 keV band varying only the partial absorber. Basedon the temperature and accretion rate, the thermal emission appears to bearising from the boundary layer between the accreting white dwarf and theaccretion disk.

High-resolution X-ray Spectra Of The Symbiotic Star SS73 17