COMPACTS OBJECTS IN OUR GALAXY PROVIDE AN EXCELLENT LABORATORY IN WHICH TO STUDY MATTER IN EXTREME CONDITIONS. OF MOST INTEREST ARE NEUTRON STARS (NS) AND BLACK HOLES (BH) IN BINARY SYSTEMS WHERE THE COMPACT OBJECT ACCRETES MATERIAL FROM ITS COMPANION STAR EITHER THROUGH ROCHE LOBE OVERFLOW OF THROUGH A STELLAR WIND FROM THE COMPANION. THE INFLOWING MATERIAL FORMS AN ACCRETION DISK AROUND THE COMPACT OBJECT WITH TEMPERATURES HOT ENOUGH TO PRODUCE COPIOUS AMOUNTS OF THERMAL X-RAYS AND GIVING RISE TO A CORONA OF NONTHERMAL ELECTRONS EMITTING IN THE HARD X-RAY BAND. .THE HARD X-RAY (E>3 KEV) BANDPASS PROVIDES ESSENTIAL DIAGNOSTIC INFORMATION ON ACCRETION STATE OF THE SOURCE AND CLUES TO THE NATURE OF THE COMPACT OBJECT IN THE SYSTEM. THE HIGH (E>20 KEV) SPECTRUM OF THE X-RAY BINARIES IN THE GALACTIC PLANE HAVE BEEN SURVEYED WITH LOW SPECTRAL RESOLUTION INSTRUMENTS ON INTEGRAL AND SWIFT. TARGETED OBSERVATIONS WITH NUSTAR HAVE DEMONSTRATED THE DIAGNOSTIC POWER OF A SENSITIVE INSTRUMENT OVER THE 3-79 KEV BANDPASS BUT UNFORTUNATELY SUCH OBSERVATIONS ARE NECESSARILY SHORT AND SPARSE FOR BRIGHT TARGETS DUE TO TELEMETRY RESTRICTIONS. .WHILE NUSTAR IS THE FIRST FOCUSING HARD X-RAY SATELLITE IN ORBIT THE OPEN GEOMETRY OF THE MAST THAT CONNECTS THE OPTICS BENCH TO THE FOCAL PLANE BENCH ALLOWS FOR THE POSSIBILITY OF STRAY LIGHT SHINING ON THE DETECTORS FROM X-RAY SOURCES WITHIN 1-4 DEGREES OF THE TELESCOPE AIM POINT. USING THE COLLIMATOR INSTRUMENT RESPONSE IS RELATIVELY SIMPLE AND EASY TO ANALYZE AND HAS ALREADY BEEN SHOWN TO BE SCIENTIFICALLY VALUABLE. .THERE ARE SEVERAL HUNDRED UNEXPLORED NUSTAR OBSERVATIONS WHERE THE PRIMARY SCIENCE TARGET IS CLOSE ENOUGH TO A BRIGHT GALACTIC XRAY BINARY SUCH PART OF THE NUSTAR FIELD-OF-VIEW CAPTURES THE STRAY LIGHT EMISSION FROM THE X-RAY BINARY. .FOR THIS PROJECT WE WILL MINE THIS SERENDIPITOUS DATA SET TO STUDY GALACTIC X-RAY BINARIES. WE WILL PRODUCE DATA PRODUCTS FOR 20-30 BRIGHT BLACK HOLE AND NEUTRON STAR X-RAY BINARIES THAT ARE OFTEN SEEN IN STRAY LIGHT. THE PRODUCTS WILL INCLUDE LIGHT CURVES IN MULTIPLE ENERGY BANDS OBSERVATION-BY-OBSERVATION SPECTRA STACKED SPECTRA OF STABLE SOURCES AND POWER SPECTRA OF THESE SOURCES. USING THESE PRODUCTS WE WILL: CHARACTERIZE THE VARIABILITY OF THE X-RAY BINARIES ON SHORT AND LONG TIME SCALES; SEARCH FOR RARE PHENOMENA SUCH AS X-RAY BURSTS FROM NEUTRON STARS FLARES OR DIPS; PIN POINT SPECTRAL STATE CHANGES; STUDY THE EVOLUTION OF QUASI-PERIODIC OSCILLATIONS AND OTHER TIMING PHENOMENA WITH THE SOURCE STATE; AND LOOK FOR VARIATIONS IN IRON EMISSION LINES SUCH AS THE RELATIVISTIC LINES SEEN FOR ACCRETING BLACK HOLES AND THE PRESENCE OF NON-THERMAL HARD X-RAY TAILS SEEN IN LMXB NEUTRON STAR SYSTEMS. .