WE PROPOSE TO BUILD AND FLY A VUV SOUNDING ROCKET SPECTROMETER FURST: THE FULL-SUN ULTRAVIOLET ROCKET SPECTROGRAPH TO OBTAIN THE FIRST HIGH RESOLUTION HIGH QUALITY VUV SPECTRUM OF THE SUN-AS-A-STAR. OUR PROPOSED SPECTROMETER COVERS THE 112-200 NM WAVELENGTH RANGE WITH A SPECTRAL RESOLUTION R>20 000 AND WILL UNDERGO ABSOLUTE RADIOMETRIC AND WAVELENGTH CALIBRATION PRIOR TO LAUNCH. OUR TEAM'S EXTENSIVE COMBINED EXPERIENCE HAS BEEN BROUGHT TO BEAR TO PRODUCE AN ELEGANT AND ROBUST PAYLOAD DESIGN THAT SIMPLIFIES CALIBRATION AS WELL AS DEPLOYMENT AND OPERATION IN SPACE. A DEFINING GOAL OF HELIOPHYSICS IS TO UNDERSTAND THE INFLUENCE OF SOLAR RADIATION PLASMA AND MAGNETIC FIELD WITH INTERPLANETARY SPACE WITH THE PLANETS AND SMALLER SOLAR SYSTEM BODIES. STRIKINGLY NO HIGH RESOLUTION SPECTRUM OF SOLAR IRRADIANCE EXISTS AND CONSTRUCTION OF SUCH A SPECTRUM FROM EXISTING DATA AND MODELS IS FRAUGHT WITH DIFFICULTIES. IN CONTRAST HUBBLE SPACE TELESCOPE (HST) DATA OF OBJECTS INCLUDING SUN-LIKE STARS SUCH AS ALPHA CEN A ARE OF FAR HIGHER QUALITY THAN SOLAR DATA. THUS WE ARE FACING THE PECULIAR FACT THAT WE KNOW THE INPUTS OF VUV RADIATION TO THE HELIOSPHERE OF A PLANET SURROUNDING ALPHA CEN A FAR MORE PRECISELY THAN WE CAN FOR OUR OWN HELIOSPHERE! CRITICALLY A RESOLUTION OF>10 000 (<30 KM/S) IS NEEDED IN THE HELIOSPHERE AS MANY OBJECTS (PLANETARY SATELLITES COMETS MAGNETOSPHERES) HAVE COMPARABLE ORBITAL AND PLASMA SPEEDS. UV MONITOR EXPERIMENTS (INCLUDING THOSE ON AE SATELLITES SME SOLSTICE EVE ON SDO) HAVE R<1200 OR SO ARE QUITE INADEQUATE FOR DEFINING ACCURATE IRRADIANCES NEEDED FOR THE INPUTS TO MANY HELIOSPHERIC PROBLEMS OF INTEREST. AS WELL AS ADVANCING HELIOSPHERIC PHYSICS OUR EXPERIMENT WILL PROVIDE A CRITICALMISSING LINK BETWEEN THE SUN AND THE STARS WHICH WILL ENABLE UNIQUE INSIGHTS INTO THE HEATING OF THE CHROMOSPHERE AND CORONA. HST STELLAR SPECTRA WITH R>10 000 CONTAIN IMPORTANT SIGNATURES OF MAGNETIC RECONNECTION ACCRETION OTHER MAGNETIC PROCESSES AND INTERSTELLAR ABSORPTION. BUT WE CANNOT CURRENTLY UNDERSTAND HOW THESE DIAGNOSTIC FEATURES RELATE TO THE SPATIALLY RESOLVED DATA WITH R>10 000 ON THE SUN. THE UNKNOWN CENTER-TO-LIMB VARIATIONS OF BRIGHTNESS WITH WAVELENGTHS ACROSS LINE PROFILES PRESENTS A FUNDAMENTAL CHALLENGE FOR WHICH DATA SIMPLY DO NOT EXIST. OUR AIM WILL BE TO DELIVER A FULLY CALIBRATED UV SPECTRUM TO THE COMMUNITY AT THE EARLIEST OPPORTUNITY. THIS WILL FOSTER CROSS-COMMUNITY COLLABORATIONS ACROSS HELIO- AND ASTRO- PHYSICS INCLUDING SOME NEEDS FOR AERONOMY OF PLANETARY ATMOSPHERES INCLUDING THOSE OUTSIDE OF THE SOLAR SYSTEM. THE ANALYSIS OF FURST DATA WILL SHED LIGHT ON THE FUNDAMENTAL PROCESSES OF CHROMOSPHERIC AND CORONAL HEATING BY FOCUSING UPON SOMETIMES SUBTLE YET VERY SIGNIFICANT DIFFERENCES IN HIGH QUALITY UV SPECTRA OF THE SUN AND THE STARS. HST DATA EXIST FOR A DOZEN OR SO SUN-LIKE STARS OF A QUALITY ALREADY BEYOND OUR ABILITY TO CONSTRUCT A COMPARABLE SUN-AS-A-STAR UV SPECTRUM. THE NEW SOLAR SPECTRA WILL ENABLE US TO UNDERSTAND THE NATURE OF MAGNETIC ENERGY DISSIPATION AS A SUN-LIKE STAR EVOLVES AND THE DEPENDENCE OF MAGNETIC ACTIVITY ON STELLAR MASS AND METALLICITY. THIS PROPOSED RESEARCH ADDRESSES THREE OF THE FOUR MAIN GOALS OF HELIOPHYSICS AS ARTICULATED BY THE DECADAL PANEL: 1. DETERMINE THE ORIGINS OF THE SUN'S ACTIVITY AND PREDICT THE VARIATIONS IN THE SPACE ENVIRONMENT FORM NRESS-300 VERSION 3.0 APR 09 3. DETERMINE THE INTERACTION OF THE SUN WITH THE SOLAR SYSTEM AND THE INTERSTELLAR MEDIUM. 4. DISCOVER AND CHARACTERIZE FUNDAMENTAL PROCESSES THAT OCCUR BOTH WITHIN THE HELIOSPHERE AND THROUGHOUT THE UNIVERSE.