THE SOLAR WIND PLAYS A FUNDAMENTAL ROLE IN SHAPING THE HELIOSPHERE AND GOVERNING THE INTERACTIONS IN THE NEAR EARTH SPACE ENVIRONMENT AND ATMOSPHERE AND IT ULTIMATELY DRIVES THE CONDITIONS IN THE REGION OF INTERPLANETARY SPACE THAT WILL BE EXPLORED BY HUMANS. DESPITE ITS IMPORTANCE AND ALL THE EFFORTS AIMED AT STUDYING IT THERE ARE STILL MANY UNANSWERED QUESTIONS REGARDING THE ORIGIN ACCELERATION AND EVOLUTION OF THE SOLAR WIND. TWO FUNDAMENTAL OPEN QUESTIONS IN SOLAR WIND SCIENCE ARE: 1) WHERE DOES THE SOLAR WIND PLASMA COME FROM I.E. FROM WHAT TYPE OF PLASMA STRUCTURES AND FROM WHAT REGIONS IN THE SOLAR ATMOSPHERE AND 2) HOW ISTHE SOLAR WIND HEATED AND ACCELERATED? WE PROPOSE TO DIRECTLY AND QUANTITATIVELY COMBINE HIGH-RESOLUTION OBSERVATIONS OF THE EUV EMISSION OF SOLAR CORONAL PLASMAS WITH IN-SITU PLASMA OBSERVATIONS OBTAINED DURING QUADRATURE BETWEEN ULYSSES SOHO AND HINODE TO ACHIEVE THREE GOALS: 1) TO DETERMINE THE SOURCE REGIONS OF THE FAST AND SLOW SOLAR WIND; 2) TO PROVIDE AN EMPIRICAL DETERMINATION OF WIND PLASMA PARAMETERS AND HEATING; AND 3) TO DEVELOP A PREDICTIVE TOOL THAT USES EMPIRICAL OR MODEL WIND TEMPERATURE DENSITY AND VELOCITY AS A FUNCTION OF DISTANCE FROM THE SUN TO PRODUCE DETAILED QUANTITATIVE PREDICTIONS OF THE EVOLUTION OF THE SOLAR WIND CHARGE STATE COMPOSITION. PREDICTED CHARGE STATES WILL BE USED TO DETERMINE BOTH THE FINAL FROZEN-IN CHARGE STATES IN THE SOLAR WIND AND THE X-RAY EUV AND UV EMISSION OF THE WIND SOURCE REGIONS IN THE INNER CORONA. THESE GOALS WILL BE ACHIEVED THROUGH A UNIQUE COMBINATION OF SPECTROSCOPIC AND IN SITU TECHNIQUES. WE WILL MEASURE THE PHYSICAL PROPERTIES OF THE SOLAR WIND SOURCE REGIONS USING HIGH-RESOLUTION SPECTRA FROM SOHO AND HINODE. WE WILL USE THE SPECTROSCOPIC MEASUREMENTS OF PLASMA PARAMETERS AS INPUT TO THE IONCOMPOSITION MODEL TOGETHER WITH AN ASSUMED PLASMA VELOCITY FUNCTION TO PREDICT ION COMPOSITION AS A FUNCTION OF DISTANCE FROM THE WIND SOURCE REGION. THE ION COMPOSITION WILL BE USED TO 1) COMPARE FROZEN-IN CHARGE STATES WITH ULYSSES MEASUREMENTS AT ONE END OF THE SOLAR WIND TRAJECTORY AND 2) CALCULATE LINE INTENSITIES AND NARROW-BAND IMAGES IN THE INNERMOST REGIONS OF THE SOLAR CORONA TO BE COMPARED WITH OBSERVATIONS FROM THE SPECTROMETERS ON BOARD SOHO AND HINODE AT THE OTHER END OF THE WIND TRAJECTORY. THIS DOUBLE COMPARISON WILL ALLOW US TO: 1) TEST THE ACCURACY OF THE IONIZATION MODEL'S PREDICTION 2) DIRECTLY TEST THE WIND PLASMA PARAMETERS (DENSITY TEMPERATURE AND VELOCITY) USED AS INPUT TO THE IONIZATION MODEL; AND 3) DEVELOP AN EMPIRICAL MODEL OF THE PLASMA VELOCITY ACCELERATION AND THERMAL HISTORY BELOW 1.5 SOLAR RADII. THE RESULTS OF THIS PROPOSED WORK WILL BE TWOFOLD. FIRST WE WILL PROVIDE THE COMMUNITY WITH A NEW POWERFUL TOOL TO PREDICT THE EVOLUTION OF ION CHARGE STATES IN THE SOLAR WIND AS WELL AS A NEW METHODOLOGY TO STUDY THE SOLAR WIND QUANTITATIVELY MATCHING TWO COMPLETELY DIFFERENT TYPES OF OBSERVATIONS: REMOTE-SENSING OBSERVATIONS AND IN-SITUION COMPOSITION MEASUREMENT. SECOND THE APPLICATION OF THIS NEW METHODOLOGY TO EXISTING IN SITU AND REMOTE SENSING OBSERVATIONS WILL RESULT IN A) AN ACCURATE EMPIRICAL DESCRIPTION OF THE WIND HEATING AND ACCELERATION; AND B) THE IDENTIFICATION OF THE WIND SOURCE REGIONS. RESULTS FROM THE PROPOSED INVESTIGATIONS WILL PROVIDE CRITICAL INPUT TO THEORETICAL MODELS OF SOLAR WIND HEATING AND ACCELERATION. THE PROPOSED INVESTIGATION WILL PAVE THE WAY TO A NEW METHOD TO STUDY EXISTING DATA FROM NASA MISSIONS AND INSTRUMENTS ENHANCING THEIR SCIENTIFIC RETURN. THE GOALS OF THE PROPOSED INVESTIGATION ARE OF DIRECT FUNDAMENTAL IMPORTANCE TO NASA'S STRATEGIC GOAL 2.2("UNDERSTAND THE SUN AND ITS INTERACTIONS WITH EARTH AND THE SOLAR SYSTEM") AND ARE IN LINE WITH THE GOALS OF ALL THE NASA MISSIONS AND INSTRUMENTS INVOLVED IN THE PROPOSED WORK: ULYSSES HINODE AND SOHO.