IN RESPONSE TO THE HELIOPHYSICS GUEST INVESTIGATORS SOLICITATION WE INTEND TO DISCOVER AND CHARACTERIZE THE FUNDAMENTAL PROCESSES THAT OCCUR BOTH WITHIN THE HELIOSPHERE AND THROUGHOUT THE UNIVERSE BY IMPROVING OUR OBSERVATIONAL KNOWLEDGE OF MAGNETIC RECONNECTION. WE PROPOSE TO MAKE SIGNIFICANT CONTRIBUTIONS TO THIS ACTIVE AREA OF RESEARCH BY CONNECTING VARIOUS REMOTE SENSING OBSERVATIONS OF THE SOLAR CORONA WITH IN SITU MAGNETOSPHERIC DATA. THIS INTERDISCIPLINARY COLLABORATION WILL AID IN UNDERSTANDING THE ORIGIN OF THE SUN S ACTIVITY AND PREDICT THE VARIATIONS IN THE SPACE ENVIRONMENT AS WELL AS THE DYNAMICS AND COUPLING OF EARTH S MAGNETOSPHERE IONOSPHERE AND ATMOSPHERE AND THEIR RESPONSE TO SOLAR AND TERRESTRIAL INPUTS. THE MAIN FOCUS OF THIS STUDY IS SOLAR TRANSIENT EVENTS BUT WILL INCLUDE ASPECTS OF THE SOLAR ATMOSPHERE PARTICLE ACCELERATION TRANSPORT MODULATION IN THE HELIOSPHERE AS WELL AS THE MAGNETOSPHERE - IONOSPHERE COUPLING/MAGNETOTAIL. WHILE DIRECT OBSERVATIONS OF THE EXACT LOCATION OF MAGNETIC RECONNECTION HAVE ELUDED SOLAR RESEARCHERS NUMEROUS POTENTIAL INFLOWS AND OUTFLOWS FROM THESE EVENTS HAVE BEEN OBSERVED (E.G. SAVAGE ET AL 2012). OF PARTICULAR INTEREST ARE THE REGIONS OF DENSITY DEPLETION BEHIND OUTFLOWING LOOPS (KNOWN AS SUPRA ARCADE DOWNFLOWING LOOPS --- SADLS) OBSERVED AS SUPRA ARCADE DOWNFLOWS (SADS). AS THE OUTFLOWING LOOPS DESCEND THROUGH REGIONS OF ENHANCED DENSITY (THE SUPRA ARCADE FAN) THE RETRACTING LOOPS COLLECT PLASMA ON THE LEADING EDGE CREATING A WAKE OF RARIFIED PLASMA BEHIND WHICH APPEAR AS TEARDROP-SHAPED TROUGHS BEHIND THE DESCENDING LOOPS. THE SPEED SIZE AND ORIENTATION OF THE SADS AND SADLS CAN TELL US ABOUT THE CONDITIONS FACILITATING MAGNETIC RECONNECTION. IN MAGNETOSPHERIC SUBSTORMS IT IS PREDICTED THAT SIMILAR WAKES SHOULD BE FOUND BEHIND DIPOLARIZATION FRONTS. WHEN RECONNECTION OCCURS IN THE EARTH S MAGNETOTAIL MAGNETIC FIELD LINES CONNECT THE EARTH S POLES ON THE NIGHT SIDE OF THE EARTH. THESE FIELD LINES APPEAR MORE DIPOLAR AND DESCEND TOWARDS THE EARTH. BEHIND THESE DESCENDING DIPOLARIZATION FRONTS NOTABLE RARIFIED PLASMA IS EXPECTED SIMILAR TO THE SADS SEEN IN THE CORONAL CASE. THIS STUDY WILL UTILIZE ARCHIVAL DATA FROM A HOST OF HELIOSPHERIC MISSIONS PARTICULARLY HINODE'S X-RAY TELESCOPE (XRT). TO IMPROVE KNOWLEDGE OF THE CORONAL ASPECT OF SADS FLOW TRAJECTORIES IN CORRELATION TO SOFT X-RAY LIGHTCURVES FROM THE XRT WILL BE COMBINED WITH OBSERVATIONS FROM HINODE'S EXTREME ULTRAVIOLET IMAGING SPECTROMETER THE SOLAR DYNAMICS OBSERVATORY'S ATMOSPHERIC IMAGING ASSEMBLY AND THE RAMATY HIGH ENERGY SOLAR SPECTROSCOPIC IMAGER (RHESSI) IN ORDER TO ESTIMATE THE TEMPERATURE AND DENSITY AROUND THESE FLOWS CONTEXTUAL MAGNETIC FIELD ALIGNMENT HEATING AND NON-THERMAL PARTICLE ACCELERATION. ADDITIONAL INFORMATION FROM THE EXTENDED CORONA WILL BE PROVIDED BY THE LARGE ANGLE AND SPECTROMETRIC CORONAGRAPH EXPERIMENT ON THE SOLAR AND HELIOSPHERIC OBSERVATORY AND THE CORONAGRAPHS ON THE SOLAR TERRESTRIAL RELATIONS OBSERVATORY. A VITAL AND UNIQUE ASPECT OF THIS STUDY IS THE INCORPORATION OF IN SITU DATA OF MAGNETOSPHERIC RECONNECTION EVENTS (SUBSTORMS) USING THE TIME HISTORY OF EVENTS AND MACROSCALE INTERACTIONS DURING SUBSTORMS (THEMIS). THE DATA FROM UP TO 5 THEMIS SPACECRAFT WILL PROVIDE INFORMATION CONCERNING THE ACTUAL LOCAL PLASMA PARAMETERS (TEMPERATURE DENSITY VELOCITIES ELECTRIC FIELDS AND MAGNETIC FIELDS) AROUND OUTFLOWING LOOPS VIA THE ELECTROSTATIC ANALYZER AND SOLID STATE TELESCOPE WHILE THE COIL MAGNETOMETER DIRECTLY MEASURES THE MAGNETIC FIELD AROUND THE RECONNECTION REGION. WITH THEMIS WE CAN DIRECTLY MEASURE PLASMA PROPERTIES THAT CAN ONLY BE ROUGHLY ESTIMATED IN THE CORONA WITH REMOTE SENSING OBSERVATORIES. CONVERSELY IT IS INTENDED THAT THE MORPHOLOGICAL DATA AVAILABLE FROM REMOTE SENSING OF THE CORONAL REGIME MAY ALSO HELP INFORM MAGNETOSPHERIC OBSERVATIONS.