WE PROPOSE TO USE DATA FROM THE INTERFACE REGION IMAGING SPECTROGRAPH (IRIS) THE SOLAR DYNAMICS OBSERVATORY (SDO) AND OTHER SOURCES TO MEASURE THE PROPERTIES OF SMALL-SCALE ERUPTIVE EVENTS IN PARTICULAR THEIR RELATION TO THE MAGNETIC FIELD STRUCTURE AND THE PHOTOSPHERIC FLOW FIELD WHICH PROVIDES IMPORTANT CONSTRAINTS ON ERUPTIVE EVENT MODELLING. SCIENCE GOALS AND OBJECTIVES: LARGE SCALE ERUPTIVE PHENOMENA LIKE FLARES AND CORONAL MASS EJECTIONS ARE SOME THE MOST STUDIED TOPICS IN SOLAR PHYSICS DUE TO THEIR ROLE IN THE RELEASE OF ENERGY MASS AND MAGNETIC FIELD WHICH CAN IMPACT EARTH ENVIRONMENT. AMONG THE SMALL-SCALE TYPES OF ERUPTIONS CORONAL JETS EMANATING FROM CORONAL BRIGHT POINTS (CBPS) HAVE RECEIVED MOST OF THE ATTENTION IN RECENT YEARS (E.G. MUGLACH&YOUNG 2014). ONE OF THE SMALLEST KINDS OF ERUPTIVE EVENTS ON THE SUN ARE TRANSITION REGION EXPLOSIVE EVENTS (EES) WITH SPATIAL SCALES OF ONLY ABOUT 1" - 2". A RECENT CASE STUDY HAS SHOWN HOW EES END UP AT THE INTERSECTION OF THE SUPERGRANULAR BOUNDARIES (ATTIE ET AL. 2016) WHICH EMPHASIZES THE INTERACTION BETWEEN THE MAGNETIC FIELD EVOLUTION AND THE PHOTOSPHERIC FLOWS ALL OVER THE QUIET SUN. ALL OF THESE PHENOMENA PROVIDE STRONG EVIDENCE FOR MAGNETIC RECONNECTION OCCURRING IN THE SUN'S ATMOSPHERE. TO UNDERSTAND THEM AND CONSTRAIN MODELS IT IS CRITICAL TO PROPERLY CHARACTERIZE THEM TO DETERMINE THE MAGNETIC EVOLUTION THAT LEADS TO THESE PHENOMENA AND RELATE THEM TO THE MAGNETIC STRUCTURE WHERE THEY OCCUR THE MAGNETIC NETWORK. WE PROPOSE TO USE DATA FROM IRIS AND SDO TO INVESTIGATE THESE SMALL-SCALE ERUPTIVE EVENTS. WE WILL ADDRESS THE FOLLOWING SPECIFIC QUESTIONS: WHERE ARE THESE EVENTS LOCATED (NETWORK CENTER OR BOUNDARY)? WHAT IS THE MAGNETIC FIELD EVOLUTION DURING EES AND JETS? HOW IS THE MAGNETIC FIELD EVOLUTION CONNECTED TO THE PHOTOSPHERIC PLASMA FLOWS? CAN WE USE THESE RESULTS TO SUPPORT SPECIFIC NUMERICAL MODELS FOR SMALL-SCALE ERUPTIVE EVENTS? NASA MISSION DATA TO BE USED IN THIS INVESTIGATION: PRIMARILY IRIS AND SDO/HMI AND AIA COMPLEMENTED BY HINODE/SOT WHEN AVAILABLE THE DATA ANALYSIS METHODOLOGY CONSISTS OF THE FOLLOWING STEPS USING WELL-DEVELOPED COMPUTATIONAL TOOLS AVAILABLE TO THE TEAM: - APPLYING THE EE IDENTIFICATION METHOD USED IN MUGLACH (2008) MODIFIED FOR IRIS SPECTRA AND CATEGORIZE EES ACCORDING TO THE SOLAR REGION (QUIET SUN CORONAL HOLE ACTIVE REGION). - PRODUCE EVENT LIST OF CORONAL HOLE BRIGHT POINTS WHICH COVER THEIR COMPLETE LIFE CYCLE. - COALIGN IRIS AND SDO DATA AND APPLY FEATURE TRACKING TO SDO HMI MAGNETOGRAMS TO OBTAIN THE EVOLUTION OF THE MAGNETIC FIELD FOR BOTH EES AND CBP. - USE LOCAL CORRELATION TRACKING AND BALLTRACKING TO CALCULATE THE FLOW FIELD FROM HMI WHITE LIGHT IMAGES AND DETERMINE EE AND CBP LOCATIONS WITHIN THE PHOTOSPHERIC FLOW PATTERN. - USE THE MAGNETIC BALLTRACKING ALGORITHM (ATTIE ET AL. 2016) TO RELATE THE DISPLACEMENT OF THE MAGNETIC FLUX PATCHES WITH RESPECT TO THE FLOW PATTERN. RELEVANCE: THE SCIENTIFIC GOALS OF SDO AND IRIS ARE TO IMPROVE OUR UNDERSTANDING OF THE FOLLOWING SCIENCE QUESTIONS (AMONG OTHERS): - HOW IS MAGNETIC FLUX SYNTHESIZED CONCENTRATED AND DISPERSED ACROSS THE SOLAR SURFACE? - HOW DOES MAGNETIC RECONNECTION ON SMALL SCALES REORGANIZE THE LARGE-SCALE FIELD TOPOLOGY AND CURRENT SYSTEMS? - HOW DO MAGNETIC FLUX AND MATTER RISE THROUGH THE LOWER ATMOSPHERE AND WHAT ROLE DO FLUX EMERGENCE AND SURFACE FLOWS PLAY IN SOLAR ERUPTIVE EVENTS? THIS INVESTIGATION ADDRESSES TWO OF THE FOUR HIGH-LEVEL SCIENCE GOALS OF THE HELIOPHYSICS DECADAL SURVEY: 1.DETERMINE THE ORIGINS OF THE SUN'S ACTIVITY AND PREDICT THE VARIATIONS IN THE SPACE ENVIRONMENT. 4.DISCOVER AND CHARACTERIZE FUNDAMENTAL PROCESSES THAT OCCUR BOTH WITHIN THE HELIOSPHERE AND THROUGHOUT THE UNIVERSE.