GOAL AND OBJECTIVES THE GOAL OF THIS PROPOSAL IS TO ANSWER THE QUESTION - HOW AND WHY DOES THE SUN VARY. RECENT OBSERVATIONS IN EXTREME ULTRA-VIOLET WAVELENGTHS HAVE SHOWN THAT THE CORONA OSCILLATES AT MANY DIFFERENT SPATIAL SIZES AND TEMPORAL FREQUENCIES. HOWEVER MUCH REMAINS UNKNOWN ABOUT MANY OF THESE OSCILLATIONS; THEY ARE INTERMITTENT FOR UNKNOWN REASONS APPEAR ON SOME CORONAL FEATURES AND NOT ON OTHER SIMILAR NEIGHBORING FEATURES AND MAY (OR MAY NOT) BE MAGNETOHYRODYNAMIC WAVE MODES. DEFINITIVE CAUSES OF THE STRUCTURE AND ORIGINS OF THESE OSCILLATIONS IS STILL LARGELY LACKING. WE PROPOSE TO STUDY HOW AND WHY FEATURESIN THE CORONA OSCILLATE AND IF THEY OSCILLATE AS IDENTIFIABLE WAVE MODES. WE WILL MAKE USE OF AUTOMATED DETECTION AND CLASSIFICATION ALGORITHMS TO TAKE FULL ADVANTAGE OF THE LARGE VOLUME OF SDO-AIA DATA AVAILABLE. FIRST WE WILL MEASURE THE OSCILLATION CONTENT OFDIFFERENT PHYSICAL REGIONS ON THE SUN IN SDO AIA DATA. WE WILL DO THIS USING THREE DIFFERENT AUTOMATED OSCILLATION DETECTION ALGORITHMS (DEVELOPED PREVIOUSLY) TO VALIDATE THE RESULTS. THE MEASURED OSCILLATION CONTENT WILL BE CORRELATED WITH OTHER MEASURES OF THOSE REGIONS SUCH AS AREA TOTAL UNSIGNED MAGNETIC FLUX AND AGE TO OBTAIN BASIC INFORMATION ON THE PHYSICAL CONDITIONS NECESSARY FOR AN OSCILLATION TO OCCUR BASIC INFORMATION THAT HAS AS YET NOT BEEN OBTAINED. WE WILL EXTRACT ALL THIS CONTENT IN EACH AIA PASSBAND. FURTHER WEWILL ROUTINELY MEASURE THE CORONAL OSCILLATION CONTENT OF THE SUN IN THE CURRENT SOLAR CYCLE AND PROVIDE THOSE MEASUREMENTS ONLINE. SECOND WE NEED TO KNOW THE PHYSICAL SIZE OF THE COHERENT OSCILLATING STRUCTURE AND WHAT KIND OF STRUCTURE THE OSCILLATIONS OCCUR ON. WE WILL DO THIS BY IMPLEMENTING PIXEL GROUPING AND OSCILLATORY SIGNAL COHERENCE ALGORITHMS TO DETECT COHERENTLY OSCILLATING STRUCTURES. FURTHER WE WILL DEVELOP A 3D WAVELET ALGORITHM AND A CURVELET-BASED TEXTURE ANALYSIS THAT CAN DISTINGUISH BETWEEN NARROW AND EXTENDED CURVILINEAR FEATURES SUCH AS CORONAL LOOPS AND NON-LOOP EMISSION ON THE SUN. THIS WILL ALLOW US TO IDENTIFY LOOP-LIKE FEATURES AT MULTIPLE LENGTH-SCALES (LARGE LOOPS IN ACTIVE REGIONS SMALL LOOPS IN CORONAL HOLES AND QUIET SUN) AND OTHER TYPES OF EMISSION SUCH AS PLAGE OR MOSS IN EACH AIA PASSBAND. THIRD WE WILL STUDY OF ORIGINS OF LONGITUDINAL OSCILLATIONS AND FLARE-INDUCED KINK WAVES. THE COMBINATION OF AUTOMATED DETECTION OF THE OSCILLATIONS AND THE STRUCTURE SUPPORTING THESE OSCILLATIONS AS MEASURED IN EACH OF THE SDO PASSBANDS WILL ALLOW US TO TEST THEORIES OF OSCILLATION PROPAGATION CORONAL HEATING AND ENERGY DECAY MECHANISMS IN THE SOLARATMOSPHERE. RELEVANCE TO NASA THIS PROPOSAL ADDRESSES THE SCIENCE STRATEGIC GOAL 2 TO EXPAND SCIENTIFIC UNDERSTANDING OF THE EARTH AND THE UNIVERSE IN WHICH WE LIVE OUTCOME 2.2 TO UNDERSTAND THE SUN AND ITS INTERACTIONS WITH EARTH AND THE SOLAR SYSTEM OFTHE 2011 NASA STRATEGIC PLAN AND SCIENCE QUESTION WHAT CAUSES THE SUN TO VARY OBJECTIVE UNDERSTAND THE FUNDAMENTAL PHYSICAL PROCESSES OF THE SPACE ENVIRONMENT FROM THE SUN TO EARTH TO OTHER PLANETS AND BEYOND TO THE INTERSTELLAR MEDIUM OF THE 2010 SCIENCE PLAN FOR NASA S SCIENCE MISSION DIRECTORATE.