LARGE SCALE COORDINATION FOR SMALL SCALE STRUCTURES: CONNECTING TRANSIENT BRIGHTENINGS BETWEEN THE CORONA AND THE PHOTOSPHERE TRANSIENT BRIGHTENINGS (TBS) ARE UBIQUITOUS FEATURES OF THE SOLAR ATMOSPHERE ACROSS MANY LENGTH AND ENERGY SCALES THE MOST ENERGETIC OF WHICH MANIFEST AS LARGE-CLASS SOLAR FLARES. TBS TYPICALLY ORIGINATE IN HIGH MAGNETIC FLUX REGIONS AND ARE OBSERVED AS INCREASED EMISSION ACROSS WAVELENGTHS FROM X-RAY TO RADIO WITH NOTABLE DYNAMICS ON TIMESCALES OF SECONDS TO HOURS. CORONAL TBS ARE OFTEN STUDIED USING EUV AND X-RAY IMAGING AND SPECTRA. THE TBS LIKELY ORIGINATE FROM PHOTOSPHERIC ACTIVITY SUCH AS FLUX EMERGENCE BUT ARE PROXIMATELY DRIVEN BY ENERGY TRANSFER THROUGH THE CHROMOSPHERE EITHER BY CONVECTIVE WAVES DIRECT EJECTION OF CHROMOSPHERIC MATERIAL OR RECONNECTION. CHROMOSPHERIC AND TRANSITION REGION OBSERVATIONS OF THESE EVENTS HAVE NOT BEEN ROUTINE FOR THE LAST FEW DECADES. HOWEVER NEW INSTRUMENTS SENSITIVE TO CHROMOSPHERIC RADIATION HAVE BECOME AVAILABLE THAT SIGNIFICANTLY ENHANCE OUR ABILITY TO UNDERSTAND THE BI-DIRECTIONAL FLOW OF ENERGY THROUGH THE CHROMOSPHERE. IN THIS PROJECT WE WILL UTILIZE THESE NEW CHROMOSPHERIC OBSERVATIONS TO UNDERSTAND HOW CORONAL TBS ARE RELATED TO CHROMOSPHERIC BRIGHTENINGS AND WAVE SIGNATURES. THIS WILL PROVIDE TRANSFORMATIONAL INSIGHT INTO THE FLOW OF ENERGY THROUGH THE CHROMOSPHERE INTO THE CORONA AND THE FEEDBACK OF ENERGY BACK INTO THE CHROMOSPHERE. THIS COMPREHENSIVE STUDY WILL PROVIDE THE MOST COMPLETE VIEW OF CHROMOSPHERIC ACTIVITY RELATED TO SMALL SCALE BRIGHTENINGS IN THE CORONA AND CHROMOSPHERE TO DATE. RECENTLY WE OBTAINED A UNIQUELY EXTENSIVE DATA SET OF A SMALL ACTIVE AREA WITH WHICH TO STUDY THE BI-DIRECTIONAL ENERGY FLOW BETWEEN THE CHROMOSPHERE AND CORONA. THE OBSERVATIONS ALLOW US TO COMBINE SPECTRAL DATA FROM HINODE/EIS IRIS AND IBIS AT THE DUNN SOLAR TELESCOPE WITH IMAGING DATA TO TRACK PHOTOSPHERIC FLOWS WITH SDO/HMI AND HINODE/SOT; THROUGH THE CHROMOSPHERE AND TRANSITION REGION WITH SDO/AIA IBIS IRIS AND ALMA; AND INTO THE CORONA WITH HINODE/EIS HINODE/XRT AND AIA. WITHIN THE ACTIVE AREA STUDIED MANY TBS WERE DETECTED THROUGH MULTIPLE LAYERS OF THE SOLAR ATMOSPHERE. LESS EXPANSIVE DATA SETS HAVE PREVIOUSLY BEEN USED TO STUDY WAVE DYNAMICS IN THE CHROMOSPHERE BUT THEY WERE UNABLE TO CONCLUSIVELY CONNECT THIS WAVE ACTIVITY TO TBS. THE DATA WILL BE INTERPRETED BY COMPARISON TO SIMULATIONS THAT SOLVE AN EXTENDED SET OF THE FULL MHD EQUATIONS WITH LARE3D. RECENT THEORETICAL AND SIMULATION ADVANCES HAVE SHOWN A VARIETY OF PATHWAYS FOR WAVE ENERGY TO PROPAGATE HIGHER INTO THE ATMOSPHERE THAN WAS PREVIOUSLY DEEMED REALISTIC. THE NEW RESULTS CAN EXPLAIN IMPORTANT OBSERVATIONAL SIGNATURES OF WAVE ACTIVITY E.G. ACOUSTIC HALOS AND MAGNETIC SHADOWS AND ARE JUST STARTING TO BE USED TO DIRECTLY DETERMINE THE TYPES OF WAVES PRESENT AT DIFFERENT HEIGHTS IN THE SOLAR ATMOSPHERE THROUGH CHROMOSPHERIC AND CORONAL SEISMOLOGY. THE RELATIONSHIP BETWEEN WAVE ACTIVITY AND TBS IS UNCLEAR BUT THE SPATIAL CORRESPONDENCE IS SUGGESTIVE. BECAUSE LARE3D SOLVES THE FULL MHD EQUATIONS OUR SIMULATIONS ARE IDEAL FOR STUDYING BOTH THE WAVE AND NON-LINEAR ASPECTS (SHOCKS RECONNECTION) OF THE PLASMA. TRACING THE PLASMA DYNAMICS THROUGH CHROMOSPHERIC LAYERS BEFORE AND AFTER TBS WILL PROVIDE VALUABLE INSIGHT INTO THE PROPAGATION AND INITIATION OF WAVES THROUGH THE SOLAR ATMOSPHERE AND THE INTERPLAY BETWEEN WAVES AND MAGNETIC RECONNECTION IN THE SOLAR ATMOSPHERE. THESE RESULTS CAN HELP TO DETERMINE THE ORIGINS OF THE SUN S ACTIVITY AS WELL AS DISCOVER AND CHARACTERIZE FUNDAMENTAL PROCESSES THAT OCCUR BOTH WITHIN THE HELIOSPHERE AND THROUGHOUT THE UNIVERSE. THIS STUDY WILL ADDRESS THE CHALLENGES OF THE DECADAL SCIENCE SURVEY TO DETERMINE HOW THE SUN S MAGNETISM CREATES ITS HOT DYNAMIC ATMOSPHERE AND TO DETERMINE HOW MAGNETIC ENERGY IS STORED AND EXPLOSIVELY RELEASED AND HOW THE RESULTANT DISTURBANCES PROPAGATE THROUGH THE HELIOSPHERE.