INTERFACE REGION IMAGING SPECTROGRAPH (IRIS) DATA PROVIDES US AN UNPRECEDENTED PERSPECTIVE ON THE STRUCTURE OF THE CHROMOSPHERE. THE NOVELTY OF THIS DATASET PRESENTS RESEARCHERS WITH A PROBLEM OF CONTEXT MUCH OF WHAT WE KNOW ABOUT THE CHROMOSPHERE HAS BEEN DERIVED FROM SPECTRAL LINES THAT ARE ACCESSIBLE TO GROUND-BASED OBSERVATORIES. TO TRULY UNLOCK THE DIAGNOSTIC CAPABILITIES OF IRIS A DIRECT AND COMPREHENSIVE COMPARISON BETWEEN THE MG II DOUBLET AND THESE OPTICAL CHROMOSPHERIC LINES MUST BE UNDERTAKEN. WE PLAN TO CONDUCT A COMPARATIVE STUDY ON THE AFFECTS OF ACOUSTIC SHOCK PROPAGATION IN THE MAGNETIC CHROMOSPHERE USING JOINT OBSERVATIONS WITH IRIS AND THE SWEDISH SOLAR TELESCOPE CRISP IMAGING SPECTROPOLARIMETER (SST/CRISP) THAT INCLUDE COSPATIAL AND SIMULTANEOUS OBSERVATIONS IN H ALPHA CA II 8542A AND MG II H OVER VARIED MAGNETIC STRUCTURE. ACOUSTIC SHOCKS WERE ONE OF THE FIRST SUGGESTED SOLUTIONS TO THE HEATING PROBLEM FOR STELLAR ATMOSPHERES. SHOCKS ARE EASILY IDENTIFIED AS SAWTOOTH PATTERNS (A BLUE SHIFTED TO RED SHIFTED TEMPORAL DIMMING OVER 100 TO 200 SECONDS) IN CHROMOSPHERIC SPECTRAL PROFILES. SHOCKS CLEARLY PLAY A FORMATIVE ROLE IN THE NON MAGNETIC CHROMOSPHERE BUT THERE ARE MANY UNKNOWNS IN OUR UNDERSTANDING OF HOW ACOUSTIC EVENTS ARE INCORPORATED WITH A MYRIAD OF DISSIPATIVE EFFECTS AVAILABLE TO HEAT THE CHROMOSPHERE IN THE PRESENCE OF STRONG MAGNETIC FIELDS INCLUDING RECONNECTION AND MHD TURBULENCE. WE PROPOSE TO MEASURE THE NET THERMODYNAMIC IMPACT OF SHOCKS IN MAGNETIC REGIONS THROUGH THE DERIVATION OF TWO QUANTITIES: THE SHOCK OCCURRENCE RATE AND THE PLASMA CONDITIONS AT THE SHOCK FRONT. THE SHOCK OCCURRENCE RATE AND ITS VARIATION WITH MAGNETIC STRUCTURE (WHICH THEORY SUGGESTS IS SIGNIFICANT) WILL BE EXTRACTED FROM OUR OBSERVATIONAL DATASETS VIA THE PARAMETERIZATION AND AUTOMATED DETECTION OF THE SHOCK-AFFECTED SPECTRAL LINE PROFILES. THE THERMAL PROPERTIES OF THE SHOCK FRONT WILL BE DERIVED THROUGH A COMPARISON OF SYNTHESIZED NON LTE SPECTRAL PROFILES (GENERATED USING THE BIFROST SIMULATION) WITH BOTH THE PLASMA CONDITIONS OF THE MODEL AND OUR OBSERVED SPECTRA. OUR STUDY WILL SIMULTANEOUSLY ADVANCE THE DIAGNOSTIC CAPABILITIES OF THE IRIS DATASET PROVIDE ENERGY CONSTRAINTS ON THIS FUNDAMENTAL PHYSICAL PROCESS AND ALLOW US TO HONE IN ON THE PHYSICAL SHORTCOMINGS IN THE STATE OF THE ART BIFROST SIMULATION.