UNDERSTANDING THE MAGNETIC FIELD OF CORONAL MASS EJECTIONS (CMES) IS ESSENTIAL FOR ACCURATE SPACE WEATHER PREDICTIONS. REPRODUCING AND HOPEFULLY EVENTUALLY PREDICTING THE MAGNETIC PROFILES OF CME FLUX ROPES IS A VERY ACTIVE FOCUS OF THE SPACE WEATHER COMMUNITY. OFTEN IDEALIZED FLUX ROPE STRUCTURES ARE USED TO GENERATE SYNTHETIC MAGNETIC PROFILES WHICH MAY NOT ACCOUNT FOR ASYMMETRIES FREQUENTLY FOUND IN THE IN SITU OBSERVATIONS. THESE ASYMMETRIES CAN RESULT FROM EXPANSION IN THE FLUX ROPE OR AS A RESULT OF OTHER DISTORTIONS AND CAN LEAD TO SIGNIFICANT ENHANCEMENTS IN THE MAGNETIC FIELD STRENGTH BEYOND THE IDEALIZED CASE. UNIFORM EXPANSION WHICH AFFECTS A FLUX ROPE GLOBALLY RESULTS IN A DISTINCT SIGNATURE THAT CAN BE INCORPORATED IN ANALYTIC MODELS. DISTORTION HOWEVER MAY CAUSE CHANGES ON SMALLER SCALES AS DIFFERENT PARTS OF THE FLUX ROPE INTERACT WITH DIFFERENT SOLAR WIND BACKGROUNDS. WE PROPOSE TO LOOK AT ONE POTENTIAL MECHANISM FOR DISTORTIONS IN A CME FLUX ROPE - THE EFFECTS OF CME DEFLECTION AND ROTATION. OUR GOAL IS TO DETERMINE IF LARGE CME DEFLECTIONS AND ROTATIONS CAUSE ASYMMETRIES IN THE IN SITU COUNTERPARTS. AS A CME CHANGES LATITUDE LONGITUDE OR ORIENTATION PORTIONS OF THE CME WILL RAM INTO THE EXTERNAL SOLAR WIND WHILE OTHER PARTS MOVE AWAY ANALOGOUS TO THE COMPRESSION AND RAREFACTION CREATED AS A CME PROPAGATES RADIALLY THROUGH THE SOLAR WIND. THIS CORRELATION IF PRESENT COULD BE USED TO IMPROVE IN SITU PREDICTION MODELS WHEN CORONAL OBSERVATIONS OR MODELING ARE AVAILABLE. TO TEST THIS WE WILL COMBINE OBSERVATIONS AND MODELING BOTH NEAR THE SUN AND AT 1 AU SIMILAR TO THE KAY&GOPALSWAMY (2017) STUDY OF 45 NEAR-EARTH CMES. WE WILL USE WIND OBSERVATIONS TO IDENTIFY CMES WITH BOTH LARGE AND SMALL ASYMMETRIES. FOR EACH CME WE WILL IDENTIFY THE SOLAR ORIGIN AND FIT ITS COUNTERPART IN CORONAGRAPH IMAGES. WE WILL THEN USE THE DEFLECTION AND ROTATION MODEL FORECAT (KAY ET AL. 2015) TO OBTAIN TIGHTER CONSTRAINTS ON THE CORONAL BEHAVIOR. FORECAT CAN THEN BE COUPLED WITH THE MODEL FIDO (KAY ET AL. 2017) TO DETERMINE SYNTHETIC IN SITU PROFILES. FIDO HAS PREVIOUSLY BEEN USED WITH UNIFORM EXPANSION AND MULTIPLE OPTIONS FOR THE FLUX ROPE MAGNETIC FIELD MODEL. WE WILL ALSO CONSIDER THE ELLIPTICAL-CYLINDRICAL FLUX ROPE MODEL (NIEVES-CHINCHILLA ET AL. 2018) WHICH WILL ALLOW US TO EXPLORE THE EFFECTS OF DISTORTION TO THE CME'S CROSS SECTION. WE WILL SEEK CORRELATIONS BETWEEN THE MAGNITUDE OF DEFLECTION AND ROTATION AND THE DEGREE OF ASYMMETRY IN THE IN SITU OBSERVATIONS. SINCE FORECAT INCLUDES EXPANSION WE CAN ISOLATE ITS EFFECT AND DETERMINE IF THE REMAINING ASYMMETRY CAN BE EXPLAINED BY DISTORTIONS. ADDITIONALLY OTHER POTENTIAL MECHANISMS FOR ASYMMETRY SUCH AS A POLOIDAL PLASMA MOTION (ZHAO ET AL. 2017) CAN BE EASILY INCORPORATED GIVEN THEIR ANALYTIC FORM. THIS WORK WILL USE IN SITU DATA FROM WIND ACE AND DSCOVR FOR THE CME MAGNETIC FIELD AND PLASMA PARAMETERS NEAR 1 AU. ADDITIONALLY WE WILL USE REMOTE OBSERVATIONS FROM SDO SOHO AND STEREO TO CONSTRAIN INPUT PARAMETERS FOR THE CORONAL MODELS AND FOR COMPARISON OF THE CORONAL BEHAVIOR WITH THAT RECONSTRUCTED FROM MULTIPLE CORONAGRAPH VIEWPOINTS. AS THE STUDY PROGRESSES WE WILL INCORPORATE ADDITIONAL IN SITU MEASUREMENTS FROM STEREO AS WELL AS MESSENGER AND VEX. THIS WORK IS DIRECTLY RELEVANT TO THE FIRST AND THIRD GOALS OF THE HELIOPHYSICS DECADAL STUDY - "DETERMINE THE ORIGINS OF THE SUN S ACTIVITY AND PREDICT THE VARIATIONS OF THE SPACE ENVIRONMENT" AND "DETERMINE THE INTERACTION OF THE SUN WITH THE SOLAR SYSTEM AND THE INTERSTELLAR MEDIUM." WE WILL CONSIDER THE ORIGINS OF THE CMES NEAR THE SUN AND BE USE MODELS TO BETTER UNDERSTAND HOW THEIR PROPAGATION THROUGH THE SOLAR SYSTEM CAUSES VARIATIONS IN THEIR STRUCTURE WHICH AFFECTS THEIR IMPACT ON THE SPACE ENVIRONMENT.