DURING THE PAST DECADE THEORY/MODELING AND OBSERVATIONS FROM NASA MISSIONS SUCH AS STEREO AND ACE HAVE HAD A TRANSFORMATIONAL IMPACT ON OUR UNDERSTANDING OF HOW THE SUN COUPLES TO THE HELIOSPHERE. IT IS NOW WIDELY ACCEPTED THAT TOPOLOGICAL COMPLEXITY AND NON-STEADY DYNAMICS ARE ABSOLUTELY ESSENTIAL FOR UNDERSTANDING THE SUN-HELIOSPHERE CONNECTION. BOTH THE COMPLEXITY AND THE DYNAMICS ARE CLEARLY DUE TO THE ACTIONS OF THE SUN'S POWERFUL MAGNETIC FIELD BUT THE PROCESSES BY WHICH THE FIELD DRIVES THE PLASMA ARE STILL FAR FROM UNDERSTOOD. UNDERSTANDING THESE PROCESSES IS CRITICAL FOR PREDICTING THE VARIATIONS IN THE SPACE ENVIRONMENT AROUND EARTH AND FOR CHARACTERIZING THE INTERACTION OF THE SUN AND THE SOLAR SYSTEM. FURTHERMORE THE SUN-HELIOSPHERE CONNECTION IS THE PRIMARY SCIENCE OBJECTIVE OF NASAS UPCOMING HELIOPHYSICS FLAGSHIP MISSION SOLAR PROBE PLUS (SPP) AND OF THE NASA/ESA FLAGSHIP MISSION SOLAR ORBITER (SO). WE WILL USE THE ADAPTIVELY REFINED MHD SOLVER (ARMS; DEVORE&ANTIOCHOS 2008) WHICH WAS BUILT PRECISELY FOR SIMULATING PHYSICAL SYSTEMS SUCH AS THE OPEN-CLOSED BOUNDARY WHERE CURRENT-SHEET FORMATION AND RECONNECTION DOMINATE. ARMS HAS UNSURPASSED ACCURACY AND CAPABILITY FOR CALCULATING MAGNETIC RECONNECTION IN THE CORONA AND HELIOSPHERE (E.G. DEVORE&ANTIOCHOS 2008; LYNCH ET AL. 2008 2009 2016; WYPER ET AL. 2016) AND HAS BEEN USED TO DERIVE MAJOR THEORETICAL INSIGHTS INTO THE SUN-HELIOSPHERE CONNECTION. THESE INSIGHTS HAVE LED TO A NEW THEORETICAL MODEL THE S-WEB (ANTIOCHOS ET AL. 2007 2011 2012) WHICH PROMISES TO SOLVE ONE OF THE LONGEST STANDING PROBLEMS IN SOLAR AND HELIOSPHERIC PHYSICS IDENTIFYING THE SOLAR SOURCES OF THE SLOW WIND AND HAS MAJOR IMPLICATIONS FOR ALL ASPECTS OF SUN-HELIOSPHERE COUPLING.