Authors: Bibhuti Kumar Jha (SwRI, Boulder), Arpit Kumar Shrivastav (SwRI, Boulder), Ritesh Patel (SwRI, Boulder), Shanwlee Sow Mondal (NASA GSFC, Greenbelt; CUA, DC), Chris Lowder (SwRI, Boulder), Daniel B Seaton (SwRI, Boulder) and Lisa A Upton (SwRI, Boulder)

Magnetic reconnection is a fundamental process responsible for restructuring the solar magnetic field and driving a wide range of dynamic phenomena in the solar atmosphere. It occurs across a wide range of spatial and temporal scales, from equatorial regions to high-latitude polar zones. These polar regions are characterized by complex magnetic topologies capable of releasing stored magnetic energy over timescales ranging from milliseconds to hours. However, observing reconnection across these diverse environments has long been limited by the constraints of single-vantage-point observations. The advent of high-resolution, multipoint observations from the Solar Dynamics Observatory (SDO) and Solar Orbiter (SO) has now enabled detailed investigations of reconnection phenomena across the solar disk and at high latitudes. In this study, we conduct a multi-vantage point analysis of small-scale magnetic reconnection events  occurring at various solar latitudes. By combining high-cadence EUV imaging from SDO/AIA with out of ecliptic perspectives from Solar Orbiter, we examine the morphology, dynamics, and evolution of small-scale reconnection-driven transients. Our preliminary findings reveal the intricate spatial structure and temporal variability of reconnection, with a particular emphasis on the polar magnetic environment. These insights shed light on the role of polar reconnection in global magnetic flux transport and in driving solar wind outflows.