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Our current theoretical and observational understanding suggests thatcritical properties of the solar wind and Coronal Mass Ejections (CMEs) areimparted within 10 Rs, particularly below 4 Rs. This seemingly narrow spatialregion encompasses the transition of coronal plasma processes through theentire range of physical regimes from fluid to kinetic, and from primarilyclosed to open magnetic field structures. From a physics perspective,therefore, it is more appropriate to refer to this region as the CriticalCoronal Transition Region (CCTR) to emphasize its physical, rather thanspatial, importance to key Heliophysics science.  This white paper argues that the comprehensive exploration of the CCTR willanswer two of the most central Heliophysics questions, "How and where does thesolar wind form?" and "How do eruptions form?", by unifyinghardware/software/modeling development and seemingly disparate researchcommunities and frameworks. We describe the outlines of decadal-scale plan toachieve that by 2050.

The Critical Coronal Transition Region: A Physics-framed Strategy to Uncover the Genesis of the Solar Wind and Solar Eruptions