Authors: Colby C. Haggerty (University of Hawaii, Manoa), Michael Shay (University of Delaware), Tai Phan (University of California, Bekeley), Paul Cassak

Magnetic reconnection in current sheets is an effective collisionless dissipation mechanism, one which has been argued to be a potential heating mechanism of the solar wind. However, at closest approach to the sun, many of the current sheets observed by Parker Solar Probe do not appear to be undergoing reconnection. This suppression is correlated with the presence of a shear flow, and persists, unexpectedly  for sub-alfvenic speeds. Using kinetic particle-in-cell simulations of magnetic reconnection, we investigate this regime with a range of initial shear flows . For a span of initial conditions we determine the kinetic signatures and underlying physics of the diffusion region, with a focus on conservation laws. Key observational signatures of shear flow reconnection will be highlighted and compared with simulations, with a focus on implications for the solar wind of the inner heliosphere.