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We investigate the evolution of spatial distribution of solar wind sources by means of an extended time series of data-driven 3D simulations that cover solar 2 activity cycles. We examine the corresponding solar wind acceleration profiles as a function of source latitude and time, and highlight consequences for the interpretation of Parker Solar Probe (PSP) and Solar Orbiter (SolO) in-situ measurements. We relate magnetic connectivity jumps with solar wind plasma signatures, and discuss their occurrence frequency and amplitudes at different epochs of the solar cycle, on and off the ecliptic plane.We also indicate impacts on the rotation profile of the solar corona and on the occurrence of regions of enhanced poloidal and toroidal flow shear that can drive plasma instabilities. Finally, we search for and test geometrical parameters alternative to the standard ones currently used in semi-empirical solar wind forecasting methods.
Pinto et al. (Sat,) studied this question.