How the solar wind is structured and propagates through the heliosphere is a consequence of a number of changes in the solar activity. These changes include long-term variations in the active regions, coronal holes and irradiance, as well as more dynamic events such as flux emergence, flares and coronal mass ejections. Nowadays, a large range of analysis techniques has been developed improving the ability to track the solar wind transients from the solar surface upward using remote sensing observations (such as STEREO and SDO) and in-situ measurements (e.g. Wind, ACE and Ulysses). However, we still need to learn more about the underlying mechanism generating and structuring the solar wind, as well as its propagation into the interplanetary space with subsequent interactions with planets or other solar system bodies. This session aims at reviewing the different efforts to understand better how solar structures are feeding the solar wind and how the solar wind evolves upward to 1 AU and beyond. We invite contributions exploiting multiple instruments, especially emphasising the link between in-situ and remote sensing measurements or with quantitative comparisons with numerical models.