  The role of small-scale coronal eruptive phenomena in the generation and
heating of the solar wind remains an open question. Here, we investigate the
role played by coronal jets in forming the solar wind by testing whether
temporal variations associated with jetting in EUV intensity can be identified
in the outflowing solar wind plasma. This type of comparison is challenging due
to inherent differences between remote-sensing observations of the source and
in situ observations of the outflowing plasma, as well as travel time and
evolution of the solar wind throughout the heliosphere. To overcome these, we
propose a novel algorithm combining signal filtering, two-step solar wind
ballistic backmapping, window shifting, and Empirical Mode Decomposition. We
first validate the method using synthetic data, before applying it to
measurements from the Solar Dynamics Observatory, and Wind spacecraft. The
algorithm enables the direct comparison of remote sensing observations of
eruptive phenomena in the corona to in situ measurements of solar wind
parameters, among other potential uses. After application to these datasets, we
find several time windows where signatures of dynamics found in the corona are
embedded in the solar wind stream, at a time significantly earlier than
expected from simple ballistic backmapping, with the best performing in situ
parameter being the solar wind mass flux.
