  The physical mechanisms that produce the slow solar wind are still highly
debated. Parker Solar Probe's (PSP's) second solar encounter provided a new
opportunity to relate in situ measurements of the nascent slow solar wind with
white-light images of streamer flows. We exploit data taken by the Solar and
Heliospheric Observatory (SOHO), the Solar TErrestrial RElations Observatory
(STEREO) and the Wide Imager on Solar Probe to reveal for the first time a
close link between imaged streamer flows and the high-density plasma measured
by the Solar Wind Electrons Alphas and Protons (SWEAP) experiment. We identify
different types of slow winds measured by PSP that we relate to the
spacecraft's magnetic connectivity (or not) to streamer flows. SWEAP measured
high-density and highly variable plasma when PSP was well connected to
streamers but more tenuous wind with much weaker density variations when it
exited streamer flows. STEREO imaging of the release and propagation of small
transients from the Sun to PSP reveals that the spacecraft was continually
impacted by the southern edge of streamer transients. The impact of specific
density structures is marked by a higher occurrence of magnetic field reversals
measured by the FIELDS magnetometers. Magnetic reversals originating from the
streamers are associated with larger density variations compared with reversals
originating outside streamers. We tentatively interpret these findings in terms
of magnetic reconnection between open magnetic fields and coronal loops with
different properties, providing support for the formation of a subset of the
slow wind by magnetic reconnection.
