  In a previous work we analysed the white-light coronal brightness as a
function of elongation and time from Wide-Field Imager (WISPR) observations on
board the Parker Solar Probe (PSP) mission when PSP reached a minimum
heliocentric distance of ~ 28 Rs. We found 4-5 transient outflows per day over
a narrow wedge in the PSP orbital plane, which is close to the solar equatorial
plane. However, the elongation versus time map (J-map) analysis supplied only
lower limits on the number of released density structures due to the small
spatial-scales of the transient outflows and line-of-sight integration effects.
In this work we place constraints on the properties of slow solar wind
transient mass release from the entire solar equatorial plane. We simulated the
release and propagation of transient density structures in the solar equatorial
plane for four scenarios: (1) periodic release in time and longitude with
random speeds; (2) corotating release in longitude, periodic release in time
with random speeds; (3) random release in longitude, periodic release in time
and speed; and (4) random release in longitude, time, and speed. The
simulations were used in the construction of synthetic J-maps, which are
similar to the observed J-map. The four considered scenarios have similar
ranges (35-45 for the minimum values and 96-127 for the maximum values) of
released density structures per day from the solar equatorial plane and
consequently from the streamer belt, given its proximity to the solar
equatorial plane during the WISPR observation. Our results also predict that
density structures with sizes in the range 2-8 Rs, covering 1-20 % of the
perihelion could have been detectable by PSP in situ observations during that
interval.
