  The heliosphere is permeated with highly structured solar wind originating
from the sun. One of the primary science objectives of Parker Solar Probe (PSP)
is to determine the structures and dynamics of the plasma and magnetic fields
at the sources of the solar wind. However, establishing the connection between
in situ measurements and structures and dynamics in the solar atmosphere is
challenging: most of the magnetic footpoint mapping techniques have significant
uncertainties in the source localization of a plasma parcel observed in situ,
and the PSP plasma measurements suffer from a limited field of view. Therefore
it lacks a universal tool to self-contextualize the in situ measurements. Here
we develop a novel time series visualization method named Jensen-Shannon
Scalogram. Utilizing this method, by analyzing the magnetic magnitude data from
both PSP and Ulysses, we successfully identify in situ remnants of solar
atmospheric and magnetic structures spanning more than seven orders of
magnitude, from years to seconds, including polar and mid-latitude coronal
holes, as well as structures compatible with super-granulation, ``jetlets'' and
very small scale flaring activity. Furthermore, computer simulations of
Alfv\'enic turbulence support key features of the observed magnetic magnitude
distribution. Building upon these discoveries, the Jensen-Shannon Scalogram
therefore not only enables us to reveal the fractal fine structures in the
solar wind time series from both PSP and decades-old data archive, but will
also serve as a general-purpose data visualization method applicable to all
time series.
