  We present a statistical analysis for the characteristics and radial
evolution of linear magnetic holes (LMHs) in the solar wind from 0.166 to 0.82
AU using Parker Solar Probe observations of the first two orbits. It is found
that the LMHs mainly have a duration less than 25 s and the depth is in the
range from 0.25 to 0.7. The durations slightly increase and the depths become
slightly deeper with the increasing heliocentric distance. Both the plasma
temperature and the density for about 50% of all events inside the holes are
higher than the ones surrounding the holes. The average occurrence rate is 8.7
events/day, much higher than that of the previous observations. The occurrence
rate of the LMHs has no clear variation with the heliocentric distance (only a
slight decreasing trend with the increasing heliocentric distance), and has
several enhancements around ~0.525 AU and ~0.775 AU, implying that there may be
new locally generated LMHs. All events are segmented into three parts (i.e.,
0.27, 0.49 and 0.71 AU) to investigate the geometry evolution of the linear
magnetic holes. The results show that the geometry of LMHs are prolonged both
across and along the magnetic field direction from the Sun to the Earth, while
the scales across the field extend a little faster than along the field. The
present study could help us to understand the evolution and formation mechanism
of the LMHs in the solar wind.
