  Solar wind magnetic fluctuations exhibit anisotropy due to the presence of a
mean magnetic field in the form of the Parker spiral. Close to the Sun, direct
measurements were not available until the recently launched Parker Solar Probe
(PSP) mission. The nature of anisotropy and geometry of the magnetic
fluctuations play a fundamental role in dissipation processes and in the
transport of energetic particles in space. Using PSP data, we present
measurements of geometry and anisotropy of the inner heliosphere magnetic
fluctuations, from fluid to kinetic scales. The results are surprising and
different from 1 au observations. We find that fluctuations evolve
characteristically with size scale. However, unlike 1 au solar wind, at the
outer scale, the fluctuations are dominated by wavevectors quasi-parallel to
the local magnetic field. In the inertial range, average wave vectors become
less field-aligned, but still remain more field aligned than near-Earth solar
wind. In the dissipation range, the wavevectors become almost perpendicular to
the local magnetic field in the dissipation range, to a much higher degree than
those indicated by 1 au observations. We propose that this reduced degree of
anisotropy in the outer scale and inertial range is due to the nature of
large-scale forcing outside the solar corona.
