  Regions of magnetic field with near-radial, Parker Spiral-like geometry known
as quiescent regions have been observed in Parker Solar Probe data. These
regions have very low $\delta B / \langle |B| \rangle$ compared to
non-quiescent solar wind at the same heliocentric distances. Quiescent regions
are observed to have lower solar wind bulk speeds, lower proton temperatures,
and lower proton density, consistent with properties of the slow solar wind.
Inside of 15 Rs, identified quiescent regions show distinct thermal properties,
having higher proton temperature anisotropies and lower parallel plasma betas
compared to switchback patches observed at the same heliocentric distances.
When placed on $\mathcal{R}$ vs $\beta_{\parallel p}$ plots (where
$\mathcal{R}$ is the proton temperature anisotropy), quiescent region solar
wind is shown to be more stable to proton cyclotron and firehose instabilities
than non-quiescent solar wind at the same heliocentric distances. It is shown
that quiescent regions evolve similarly to the surrounding non-quiescent solar
wind, but quiescent solar wind begins at a different location in the
$\mathcal{R}$ vs $\beta_{\parallel p}$ parameter space, suggesting that these
regions have separate origins than the more turbulent non-quiescent solar wind.
Namely, enhanced temperature anisotropies and enhanced magnetic field strength
may be consistent with magnetic field lines which have undergone less magnetic
field expansion compared to non-quiescent wind at the same heliocentric
distances.
