Why does the solar wind switch to flowing straight by the time it reaches Earth? Between 02:01 and 02:29 the new NASA Goddard video 5 New Discoveries from NASA's Parker Solar Probe explains

finding # 4, A Breaking Point:
Before parker, scientists knew that the corona rotates with the visible surface below it. But they didn’t know how — or where — the solar wind switched to flowing straight by the time it reaches Earth.
Parker has finally spotted signs of this transition — and the changeover happens significantly farther out than expected.

Naively I'd apply conservation of angular momentum and assume that the particles are in individual ballistic orbits, but the solar wind contains charged particles as well as neutrals and so even though of low density and long mean free paths they can interact collectively.
But I don't understand why the solar wind would suddenly stop rotating beyond some radius from the Sun well inside Earth's orbit, rather than beyond the heliopause.
Why does this happen?
When plasma moves in a magnetic field then the charged particles follow helical paths around the field lines, due to the $q\vec{v}\times \vec{B}$ Lorentz force. If the radius of gyration is small, then the plasma is effectively tied (or frozen) to the field lines.

However to decide whether it is the motion of the magnetic field that enforces motion of the plasma or vice versa, we must compare the magnetic pressure with the gas pressure (or equivalently, compare the magnetic and kinetic energy densities).

The magnetic energy density scales with magnetic field squared and the field drops further from the Sun (e.g. a dipole field falls as $r^{-3}$), whereas the plasma kinetic energy density (which depends on the plasma density and temperature) could remain relatively high (the solar wind density drops only as $r^{-2}$ and the temperature is roughly constant).  There is a transition between the magnetic field dominating the plasma close to the Sun, to where the plasma dominates and effectively carries the field with it. This transition point is known as the Alfven radius and is usually at a few tenths of an au from the Sun.

Below this radius, the plasma (sort-of) co-rotates with the field, which is anchored to the photosphere. Beyond that the plasma is (sort-of) free to move radially outwards. This how the Sun loses angular momentum.