PeterDonis said:
I'll defer that until I've had a chance to look at the potential energy math.
Still pondering this overall, but I wanted to go ahead and post results for potential energy in de Sitter spacetime. We use static coordinates since they are the ones adapted to the timelike KVF (i.e., in which all the metric coefficients are independent of the time coordinate). In these coordinates, the metric is
$$
d\tau^2 = \left( 1 - \frac{\Lambda}{3} r^2 \right) dt^2 - \frac{1}{1 - \frac{\Lambda}{3} r^2} dr^2 + r^2 d\Omega^2
$$
where ##\Lambda## is the cosmological constant and ##d\Omega^2## is the standard angular coordinate metric on a 2-sphere (we will be ignoring the angular coordinates here so I don't need to write that part of the metric down in detail).
By a procedure analogous to how the effective potential is derived in Schwarzschild spacetime, we can write the radial equation of motion in the standard form
$$
\frac{1}{2} \left( \frac{dr}{d\tau} \right)^2 = \frac{1}{2} \left( E^2 - 1 \right) + V(r)
$$
where ##E## is the energy per unit mass (a constant of geodesic motion) and the potential ##V(r)## is given by
$$
V(r) = - \frac{\Lambda}{6} r^2
$$
Notice that this potential decreases as ##r## increases and has a maximum at ##r = 0##, so it is a "potential hill" instead of a "potential well"; contrast with Schwarzschild spacetime where the potential increases as ##r## increases, and has a maximum as ##r \rightarrow \infty## (note that the potential here diverges quadratically as ##r \rightarrow \infty##).
We can also derive the proper acceleration of a static worldline at radius ##r##, again by a proceudre analogous to that used in Schwarzschild spacetime; the result is
$$
a = - \frac{\Lambda r}{3 \sqrt{1 - \frac{\Lambda}{3} r^2}}
$$
This acceleration points inward, towards ##r = 0##, and means that objects must be held static (constant ##r## coordinate) by pushing them inward (to keep them from rolling down the potential hill); again, contrast with Schwarzschild spacetime, where static objects must be pushed outward.
To adapt this to the "two masses connected by a rope" scenario, the center of the rope would be at ##r = 0## (where the proper acceleration is zero and the center of the rope remains at this location while free-falling on a geodesic), and the two masses would both be at the same positive ##r##, but in opposite directions (the directions are captured by the angular coordinates, which I have left out in the above).