Edited examples/CassiniMulti/README.rst.
@@ -21,7 +21,7 @@ Both planets damp into a "Cassini state."
A damped orbital-rotational system can enter a "Cassini state," in which
a planet's rotational axis, orbital axis, and the local total angular momentum
vector are all coplanar. In this case, we consider Teegarden's Star's planetary
-system, which consists of two planets that are affected by tides from the
+system, which consists of two planets that are both affected by tides from the
host star. Here we assume a mutual inclination of ~10 degrees, and all orbital
and physical parameters are consistent with the observations. We assume that
planet b has no water, but planet c does; this choice means that planet b's
@@ -47,6 +47,8 @@ Evolution of Teegarden's Star b and c into Cassini states. Planet b equilibrates
to an obliquity of about 1 degree, while planet c, which is potentially
habitable, damps to about 9 degrees. Note that planet b's eccentricity
occassionally reaches values larger than 0.23, where the CPL tidal model
-predicts its rotation rate will switch to the 3/2 resonance. The dynamically
-ellipticity, i.e. oblateness, is determining by the rotation rate and assuming
-hydrostatic equilibrium.
+predicts its rotation rate will switch to the 3:2 spin-orbit resonance. The
+dynamical ellipticity, i.e. oblateness, is calculated by assuming hydrostatic
+equilibrium, including the centripetal force. For both planets, the second
+Cassini parameter (bottom right) settles to a value of approximately -1,
+indicating the presence of a Cassini state.
