  We study the contribution to the decay of de Sitter vacua from bounces with
O(3) x O(2) symmetry. These correspond to the thermal production of a vacuum
bubble at the center of a horizon volume with radius r_H and a temperature
defined by the horizon. They are analogues of the flat spacetime bounces,
independent of Euclidean time, that correspond to thermal production of a
critical bubble. If either the strength of gravity or the false vacuum energy
are increased, with all other parameters held fixed, the bounces approach, and
eventually merge with, the Hawking-Moss solution. Increasing the height of the
barrier separating the true and false vacuum, and thus the tension in the
bubble wall, causes the center of the bubble wall to approach, but never reach,
the horizon. This is in contrast with the prediction of the thin-wall
approximation, which inevitably breaks down when the wall is near the horizon.
Our numerical results show that the Euclidean action of our solutions is always
greater than that of the corresponding O(4)-symmetric Coleman-De Luccia bounce.
