  A wide range of exoplanet and exomoon models are characterized by a finite
average rigidity and a viscosity much lower than the typical values for
terrestrials. Such semiliquid bodies may or may not have rigid crusts with
permanent figures. Unlike planets with solid mantles and Earth-like rheology,
semiliquid bodies can be captured into stable pseudosynchronous spin resonance,
where the average rate of rotation is higher than the synchronous 1:1
resonance. Two basic conditions are derived for capture of planets with a
triaxial figure into pseudosynchronous rotation, one related to the
characteristic tidal wave number (the product of the tidal frequency by the
Maxwell time), and the other to the orbital eccentricity. If a semiliquid
object does not satisfy either of the two conditions, it is captured into the
synchronous resonance. For nearly axially symmetric bodies, only the first
condition is in place, and the other is much relaxed, so they should
predominantly be pseudosynchronous. It is also pointed out that the equilibrium
pseudosychronous rotation rate can not reach the widely used asymptotic value
from the constant time lag model but is in reality closer to the synchronous
spin.
