  The white dwarf stars WD1614+136 and WD1353+409 are not sufficiently massive
to have formed through single star evolution. However, observations to date
have not yet found any evidence for binarity. It has therefore been suggested
that these stars are the result of a merger. In this paper we place an upper
limit of approximately 50kms on the projected rotational velocities of both
stars. This suggests that, if these stars are the results of a merger,
efficient angular momentum loss with accompanying mass loss must have occurred.
If the same process occurs following the merging of more massive white dwarf
stars, the predicted rate of Type Ia supernovae due to merging white dwarfs may
have been greatly over-estimated. Further observations to determine binarity in
WD1614+136 and WD1353+409 are therefore encouraged.
