I would like to consider how tight binaries consisting of a super-massive black hole of mass M = 10^3-10^4 Msun and a white dwarf in quasi-circular orbit can be formed in a globular cluster. I point out that a major fraction of white dwarfs tidally captured by the black hole may be destroyed by tidal inflation and rotational break-up during ongoing tidal circularisation, and therefore the formation of tight binaries is inhibited. However, some fraction may survive tidal circularisation through being spun up to high rotation rates where tidal interactions are less effetive. I estimate the circularisation rate of this fraction and associated probability of finding of a source of GW emission. It is supposed that under certain favourable circumstances LISA could detect several such sources during its mission.