  Gravitational waves (GWs) emission due to magnetic deformation mechanism is
applied for Soft Gamma Repeaters (SGRs) and Anomalous X-Ray Pulsars(AXPs),
described as fast-spinning and magnetized white dwarfs (WDs). The emission is
caused by the asymmetry around the rotation axis of the star generated by its
own intense magnetic field. Thus, for the first time in the literature, it is
estimated the GWs counterpart for SGRs/AXPs described as WD pulsars. We find
that some SGRs/AXPs can be observed by the space detectors BBO and DECIGO. In
particular, 1E 1547.0-5408 and SGR 1806-20 could be detected in 1 year of
observation, whereas SGR 1900+14, CXOU J171405.7-381031, Swift J1834.9-0846 and
SGR 1627-41 could be observed with a 5-year observation time. We also found
that SGRs/AXPs as highly magnetized neutron stars are far below the sensitivity
curves of BBO and DECIGO. This result indicates that a possible detection of
continuous GWs originated from these objects would corroborate the WD pulsar
model.
