  Over the last decade, observational evidence has mounted that SGRs/AXPs
belong to a particular class of pulsars. Furthermore, fast and very magnetic
white dwarfs have been observed, and recently two SGRs with low magnetic fields
$B\sim(10^{12}-10^{13})$ G, namely SGR 0418+5729 and Swift J1822.3-1606 were
discovered with a period of $P\sim9.08$ s and $P\sim8.44$ s, respectively.
These new discoveries opens the question of the nature of SGRs/AXPs, emerging
alternative scenarios, in particular the white dwarf (WD) pulsar model. These
astronomical observations have based an alternative description of the
SGRs/AXPs expressed on rotating highly magnetized and very massive WDs. In this
new description, several observational properties are easy understood and well
explained as a consequence of the large radius of a massive white dwarf that
manifests a new scale of mass density, moment of inertia, rotational energy,
and magnetic dipole moment in comparison with the case of neutron stars. In
this contribution, we will show that these recent discoveries of SGRs with low
magnetic field share some properties with the recent detected fast WD pulsar AE
Aquarii, and also with RXJ 0648.0-4418, and EUVE J0317-855, supporting the
understanding of at least these SGRs with low-B as belonging to a class of very
fast and magnetic massive WDs. Furthermore, these recent astronomical
observations suggest that we should revisit the real nature of AXP/SGRs: are
they really magnetars or very fast and massive white dwarfs?
