  SGRs/AXPs are considered a subclass of pulsars powered by magnetic energy and
not by rotation, as normal radio pulsars. They are understood as strongly
magnetized neutron star, with large periods of rotation $P\sim(2-12)$ s, and
large spin-down, with typical $\dot{P}\sim(10^{-13}-10^{-10})$ s/s in contrast
to $\dot{P}\sim10^{-15}$ s for ordinary pulsars. Their persistent X-ray
luminosity, as well as the bursts and flares typical of these sources, are
instead believed to be powered by the decay of their ultrastrong magnetic
field. SGRs/AXPs typically have a larger X-ray luminosity that can not be
explained by their spin-down luminosity ($L_X>\dot{E}_{\rm rot}$), unlike
rotation-powered pulsars. However, the recent discovery of radio-pulsed
emission in four of this class of sources, where the spin-down rotational
energy lost $\dot{E}_{\rm rot}$ is larger than the X-ray luminosity $L_X$
during the quiescent state - as in normal pulsars - opens the question of the
nature of these radio sources in comparison to the others of this class. In
this contribution, we show that the radio SGRs/AXPs obey a linear log-log
relation between $L_X$ and $\dot{E}_{\rm rot}$, very similar to the one
satisfied by X-ray and gamma-ray neutron star pulsars, suggesting their neutron
star nature. Furthermore, we show that almost all the high-B pulsars are also
near the line found for the radio AXPs. In contrast, for almost all the others
SGRs/AXPs, $\log L_X$ does not vary too much as function of $\log \dot{E}_{\rm
rot}$, a phenomenology not shared by X-ray neutron star pulsars, suggesting a
different nature for these sources.
