  There are several phenomenological similarities between Soft Gamma Repeaters
and Fast Radio Bursts, including duty factors, time scales and probable
repetition. The sudden release of magnetic energy in a neutron star
magnetosphere, as in popular models of SGR, can meet the energy requirements of
FRB but requires both the presence of magnetospheric plasma in order that
dissipation occur in a transparent region and a mechanism for releasing much of
that energy quickly. FRB sources and SGR are distinguished by long-lived (up to
thousands of years) current-carrying coronal arches remaining from formation of
the young neutron star and their decay ends the phase of SGR/AXP/FRB activity
even though "magnetar" fields may persist. Runaway increase in resistance when
the current density exceeds a threshold releases magnetostatic energy in a
sudden burst and produces high brightness GHz emission of FRB by a coherent
process; SGR are produced when released energy thermalizes as an equilibrium
pair plasma. Failures of some alternative FRB models and the non-detection of
SGR~1806-20 at radio frequencies are discussed in appendices.
