  Recent ultraviolet spectra from the Hubble Space Telescope (HST) and Far
Ultraviolet Spectroscopic Explorer (FUSE) satellites demonstrate that UV line
and continuum fluxes observed from Mira B are increasing back towards the
levels that the International Ultraviolet Explorer observed in 1979-1980 and
1990-1995, after having been found in a very low state by HST and FUSE in
1999-2001. The UV emission is associated with accretion of material onto Mira B
from Mira A's massive wind, so the variability is presumably due to variations
in accretion rate. From wind absorption features, we estimate a Mira B mass
loss rate of 2.5e-12 M_sun/yr, indicating that Mira B's wind has increased in
strength along with the accretion rate. The UV variability may be associated
with a previously reported 14-year periodicity in Mira B's optical emission.
