Abstract
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 toward the levels that the International Ultraviolet Explorer (IUE) 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 2.5 × 10-12 M☉ yr-1, 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 yr periodicity in Mira B's optical emission.
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