  Many asymptotic giant branch (AGB) and supergiant stars exhibit extended
detached shells in the far-infrared, resembling rings or arcs. These structures
have long been interpreted as the bow shock formed in the interface between the
stellar wind and the interstellar medium, the astrosphere. To date, only a few
AGB stars have been observed showing an extended shell in the ultraviolet: the
cometary tail drifting away from $o$ Ceti, and a bubble around IRC+10216, CIT6,
and U Hya. This paper describes a search of UV extended shells around AGB stars
using archival GALEX far-UV images. After inspecting visually 282 GALEX images,
we identified the fourth discovery of a UV bubble around the AGB star R Dor.
The bubble is seen as a 26'x29' ring, corresponding to an actual diameter of
0.41x0.46 parsec$^2$. The mass of the thin UV bubble is estimated to be
$\simeq$0.003 $M_{\odot}$. The morphological asymmetry (less than $\sim 20$\%)
and brightness variations of this shell are uncorrelated with the stellar
proper motion and thus they can rather be ascribed to inhomogeneities in the
ISM. Archival \emph{IRAS} 60 and 100$\mu$m images reveal that the bubble is
filled with cold (i.e. < 32 K) dust. All UV bubbles known to date are limited
to be within a distance < 350 pc and at high Galactic latitudes (|b| > 35
degree), which suggests that their detection is hampered in most cases by the
strong UV interstellar extinction.
