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We report the detection of an HI counterpart to the extended,far-ultraviolet-emitting tail associated with the asymptotic giant branch starMira (o Ceti). Using the Nancay Radio Telescope (NRT), we have detectedemission as far as 88' north of the star, confirming that the tail contains asignificant atomic component (M_HI ~ 4x10e-3 M_sun). The NRT spectra reveal adeceleration of the tail gas caused by interaction with the local interstellarmedium. We estimate an age for the tail of ~1.2x10e5 years, suggesting that themass-loss history of Mira has been more prolonged than previous observationalestimates. Using the Very Large Array (VLA) we have also imaged the HI tail outto ~12' (0.4 pc) from the star. The detected emission shows a ``head-tail''morphology, but with complex substructure. Regions with detected HI emissioncorrelate with far-ultraviolet-luminous regions on large scales, but the twotracers are not closely correlated on smaller scales (<1'). We propose thatdetectable tails of HI are likely to be a common feature of red giantsundergoing mass-loss.

Discovery of an HI Counterpart to the Extended Tail of Mira