  String theory in AdS3 with purely NS-NS fluxes and vanishing RR moduli has a
continuum of winding string excitations in radial plane wave states. BTZ black
holes can emit such strings, which then flow out toward the AdS3 boundary as a
stream of massive quanta, and form a black hole analogue of the solar wind. The
winding string sector thus provides a decay channel for the black hole to
evaporate without having either to couple the system to an external reservoir
or to match the AdS3 throat onto an asymptotically flat region. We compute the
emission amplitude of this "holar wind" in the semi-classical approximation,
and consider the associated version of the black hole information paradox.
