  We report the discovery of a new, non-eclipsing SU UMa-type dwarf nova, HS
2219+1824. Photometry obtained in quiescence (V ~ 17.5) reveals a double-humped
light curve from which we derive an orbital period of ~ 86.2 min. Additional
photometry obtained during a superoutburst reaching V ~ 12.0 clearly shows
superhumps with a period of ~ 89.05 min. The optical spectrum contains
double-peaked Balmer and HeI emission lines from the accretion disc as well as
broad absorption troughs of Hbeta, Hgamma, and Hdelta from the white dwarf
primary star. Modelling of the optical spectrum implies a white dwarf
temperature of 13000 K <~ Twd <~ 17000 K, a distance of 180 pc <~ d <~ 230 pc,
and suggests that the spectral type of the donor star is later than M5.
Phase-resolved spectroscopy obtained during quiescence reveals a narrow Halpha
emission line component which has a radial velocity amplitude and phase
consistent with an origin on the secondary star, possibly on the irradiated
hemisphere facing the white dwarf. This constitutes the first detection of line
emission from the secondary star in a quiescent SU UMa star.
