  The magnetic, chemically peculiar A-star HR 710 (HD 15144, ADS 1849A, AB Cet)
has a close companion in a nearly circular orbit. Its 3-day period is unusually
short for such stars. The system emits moderately hard x-rays, which likely
come from a white dwarf secondary (ADS 1849Ab). The Sr II spectrum is very
strong, and the resonance lines show similar core-nib structure to the stronger
Ca K line. We place only loose constraints on a model. There are indications of
a lower electron/gas pressure than expected from the star's parallax and
brightness. Strong-line profiles and anomalous excitation/ionization indicate
significant deviations from traditional models, fixed by Teff, log{g}, and
abundances. Weak spectral-line profiles and wavelength shifts probably indicate
abundance patches rather than the presence of a secondary (ADS 1849Ab)
spectrum. Our UVES spectra are from only one epoch. Additional low-noise,
high-resolution spectra are needed. We discuss the spectrum within the context
of abundance stratification.
