  We obtained a new spectrum for the radio galaxy Pictor~A in December 1993.
Comparison with previous data obtained in 1983 and 1987 shows that the broad
component of the Balmer lines has increased considerably in strength and
complexity. The Balmer lines now show a boxy, double peaked profile with
FWZI$\sim$24000 \kms. Although the 1993 H\a\ profile is reminiscent of
Arp~102B, accretion disk models face immediate difficulty because (1) the
redshifted peak in the profile is considerably stronger than the blue one, and
(2) the red and blue peaks varied at different epochs. The latter finding
strongly favors a predominance of radial motion. We argue that Pictor~A, and
the rare objects with similar extremely broad emission line profiles, are
better understood if the orientation is such that the gas is predominantly
moving along the line of sight (i.e.\ a geometrical extremum).
