  We present RXTE monitoring of the eclipsing X-ray binary Hercules X-1
conducted over the short-high state of July 1998. This was one of the last
major short-high states before the source entered an anomalous low-state of
activity. A comparison with previous epochs finds no evidence for special
behavior during these observations. We determine orbital and pulsar spin
periods to facilitate measurements period derivatives during the subsequent
anomalous low state and during the next epoch of high-state activity.
Spectrally, the decay of the short-high state and concurrent pre-eclipse dips
are consistent with obscuration of a central X-ray source by a cloud of
non-uniform column density. The standard model of a warped accretion disk of
finite vertical scale height fits the characteristics of this absorber well.
Pre-eclipse dips have durations a factor of a few longer than the
characteristic durations of dips during main-high states. Pulse profile
structure increases in complexity towards the tail of the short-high state
suggesting changes in accretion curtain geometry.

Astrophysics