  The rotation periods of the host stars of extrasolar planets have been
assessed against those of the Mt. Wilson stars, open cluster stars, and
evolutionary stellar models that include rotation. They appear to be normal,
modulo certain inconsistencies in various necessary inputs. Selection of
candidate planet hosts for radial velocity surveys by low rotation or activity
has resulted in a planet host sample skewed towards older stars. Thus,
cross-comparisons must be age dependent. However, self-consistent ages are
difficult to obtain, and activity ages show signs of systematic errors. There
are indications that activity ages ought to be increased for
lower-than-solar-mass stars and decreased for higher-than-solar-mass stars. Age
uncertainties and a scarcity of measured rotation periods for planet host stars
inflate the dispersion in older stars relative to those in open clusters. The
presently available rotational models display inadequacies, most notably in
producing fast-enough early-type stars. The fact that only one planet host
star, $\tau Boo$, strongly suggests tidal spin-up, while of order ten systems
suggest orbital circularization is explicable in terms of the differing
timescales for these two phenomena. The rotational normalcy of the planet host
stars and other considerations suggest that they are not especially different
from other main sequence stars and that circumstellar matter and/or planets are
probably ubiquitous, at least among sufficiently metal-rich solar-type stars.
