  IGR J16493-4348 is an eclipsing supergiant high-mass X-ray binary (sgHMXB),
where accretion onto the compact object occurs via the radially outflowing
stellar wind of its early B-type companion. We present an analysis of the
system's X-ray variability and periodic modulation using pointed observations
(2.5-25 keV) and Galactic bulge scans (2-10 keV) from the Rossi X-ray Timing
Explorer (RXTE) Proportional Counter Array (PCA), along with Swift Burst Alert
Telescope (BAT) 70-month snapshot (14-195 keV) and transient monitor (15-50
keV) observations. The orbital eclipse profiles in the PCA bulge scans and BAT
light curves are modeled using asymmetric and symmetric step and ramp
functions. We obtain an improved orbital period measurement of 6.7828 $\pm$
0.0004 days from an observed minus calculated (O-C) analysis of mid-eclipse
times derived from the BAT transient monitor and PCA scan data. No evidence is
found for the presence of a strong photoionization or accretion wake. We refine
the superorbital period to 20.067 $\pm$ 0.009 days from the discrete Fourier
transform (DFT) of the BAT transient monitor light curve. A pulse period of
1093.1036 $\pm$ 0.0004 s is measured from a pulsar timing analysis using
pointed PCA observations spanning $\sim$1.4 binary orbits. We present pulse
times of arrival (ToAs), circular and eccentric timing models, and calculations
of the system's Keplerian binary orbital parameters. We derive an X-ray mass
function of $f_{x}(M)$ $=$ 13.2$^{+2.4}_{-2.5}$ $M_{\odot}$ and find a spectral
type of B0.5 Ia for the supergiant companion through constraints on the mass
and radius of the donor. Measurements of the eclipse half-angle and additional
parameters describing the system geometry are provided.
