  4U 1543-624 is a relatively bright persistent low-mass X-ray binary. Analysis
of archival data from ASCA, SAX and RXTE is presented. The X-ray continuum be
can modeled with the standard low-mass X-ray binary spectrum, an isothermal
blackbody and a Comptonized component. Variations in the luminosity and flux
ratio of the continuum components are seen. An increase in luminosity is
accompanied by a decrease in the blackbody luminosity and a hardening of the
spectrum. Most low-mass X-ray binaries have softer spectra and higher blackbody
luminosities in high luminosity states. The Fe K-alpha line is seen only in the
high luminosity spectra. A narrow feature near 0.7 keV, previously detected in
the ASCA data, is also seen in the SAX data. A qualitative model of the system
is presented. The X-ray observations can be explained by a low inclination
system (face-on disk) containing a slowly (P >> ms) rotating neutron star. A
slowly rotating neutron star would imply either that the system is a young
low-mass X-ray binary, or that the accretion rate is unusually low. The
empirical relation between optical and X-ray luminosity and orbital period
suggests a relatively short period.
