  The problem of detecting Jovian-sized planets orbiting White Dwarf stars is
considered. Significant IR excesses result from warm Jupiters orbiting a White
Dwarf of $T_{\rm eff}=10000$ K at a distance of $\sim 10^3$ White Dwarf radii
(corresponding to $\sim 10^2$ Jupiter radii or a few tenths of an AU) with an
orbital period of $\sim 100$ days. Such a planet will have a 10 micron flux
density at its Wien peak that is comparable to the emission of the White Dwarf
at that wavelength. Although the White Dwarf is much hotter than the planet,
the planet will have peak brightness at the IR, well into the Rayleigh-Jeans
tail of the White Dwarf, plus Jovians are about 10 times larger than White
Dwarfs, so there is a substantial gain in the planet to star brightness
contrast as compared to planets around Main Sequence stars. In the solar
neighborhood, there are 51 White Dwarf stars within 13 pc of the Sun. At 10 pc,
the IR flux density of ``warm'' Jupiters (a few hundred Kelvin) will fall in
the range 10--100 micro-Jansky which should be observable with {\it SIRTF}.
