During the inbound trajectory toward Uranus the Planetary Radio Astronomy instrument on board the Voyager 2 spacecraft observed narrowband smooth (n-smooth) emission at frequencies centered near 60 kHz and O mode emission (the ''dayside source'') in a frequency range narrowly confined around 160 kHz. By assuming empirical models of the plasma density for the dayside magnetosphere of Uranus, and by using cold plasma theory together with observational constraints, we have performed ray-tracing calculations to determine the source location of the O mode emission. The ''dayside source'' appears to originate along magnetic field lines with a footprint near the north magnetic pole. Sources of nightside, high-frequency, broadband smooth (b-smooth) emission observed by Voyager after encounter are believed to exist near the conjugate footprint of these same field lines. This would indicate that the particle population supplying the free energy source has energies at least as high as a few keV and the density in the source region satisfies the condition 0.3<fp/fce<1.0 where fp and fce are the electron plasma frequency and gyrofrequency, respectively. ¿ American Geophysical Union 1990