REFLECTION PROPERTIES OF VENUS AT 3.8 cm
MASSACHUSETTS INST OF TECH LEXINGTON LINCOLN LAB
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During the fall of 1967, radar was employed to study the scattering properties of the planet Venus at 3.8-cm wavelength. An increase in the transmitter power to 300 kW CW and a reduction in the system noise temperature to 60 degrees K provided a considerable improvement in the radar performance. The frequency power spectra of the echoes were determined by digital Fourier analysis of the received signals. The total power in each spectrum was computed to yield the value for the radar cross section of Venus. These average 1.75 percent of the projected area of the disk.