REFLECTION PROPERTIES OF VENUS AT 3.8 cm

Abstract

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.

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Document Details

Document Type
Technical Report
Publication Date
Sep 06, 1968
Accession Number
AD0681467

Entities

People

  • Gordon H. Pettengill
  • James I. Levine
  • John V. Evans
  • Richard A. Brockelman
  • Richard P. Ingalls

Organizations

  • Massachusetts Institute of Technology

Tags

DTIC Thesaurus Topics

  • Atmospheric Attenuation
  • Atmospheric Refraction
  • Bandwidth
  • Computer Programs
  • Continuous-Wave Radar
  • Data Analysis
  • Data Processing
  • Doppler Effect
  • Frequency Shift
  • General Relativity
  • Geometry
  • Jet Propulsion
  • Measurement
  • Radar
  • Radio Frequency
  • Radio Frequency Power
  • Refraction

Readers

  • Astronomy/Astrophysics
  • Neurological Diseases/Conditions/Disorders
  • Radar Systems Engineering.