As the beam that we are currently able to transmit is rather weak, it would be better to place detectors directly on the spacecraft where the beam is being transmitted from. In this mission it will be possible meaningfully to measure composition, charge and temperature variations caused directly by the beamed microwaves using instruments located on the platform itself. These results are interesting both for the lower layers of the terrestrial atmosphere and for the ambient medium through which the satellite travels. A retarding potential spectrometer will measure the composition of the local medium, measuring mass, charge and temperature composition. This is important for the study of various factors affecting the lifetime of any future solar power satellite. A multi-band electromagnetic spectrometer will measure absorption of the microwaves by the various components of the atmosphere and their re-emission. This will give important information on the temperature variations caused by the beam, as well as pointing up any anomalous acceleration effects that might be caused. While unimportant for low power systems, as beam concentrations increase this could prove important. Finally, series of static charge sensors on the transmitting antenna will enable a cull dynamic charge profile to be built up. As the outer atmosphere has significant ionization, any significant charge differential across the surface may set up electric currents, shorting the transmission circuit and preventing any power beaming at all, This could also cause significant heating problems for the spacecraft. Effects of Beamed Power (Living Organisms) Power leakage at the rectenna site can promote changes in the local climate. The amount of leakage would increase with increasing frequency but affect a smaller area as the rectenna size decreases. This MLS: Microwave Limb Sounder Radiometer sensing atmospheric microwave emissions at frequencies of 63, 183, and 205 GHz Concentrations of CIO, H2O, O3, and atmospheric pressure at various altitudes from 5 to 85 km HALOE: Halogen Occultation Experiment Radiometer sensing atmospheric infrared absorption from occulted sunlight in the spectral range 2.43-10.25 microns Vertical distributions of HC1, HF, CH4, COj, O3, H2O and members of the N family. HRDI: High Resolution Doppler Imager Fabry-Perot interferometer sensing atmospheric emission and absorption in visible and near-infrared spectral ranges Velocity of upper-atmosphere wind field through measurement of Doppler shifts of molecular absorption lines (below 45 km, daytime only) and atomic emission lines (above 60 km, day/night) WINDII: Wind Imaging Interferometer Michelson interferometer sensing atmospheric emissions in visible and near-infrared spectral ranges Velocity of upper-atmosphere wind field through measurement of Doppler shifts of molecular and atomic emission lines above 80 km SUSIM: Solar Ultraviolet Spectral Irradiance Monitor Full-disk solar ultraviolet irradiance spectrometer Spectrum of solar ultraviolet radiation from 120 to 400 run, with resolution of 0.1 nm SOLSTICE: Solar/Stellar Irradiance Comparison Experiment Full-disk solar ultraviolet irradiance spectrometer Spectrum of solar ultraviolet radiation from 115 to 430 nm, with resolution of 0.12 nm PEM: Particle Environment Monitor Electron, proton, and imaging X-ray spectrometer Energy spectrum of electrons (1 eV-5 MeV), protons (1 eV-150 MeV) and X-rays (2-50 keV)
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