are given to the dependence of (illegible text) high speed spectroscopic parameters on the visible light emissions by the blast. The influence of atmospheric absorption and turbulance on the spectrographic information yield by existing stellar spectrographs is presented in a tabulated form. Balloon carried telescope and spectrograph up to an altitude of approximately 150,000 feet is considered. Whereas, a number of practical problems are known to exist in high altitude balloon telescopy, it is clear that an extension of the UV spectra, as well as freedom from atmospheric turbulances, will be achieved by going above, say, 130 - 140,000 feet.
In the past, thermal conductivity of the lunar surface has been calculated by measurements in variation of temperature on the moon's surface during a lunar eclipse, With the nuclear detonation acting aa a strong heat source and with the availability of highly sensitive infrared detectors, it seems possible to calculate thermal conductivity of lunar surface to a high degree of accuracy. The influence of atmospheric absorption and turbulance on these measurements is tabulated for various existing telescopes and infrared receptors.
Section One
Marker Visibility
The problem of sending a vehicle to the moon and of landing an instrument package on the moon raises the question of tracking in flight and accurate location on the surface of the moon, Visual optical approaches to the problem are preferred because of the great sensitivity of the human eye
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