Publisher's Synopsis
Excerpt from Further Tests of Stellar Radiometers and Some Measurements of Planetary Radiation
The purpose of the present paper is to describe improvement in the radiometric apparatus used and the results (of interest to physicists) of some preliminary measurements of planetary radia tion as well as a verification of the measurements obtained a year ago in determining stellar temperatures by means of spectral transmission screens.
In this connection it is relevant to point out that the results obtained in mapping the spectral energy distribution of a' star by means of a spectrobolometer may not be essentially different from those obtained by the use of transmission screens. For, as may be seen from inspection of photographs of stellar spectra, the spectrum of a star consists of a bright continuous background superposed upon a series of absorption (and in some cases bright emission) lines. Hence, unless a very large dispersion can be used, the spectrobolometer will merely bridge over wide regions of the spectrum containing bright and dark bands. The spectral transmission screen does practically the same thing, in the sense that it integrates the energy present in a certain spectral region (without indicating the amount lost in the spectral absorption lines) and has the advantage of utilizing perhaps 40 per cent of the total intensity of the incident radiations, which is lost by employing a spectroscope.
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