Radiative transfer in spherical shell atmospheres. III. Application to Venus |
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| Authors: | George W Kattawar |
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| Institution: | Department of Physics, Texas A&M University, College Station, Texas 77843, USA |
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| Abstract: | We have introduced a method of partitioning the radiance emerging from a planetary atmosphere in proportion to the average number of scatterings in each atmospheric layer in order to gain a more fundamental understanding of the so-called level of line formation. A realistic model of the Venus atmosphere was used to compute the radiance for a range of phase angles and two planetary colatitudes, namely, 20 and 90°. We computed the core and continuum radiances for the P(16) line of 8689-Å CO2 band and introduced two ways of computing an effective temperature. Both definitions yielded similar results. We found that these effective temperatures varied little with phase angles up to 120°, but fell rather rapidly beyond this point. Also colder effective temperatures were found as we went from equator to pole. The results obtained are all consistent with the spectroscopic temperature determination from CO2 band studies. We have also defined an effective optical depth, τeff, which we feel gives a better understanding of the level of line formation than other definitions used to date. |
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