Accurate and approximate calculations of Raman scattering in the atmosphere of Neptune

Details Accurate and approximate calculations of Raman scattering in the atmosphere of Neptune Accurate and approximate calculations of Raman scattering in the atmosphere of Neptune

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005icar..173..254s&link_type=abstract

Icarus, Volume 173, Issue 1, p. 254-283.

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Neptune, Neptune Atmosphere, Spectrophotometry, Data Reduction Techniques

Scientific paper

Raman scattering by H2 in Neptune's atmosphere has significant effects on its reflectivity for λ<0.5 μm, producing baseline decreases of ˜20% in a clear atmosphere and ˜10% in a hazy atmosphere. However, few accurate Raman calculations are carried out because of their complexity and computational costs. Here we present the first radiation transfer algorithm that includes both polarization and Raman scattering and facilitates computation of spatially resolved spectra. New calculations show that Cochran and Trafton's (1978, Astrophys. J. 219, 756-762) suggestion that light reflected in the deep CH4 bands is mainly Raman scattered is not valid for current estimates of the CH4 vertical distribution, which implies only a 4% Raman contribution. Comparisons with IUE, HST, and groundbased observations confirm that high altitude haze absorption is reducing Neptune's geometric albedo by ˜6% in the 0.22-0.26 μm range and by ˜13% in the 0.35-0.45 μm range. A sample haze model with 0.2 optical depths of 0.2-μm radius particles between 0.1 and 0.8 bars fits reasonably well, but is not a unique solution. We used accurate calculations to evaluate several approximations of Raman scattering. The Karkoschka (1994, Icarus 111, 174-192) method of applying Raman corrections to calculated spectra and removing Raman effects from observed spectra is shown to have limited applicability and to undercorrect the depths of weak CH4 absorption bands. The relatively large Q-branch contribution observed by Karkoschka is shown to be consistent with current estimates of Raman cross-sections. The Wallace (1972, Astrophys. J. 176, 249-257) approximation, produces geometric albedo ˜5% low as originally proposed, but can be made much more accurate by including a scattering contribution from the vibrational transition. The original Pollack et al. (1986, Icarus 65, 442-466) approximation is inaccurate and unstable, but can be greatly improved by several simple modifications. A new approximation based on spectral tuning of the effective molecular single scattering albedo provides low errors for zenith angles below 70° in a clear atmosphere, although intermediate clouds present problems at longer wavelengths.

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