Absorption coefficients for the 6190-Å CH4 band between 290 and 100°K with application to Uranus' atmosphere

Scattering and Absorption Cross-sections of Atmospheric Gases in the Ultraviolet-Visible Wavelength Range (307–725 nm)

“…The absorption cross-section, which is the difference between the total extinction and the Rayleigh scattering cross-section, is shown in Figure 8c. At most spectral ranges, our results are in good agreement with the results from previous studies (Giver, 1978;Smith et al, 1990). For example, the difference as compared to the results from Giver (1978) at 542, 576.4, 598, 619, 665.7, and 703.6 nm is 4.0% on average.…”

“…Methane has weak vibrational overtone absorption in the UV-vis wavelength range that is comparable to or greater than its Rayleigh scattering. Previous high-resolution spectroscopy studies have identified smooth and unstructured absorption bands across the UV-visible range (Giver, 1978;Smith et al, 1990). The spectral features are substantially broader than 0.8 nm, thus the absorption by CH4 can be measured by our BBCES.…”

Saturn's vertical and latitudinal cloud structure 1991–2004 from HST imaging in 30 filters☆

“…The temperature dependence was assumed to be a power law in temperature with the room-temperature coefficient at Fink's values and the value at 80 K taken from the indirect estimation of cold-temperature methane absorption coefficients by Karkoschka (1998). Measured coefficients at cold temperatures are only available at some limited wavelength intervals (Smith et al, 1990;Singh and O'Brien, 1995), and they roughly agree with those by Karkoschka (1998). The chosen value for the self-broadened Lorenz half-width was 0.085 cm −1 .…”

Exploring The Saturn System In The Thermal Infrared: The Composite Infrared Spectrometer

“…Previous efforts to determine the hydrogen para fraction in the observable layers of the atmospheres of the giant planets include analyses of measurements of reflected solar radiation in the near-infrared hydrogen lines (Baines and Bergstralh, 1986;Smith and Baines, 1990;Baines et al, 1995) and analyses of emission measurements in the thermal infrared. Retrievals from Voyager IRIS thermal emission spectra mapped the para fraction in the upper troposphere at ∼100-300 mbar.…”