The variation of snow albedo with wavelength across the solar spectrum from 0.3 gm in the ultraviolet (UV) to 2.5 gm in the near infrared (IR) was measured at Amundsen-Scott South Pole Station during the Antarctic summers of 1985-1986and 1990 results were obtained at Vostok Station in summer 1990-1991. The albedo has a uniformly high value of 0.96-0.98 across the UV and visible spectrum, nearly independent of snow grain size and solar zenith angle, and this value probably applies throughout the interior of Antarctica. The albedo in the near IR is lower, dropping below 0.15 in the strong absorption bands at 1.5 and 2.0 gm; and it is quite sensitive to grain size and somewhat sensitive to zenith angle. Near-IR albedos were slightly lower at Vostok than at South Pole, but day-to-day variations in the measured grain size due to precipitation, drifting, and metamorphism were found to cause temporal variations in near-IR albedo larger than those due to any systematic geographical change from South Pole to Vostok. The spectrally averaged albedos ranged from 0.80 to 0.85 for both overcast and clear skies, in agreement with measurements by others at South Pole and elsewhere in Antarctica. Using a two-layer radiative transfer model, the albedo can be explained over the full wavelength range. Tests were made to correct for systematic errors in determining spectral albedo. Under clear skies at about 3000-m elevation the diffuse fraction of downward irradiance varied from 0.4 in the near UV to less than 0.01 in the near IR; knowledge of this fraction is required to correct the measured irradiance for the instrument's deviation from a perfect cosine-response. Furthermore, the deviation from cosine response is itself a function of wavelength. Under clear skies a significant error in apparent albedo can result if the instrument's cosine collector is not parallel to the surface; e.g., if the instrument is leveled parallel to the horizon, but the local snow surface is not horizontal. The soot content of the snow upwind of South Pole Station was only 0.3 ng/g. It was somewhat greater at Vostok Station but was still too small to affect the albedo at any wavelength. Bidirectional reflectance at 0.9-gm wavelength, measured from a 23-m tower at the end of summer after the sastrugi (snow dunes) had diminished, showed a pattern remarkably similar to the spectrally averaged pattern obtained from the Nimbus 7 satellite.In those radiation studies, special attention has always been given to measurement of the snow albedo. This is because snow albedo is in general highly variable. It should actually be less variable on the Antarctic plateau than elsewhere, because the snow always remains well below freezing and metamorphism proceeds slowly; but since the Antarctic surface albedo is high, small differences in albedo can mean large differences in absorbed radiation. For Antarctic snow the reported spectrally averaged albedo in summer ranges from about 0.8 to 0.9 [Liljequist, 1956; Hanson, 1960; Hoinkes, 1961; Kuhn et al., 1977; Peterson, 1978; ...

Spectral albedo was measured along a 6 km transect near the Allan Hills in East Antarctica. The transect traversed the sequence from new snow through old snow, firn, and white ice, to blue ice, showing a systematic progression of decreasing albedo at all wavelengths, as well as decreasing specific surface area (SSA) and increasing density. Broadband albedos under clear‐sky range from 0.80 for snow to 0.57 for blue ice, and from 0.87 to 0.65 under cloud. Both air bubbles and cracks scatter sunlight; their contributions to SSA were determined by microcomputed tomography on core samples of the ice. Although albedo is governed primarily by the SSA (and secondarily by the shape) of bubbles or snow grains, albedo also correlates highly with porosity, which, as a proxy variable, would be easier for ice sheet models to predict than bubble sizes. Albedo parameterizations are therefore developed as a function of density for three broad wavelength bands commonly used in general circulation models: visible, near‐infrared, and total solar. Relevance to Snowball Earth events derives from the likelihood that sublimation of equatorward‐flowing sea glaciers during those events progressively exposed the same sequence of surface materials that we measured at Allan Hills, with our short 6 km transect representing a transect across many degrees of latitude on the Snowball ocean. At the equator of Snowball Earth, climate models predict thick ice, or thin ice, or open water, depending largely on their albedo parameterizations; our measured albedos appear to be within the range that favors ice hundreds of meters thick.

A radiative transfer model is developed to illustrate the processes which determine the spectral albedo and transmission of lake ice. The calculated spectral albedo is dominated by specular reflection from the ice surface in the near infrared, whereas multiple scattering by bubbles below the surface dominates the visible albedo. Adding a snow cover to lake ice will normally increase the visible albedo, but may reduce the albedo in some regions of the near infrared if the sun is low, by reducing the specular reflection. In a preliminary test of the model, spectral albedo was measured on the natural ice cover of a frozen lake. The measurements are explained using the radiative transfer model applied to the air bubble size distribution measured in the same ice. The uncertainty in measurement of bubble size distribution leads to uncertainty in the theoretical albedo which is much larger than the error due to approximations used in derivation of the model.

Nine hundred and sixty-eight bird species, covering all orders, were studied in search of distinctive ultraviolet reflections. All species in the following orders were completely surveyed: Struthioniformes, Tinamiformes, Craciformes, Turniciformes, Galbuliformes, Upupiformes, Coliiformes, Apodiformes and Musophagiformes. The coloured plumage regions in particular exhibited high proportions of UV-reflecting feathers. Bird orders with species which are believed to possess VS (violet-sensitive) cone types mostly had their UV maxima between 380 and 399 nm while orders with species which are assumed to have UVS (ultravioletsensitive) cone types contained significantly species which had their UV maxima between 300 and 379 nm. With an emphasis on non-passerine birds the present study provides evidence that birds of many more groups may see UV light than have been studied to date. Ecological aspects related to UV reflection and perception, as well as sexual dimorphism visible only in the UV, are discussed.

Plumage colour has always been a major criterion when describing and distinguishing bird taxa. Today, the use of reflection spectrophotometry is the most commonly used technique to study plumage coloration. A major advantage of this method is the opportunity of observing reflection beyond the human colour vision range-including the UV-waveband. Traditional taxonomic and phylogenetic research is often based on bird skins held in collections in natural history museums worldwide. Different agents for preservation have been used to prevent skins from being damaged by arthropod pests. Sometimes, parts of the plumage have been contaminated with stains from preservation agents. When dried, they are almost invisible to the human eye under normal sunlight conditions and cause no obvious change to feather coloration. However, some preservation agents contain fluorescent components which show up brightly when illuminated with UV-light. Furthermore, undetectable to the human eye, stains from these agents annihilate UV-reflection, preventing accurate data collection based on the UV-reflection of bird feathers. Measuring plumage parts which have been accidentally stained will lead to a relative underestimate of UV-reflection. In studying 20,000 samples, we found fluorescent stains in some 300 bird skins of varying ages in museum collections throughout Europe and the USA. Different preservation agents have been evaluated for their fluorescence properties.