4.6 Article

Effect of small-scale snow surface roughness on snow albedo and reflectance

期刊

CRYOSPHERE
卷 15, 期 2, 页码 793-820

出版社

COPERNICUS GESELLSCHAFT MBH
DOI: 10.5194/tc-15-793-2021

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资金

  1. Academy of Finland [315497, 295874, 120949, 260027, 254195, 296302]
  2. EUMETSAT in the projects Satellite Application Facility on Climate Monitoring (CM SAF)
  3. Satellite Application Facility on Support to Operational Hydrology and Water Management (H SAF)
  4. Satellite Application Facility on Land Surface Analysis (LSA)
  5. Academy of Finland (AKA) [254195, 120949, 296302, 315497, 260027, 120949, 315497, 296302, 295874, 254195, 260027, 295874] Funding Source: Academy of Finland (AKA)

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This study presents a snow surface albedo model considering small-scale surface roughness effects, based on photon recollision probability, which can be combined with existing bulk volume albedo models. The research shows that surface roughness has a greater impact on albedo as the melting season progresses, and it increases backward scattering, particularly for larger solar zenith angle values.
The primary goal of this paper is to present a model of snow surface albedo accounting for small-scale surface roughness effects. The model is based on photon recollision probability, and it can be combined with existing bulk volume albedo models, such as Two-streAm Radiative Trans-fEr in Snow (TARTES). The model is fed with in situ measurements of surface roughness from plate profile and laser scanner data, and it is evaluated by comparing the computed albedos with observations. It provides closer results to empirical values than volume-scattering-based albedo simulations alone. The impact of surface roughness on albedo increases with the progress of the melting season and is larger for larger solar zenith angles. In absolute terms, small-scale surface roughness can decrease the total albedo by up to about 0.1. As regards the bidirectional reflectance factor (BRF), it is found that surface roughness increases backward scattering especially for large solar zenith angle values.

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