Impact of Aerosol Optical Properties, Precipitable Water, and Solar Geometry on Sky Radiances Using Radiative Transfer Modeling

Presented at the 16th International Conference on Meteorology, Climatology and Atmospheric Physics—COMECAP 2023, Athens, Greece, 25–29 September 2023


Introduction
The distribution of diffuse radiance over the sky hemisphere is frequently required in many fields and applications, like predicting the solar irradiance on sloped planes or a titled solar collector [1], or to quantify the spectral angular effects on photovoltaic (PV) devices' performance [2,3].Other solar applications include the prediction of irradiance incident on concentrating collectors [4], the calculation of the geometrical correction factor for a tilted sensor [5], and the evaluation of solar UV exposure of living organisms [6].
Sky radiance or luminance, in the absence of clouds, mainly depends on aerosols' optical properties.Aerosols influence the Earth's radiative budget by attenuating (scattering and absorbing) the incoming solar radiation (direct effect) and by acting as cloud condensation nuclei and changing the microphysical properties of clouds and their lifetime (indirect effect) [7].Understanding the contribution of aerosols to radiative processes is often characterized by uncertainties due to the incomplete knowledge of aerosol microphysical and optical properties.In addition to that, the high spatiotemporal variability of both natural (e.g., volcanic eruption, desert dust, and sea-spray) and anthropogenic aerosols (e.g., biomass burning and engine fuel combustion) makes the problem particularly challenging.The intensity of scattered radiation and its angular distribution depends on the nature of the scatterer and its size in relation to the wavelength of the interacting radiation.The aerosol optical depth (AOD), the volume size distribution, the single-scattering albedo (SSA), the phase function and other aerosol optical properties (AOPs) were retrieved using an inversion algorithm based on measured or estimated sky radiances [8,9].Different instruments exist to measure the sky radiance experimentally, such as sky scanners [10,11], radiometers [12], spectroradiometers [13,14] and, recently, all-sky imagers (ASIs) [14,15].
However, the limited number of stations around the globe that provide quality-assured solar data and the cost of the equipment lead to limited special coverage of sky radiance data.This has resulted in the development of sky radiance models that can be applied universally and provide accurate results under any atmospheric condition.Many empirical and semi-empirical approaches have been proposed for the determination of sky diffuse radiation, accompanied by certain limitations [16][17][18][19].
Radiative transfer modeling constitutes a valuable tool to accurately estimate the sky radiance/luminance [20][21][22][23][24].These models take into account the optical depth of the atmosphere, the multiple extinction and scattering events at the atmosphere.A planeparallel atmosphere is considered when solving the radiative transfer equation.In the present study, a sensitivity analysis of the clear-sky radiances is performed at various atmospheric conditions using the radiative transfer model libRadtran [25,26].

Radiative Transfer Simulations
LibRadtran provides a library for radiative transfer modeling and includes several functions for the calculation of solar and thermal radiation in the Earth's atmosphere.At the core of libRadtran lies the UVSPEC radiative transfer code A radiative transfer model (RTM) calculates how extraterrestrial solar radiation is altered by its path through the atmosphere and the interactions with its constituents (namely, gases, aerosols, clouds).RTMs consider a plane-parallel atmosphere, i.e., a one-dimensional atmosphere bounded at the top and bottom by horizontal plane surfaces.Other assumptions made in the models worth mentioning include the fact that the medium (e.g., atmospheric layer) does not change with time as the photon passes through it, that the frequency of the photon does not change as it interacts with the matter, and that the photons move in straight lines.
To generate the sky's spectral radiance, version 2.0.1 of the libRadtran software package and the UVSPEC radiative transfer model are adopted.Different input values of AOD, the Ångström exponent (AE), single-scattering albedo (SSA), precipitable water (PW) and solar zenith angle (SZA) are selected to examine the effect of aerosol conditions to the sky luminance.We used DISORT (discrete-ordinate-method radiative transfer) method for solving the radiative transfer equation that assumes that the atmosphere consists of a number of adjacent homogenous layers.

Results
The simulated diffuse clear sky radiances are visually demonstrated as contour plots of the relative difference (%) of the radiances from a reference scenario at three solar zenith angles (10 • , 40 • and 70 • ) in three different spectral regions-ultraviolet A (UV-A, 320-400 nm), visible (VIS, 400-750 nm), and near-infrared (NIF, 750-2500 nm)-for the hemisphere above the horizon.Not all cases are presented in the current study.The ones with the most significant effect are selected.
Figure 1 shows the effect of AOD on the distribution of the diffuse sky radiance under cloud-free conditions at the visible spectral range.To explicitly quantify how the AOD affects the radiance simulations, the relative differences of the sky radiances were simulated by assuming no-aerosol and high-aerosol conditions in the atmosphere and calculated using Formula (1), as follows: It is clear that the presence of high aerosol load in the atmosphere results in extremely more scattered lights distributed in the sky with maximum values in the area near the Sun.As the aerosol load increases, the Mie scattering dominates over Rayleigh and the size of the solar disk increases, resulting in the above differences.For high SZA angles, the path of the incident light increases, as well as the interactions between the light beams and the aerosols, leading to more scattered radiation distributed in the sky.The above can be confirmed from the results in Figure 1.In Figure 2, the effect of AE on the distribution of sky radiance is presented.The corresponds to the foremost aerosol size.The relative differences are calculated as for AOD by comparing the cases with fine (AE = 1.9) and coarse (AE = 0.01) aerosol sizes.apparent that the coarse aerosols revealed a positive relative difference at scattering an close to the circumsolar region due to Mie theory.At the edge of the polar plots, the radiances were higher for the fine aerosols.The latter comes to an agreement with aerosol phase function for Mie theory.Figure 3 depicts the effect of SSA on the scattered radiation and its angular distr tion.SSA is defined as the ratio of scattering to total extinction and corresponds to aer absorptivity.Higher SSA values signify that aerosols tend to scatter the solar radiat while lower values reveal aerosols that are more absorbent.The relative differences calculated as for the AOD and AE by comparing the cases with absorbing (SSA = 0.85) non-absorbing (SSA = 0.99) aerosols.Based on Figure 3, for all scattering angles, the r tive differences were positive, ranging from 26 to 56%.More specifically, at the edge the polar plots, the relative differences were higher.In Figure 2, the effect of AE on the distribution of sky radiance is presented.The AE corresponds to the foremost aerosol size.The relative differences are calculated as for the AOD by comparing the cases with fine (AE = 1.9) and coarse (AE = 0.01) aerosol sizes.It is apparent that the coarse aerosols revealed a positive relative difference at scattering angles close to the circumsolar region due to Mie theory.At the edge of the polar plots, the sky radiances were higher for the fine aerosols.The latter comes to an agreement with the aerosol phase function for Mie theory.In Figure 2, the effect of AE on the distribution of sky radiance is presented.The corresponds to the foremost aerosol size.The relative differences are calculated as for AOD by comparing the cases with fine (AE = 1.9) and coarse (AE = 0.01) aerosol sizes.apparent that the coarse aerosols revealed a positive relative difference at scattering an close to the circumsolar region due to Mie theory.At the edge of the polar plots, the radiances were higher for the fine aerosols.The latter comes to an agreement with aerosol phase function for Mie theory.Figure 3 depicts the effect of SSA on the scattered radiation and its angular distr tion.SSA is defined as the ratio of scattering to total extinction and corresponds to aer absorptivity.Higher SSA values signify that aerosols tend to scatter the solar radiat while lower values reveal aerosols that are more absorbent.The relative differences calculated as for the AOD and AE by comparing the cases with absorbing (SSA = 0.85) non-absorbing (SSA = 0.99) aerosols.Based on Figure 3, for all scattering angles, the r tive differences were positive, ranging from 26 to 56%.More specifically, at the edge the polar plots, the relative differences were higher.Figure 3 depicts the effect of SSA on the scattered radiation and its angular distribution.SSA is defined as the ratio of scattering to total extinction and corresponds to aerosol absorptivity.Higher SSA values signify that aerosols tend to scatter the solar radiation, while lower values reveal aerosols that are more absorbent.The relative differences are calculated as for the AOD and AE by comparing the cases with absorbing (SSA = 0.85) and non-absorbing (SSA = 0.99) aerosols.Based on Figure 3, for all scattering angles, the relative differences were positive, ranging from 26 to 56%.More specifically, at the edges of the polar plots, the relative differences were higher.Globally, water vapor absorbs in the visible and near-infrared solar spectrum m than any other atmospheric constituent.Under cloud-free conditions, water vapor abso the majority of the total solar absorption in the atmosphere.The predominance of the ter vapor absorption occurs in near-infrared.With that considered, the effect of the PW the diffuse radiance field in the NIF spectral range is shown in Figure 4.The absorp of PW leads to a decrease in the sky radiance of around 20-40%, with the highest di ences occurring in the horizon.Globally, water vapor absorbs in the visible and near-infrared solar spectrum more than any other atmospheric constituent.Under cloud-free conditions, water vapor absorbs the majority of the total solar absorption in the atmosphere.The predominance of the water vapor absorption occurs in near-infrared.With that considered, the effect of the PW in the diffuse radiance field in the NIF spectral range is shown in Figure 4.The absorption of PW leads to a decrease in the sky radiance of around 20-40%, with the highest differences occurring in the horizon.Globally, water vapor absorbs in the visible and near-infrared solar spectrum m than any other atmospheric constituent.Under cloud-free conditions, water vapor abs the majority of the total solar absorption in the atmosphere.The predominance of the ter vapor absorption occurs in near-infrared.With that considered, the effect of the PW the diffuse radiance field in the NIF spectral range is shown in Figure 4.The absorp of PW leads to a decrease in the sky radiance of around 20-40%, with the highest di ences occurring in the horizon.

Conclusions
In this contribution, numerous radiative transfer simulations were performed to scribe the spectral radiance of clear skies under different aerosol conditions.To cov large range of cases, the clear sky radiance/luminance relative changes were calcula varying AOD, AE, SSA, and PW for different solar geometries in three broadband w lengths.The presented findings highlight the increase in diffuse sky radiance with values of AOD and large SZAs, especially in the circumsolar region.

Figure 1 .
Figure 1.The effect of AOD on diffuse sky radiances in the visible spectral range.The color indicates the relative difference of radiance between high-aerosol and no-aerosol conditions in atmosphere for SZA = 10° (left plot), SZA = 40° (middle plot), and SZA = 70° (right plot).The p diagrams account for all the azimuth and solar angles for a given viewing angle of 0°.

Figure 2 .
Figure 2. The effect of the AE on diffuse sky radiances in the visible spectral range.The colo indicates the relative difference of radiance between fine aerosols (AE = 1.5) and coarse (AE = aerosols for SZA = 10° (left plot), SZA = 40° (middle plot), and SZA = 70° (right plot).The p diagrams account for all the azimuth and solar angles for a given viewing angle of 0°.

Figure 1 .
Figure 1.The effect of AOD on diffuse sky radiances in the visible spectral range.The color bar indicates the relative difference of radiance between high-aerosol and no-aerosol conditions in the atmosphere for SZA = 10 • (left plot), SZA = 40 • (middle plot), and SZA = 70 • (right plot).The polar diagrams account for all the azimuth and solar angles for a given viewing angle of 0 • .

Figure 1 .
Figure 1.The effect of AOD on diffuse sky radiances in the visible spectral range.The color indicates the relative difference of radiance between high-aerosol and no-aerosol conditions in atmosphere for SZA = 10° (left plot), SZA = 40° (middle plot), and SZA = 70° (right plot).The p diagrams account for all the azimuth and solar angles for a given viewing angle of 0°.

Figure 2 .
Figure 2. The effect of the AE on diffuse sky radiances in the visible spectral range.The colo indicates the relative difference of radiance between fine aerosols (AE = 1.5) and coarse (AE = aerosols for SZA = 10° (left plot), SZA = 40° (middle plot), and SZA = 70° (right plot).The p diagrams account for all the azimuth and solar angles for a given viewing angle of 0°.

Figure 2 .
Figure 2. The effect of the AE on diffuse sky radiances in the visible spectral range.The color bar indicates the relative difference of radiance between fine aerosols (AE = 1.5) and coarse (AE = 0.0) aerosols for SZA = 10 • (left plot), SZA = 40 • (middle plot), and SZA = 70 • (right plot).The polar diagrams account for all the azimuth and solar angles for a given viewing angle of 0 • .

Figure 3 .
Figure 3.The effect of the SSA on diffuse sky radiances in the UV-A spectral range.The color indicates the relative difference of radiance between non-absorbing and absorbing SSA value SZA = 10° (left plot), SZA = 40° (middle plot), and SZA = 70° (right plot) for an AOD of 0.5.The p diagrams account for all the azimuth and solar angles for a given viewing angle of 0°.

Figure 4 .
Figure 4.The effect of the PW on diffuse sky radiances in the NIF spectral range.The color indicates the relative difference of radiance between high-PW and no-PW values for SZA = 10° plot), SZA = 40° (middle plot), and SZA = 70° (right plot).The polar diagrams account for al azimuth and solar angles for a given viewing angle of 0°.

Figure 3 .
Figure 3.The effect of the SSA on diffuse sky radiances in the UV-A spectral range.The color bar indicates the relative difference of radiance between non-absorbing and absorbing SSA values for SZA = 10 • (left plot), SZA = 40 • (middle plot), and SZA = 70 • (right plot) for an AOD of 0.5.The polar diagrams account for all the azimuth and solar angles for a given viewing angle of 0 • .

Figure 3 .
Figure 3.The effect of the SSA on diffuse sky radiances in the UV-A spectral range.The colo indicates the relative difference of radiance between non-absorbing and absorbing SSA value SZA = 10° (left plot), SZA = 40° (middle plot), and SZA = 70° (right plot) for an AOD of 0.5.The p diagrams account for all the azimuth and solar angles for a given viewing angle of 0°.

Figure 4 .
Figure 4.The effect of the PW on diffuse sky radiances in the NIF spectral range.The colo indicates the relative difference of radiance between high-PW and no-PW values for SZA = 10° plot), SZA = 40° (middle plot), and SZA = 70° (right plot).The polar diagrams account for al azimuth and solar angles for a given viewing angle of 0°.