A Polarized Atmospheric Radiative Transfer Model for Calculations of Spectra of the Stokes Parameters of Shortwave Radiation Based on the Line-by-Line and Monte Carlo Methods

Fomin, B. A.; Falaleeva, V. A.

doi:10.3390/atmos3040451

Cited by 13 publications

(6 citation statements)

References 21 publications

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“…LibRadtran was applied with a six‐stream discrete ordinate solver in a spectrally resolved mode, specifically: 0.001 nm steps in the 121–130 nm range, 0.5 nm steps in the 130–175 nm range, 0.001–0.002 nm steps in the 175–205 nm range, 0.5 nm steps in the 205–305 nm range, and 1 nm steps in the 350–700 nm range. Another high‐resolution model is the short‐wave version of the FLBLM model [ Forster et al ., ; Fomin and Falaleeva , ], which is based on the Monte Carlo approach and has a spectral resolution of 0.25 cm −1 (about 0.0004 nm at 125 nm and about 0.003 nm at 350 nm). Both reference models used linear interpolation and the latest recommended cross sections and quantum yields [ Sander et al ., ] for all species except ozone (cross sections are mostly from Molina and Molina [] and quantum yields are from Talukdar et al .…”

Section: Description Of the Data Sets And Modelsmentioning

confidence: 99%

Evaluation of simulated photolysis rates and their response to solar irradiance variability

et al. 2016

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The state of the stratospheric ozone layer and the temperature structure of the atmosphere are largely controlled by the solar spectral irradiance (SSI) through its influence on heating and photolysis rates. This study focuses on the uncertainties in the photolysis rate response to solar irradiance variability related to the choice of SSI data set and to the performance of the photolysis codes used in global chemistry-climate models. To estimate the impact of SSI uncertainties, we compared several photolysis rates calculated with the radiative transfer model libRadtran, using SSI calculated with two models and observed during the Solar Radiation and Climate Experiment (SORCE) satellite mission. The importance of the calculated differences in the photolysis rate response for ozone and temperature changes has been estimated using 1D radiative-convective-photochemical model. We demonstrate that the main photolysis reactions, responsible for the solar signal in the stratosphere, are highly sensitive to the spectral distribution of SSI variations. Accordingly, the ozone changes and related ozone-temperature feedback are shown to depend substantially on the SSI dataset being used, which highlights the necessity of obtaining accurate SSI variations. To evaluate the performance of photolysis codes, we compared the results of eight, widely used, photolysis codes against two reference schemes. We show that, in most cases, absolute values of the photolysis rates and their response to applied SSI changes agree within 30%. However, larger errors may appear in specific atmospheric regions because of differences, for instance, in the treatment of Rayleigh scattering, quantum yields or absorption cross-sections. Key points Uncertainty in the photolysis rates related to SSI variability is characterized. Ozone feedback can constitute up to a half of the stratospheric temperature response. Performed analysis of photolysis codes is useful for CCM results interpretation.

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Section: Description Of the Data Sets And Modelsmentioning

confidence: 99%

Evaluation of simulated photolysis rates and their response to solar irradiance variability

et al. 2016

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“…Our reference Monte-Carlo model was previously successfully exploited for Earth' conditions in UV region by Sukhodolov et al (2016). It is a high-resolution (0.25 cm −1 ) plane-parallel short-wave version of FLBLM model (Forster et al, 2011;Fomin & Falaleeva, 2012). For the present studies it was adopted to the Venus' conditions according to the baseline work (Haus et al, 2015), in which authors preformed line-by-line calculations along with sensitivity analysis to various spectroscopic and atmospheric parameters from 125 nm to 1000 µm.…”

Section: Monte-carlo Reference Modelmentioning

confidence: 99%

Effective parameterization of absorption by gaseous species and unknown UV absorber in 125-400 nm region of Venus atmosphere

Fomin,

Razumovskiy

2021

Preprint

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We present an effective parameterization of molecular absorption of solar radiation in Venus atmosphere. It is addressed to general circulation modeling to accelerate radiative transfer calculations in spectral region 125 -400 nm (25000 -80000 cm −1 ). In F-UV and M-UV regions strong absorption of CO 2 enables to parameterize gaseous absorption with only two effective cross-sections. In N-UV region absorption of SO 2 and unknown UV absorber are parameterized with five effective cross-sections. Also for treatment of Rayleigh scattering and optical properties of Venus' clouds seven effective spectral points are recommended. Parameterizations were validated by the original reference line-by-line Monte-Carlo radiative transfer model. The outcome of the validation shows the discrepancy in fluxes less than 3%. Thus, it takes only sevenfold solution of radiative transfer equations to appropriately describe solar fluxes and heating rates in the whole ultraviolet region.

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“…The polarized light serves as a compass cue [9,10]. In other applications, skylight polarization is a viable option for navigation [11,12] and remote sensing [13,14]. It is commonly used to obtain the attitude and position of carriers [15] and to detect atmospheric composition or optical properties [16,17].…”

Section: Introductionmentioning

confidence: 99%

Clear Night Sky Polarization Patterns Under the Super Blue Blood Moon

Yang

Jian

et al. 2020

Atmosphere

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Investigating celestial polarization patterns in the case of different environments is important for exploring the atmospheric radiative transfer mechanism. Although intensive studies on clear sky, foggy sky, and even total solar eclipse sky have been conducted, the polarization distribution generated by the moonlight has not been well investigated. This study analyzes celestial polarization patterns generated by the Super Blue Blood Moon (SBBM) through several comparative studies. The polarization patterns under the SBBM are collected, analyzed, and compared with both those generated by the ideal single-scattering Rayleigh model and those in the normal sky. From the analysis of the relative variation of the celestial polarization characteristics including the Degree of Polarization (DoP) and Angle of Polarization (AoP), the changes of the extremum, frequency, symmetric line, and neutral points are discussed. As a result, SBBM polarization patterns change at the beginning of the partial eclipse, and the neutral points vary from traditional neutral points. The value of DoP gradually decreases as the obscuration ratio of the Moon increases. The AoP is no longer symmetrical about the celestial meridian. As a conclusion, it is suggested that the variation of the polarized skylight during the SBBM should be considered in atmospheric model calculation for nocturnal biological activity and navigation information computation.

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A Polarized Atmospheric Radiative Transfer Model for Calculations of Spectra of the Stokes Parameters of Shortwave Radiation Based on the Line-by-Line and Monte Carlo Methods

Cited by 13 publications

References 21 publications

Evaluation of simulated photolysis rates and their response to solar irradiance variability

Evaluation of simulated photolysis rates and their response to solar irradiance variability

Effective parameterization of absorption by gaseous species and unknown UV absorber in 125-400 nm region of Venus atmosphere

Clear Night Sky Polarization Patterns Under the Super Blue Blood Moon

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