Modelling of the twilight sky brightness using a numerical solution of the radiation transfer equation

Belikov, Yu. E.

doi:10.1016/0021-9169(95)00175-1

Cited by 10 publications

(4 citation statements)

References 8 publications

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“…We wish to validate our simulations results by comparing our rendered images to calibrated photographs of sunsets during known atmospheric conditions. In this way, we intend to advance previous work on atmospheric aerosol probing based on twilight measurements [Bigg 1956;Shah 1970;Jadhav and Londhe 1992;Belikov 1996]. The light level during twilight ranges between pure photopic (3.4 cd/m 2 ) and scotopic (0.034 cd/m 2 ) vision.…”

Section: Discussionmentioning

confidence: 97%

“…While a lot of computer experiments were conducted in climatology to investigate global radiative transfer, only a handful of publications are concerned with the visual aspects of twilight colors, mainly to remotely probe atmospheric constituents and aerosol density [Bigg 1956;Shah 1970;Jadhav and Londhe 1992;Belikov 1996]. To compute the radiance observed at a single point on the Earth's surface during twilight, numerical simulations have been performed by various authors.…”

Section: Previous Workmentioning

confidence: 99%

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Physically-based simulation of twilight phenomena

2005

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We present a physically-based approach to compute the colors of the sky during the twilight period before sunrise and after sunset. The simulation is based on the theory of light scattering by small particles. A realistic atmosphere model is assumed, consisting of air molecules, aerosols, and water. Air density, aerosols, and relative humidity vary with altitude. In addition, the aerosol component varies in composition and particle-size distribution. This allows us to realistically simulate twilight phenomena for a wide range of different climate conditions. Besides considering multiple Rayleigh and Mie scattering, we take into account wavelength-dependent refraction of direct sunlight as well as the shadow of the Earth. Incorporating several optimizations into the radiative transfer simulation, a photo-realistic hemispherical twilight sky is computed in less than two hours on a conventional PC. The resulting radiometric data is useful, for instance, for high-dynamic range environment mapping, outdoor global illumination calculations, mesopic vision research and optical aerosol load probing.

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Section: Discussionmentioning

confidence: 97%

Section: Previous Workmentioning

confidence: 99%

Physically-based simulation of twilight phenomena

2005

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“…As the angle increases, second-and higher-order scattering become important. [25] Night Sky Brightness…”

Section: As Night Falls: Setting the Stagementioning

confidence: 99%

Night Sky Brightness Measurement, Quality Assessment and Monitoring

Barentine

2022

Preprint

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Ground-based optical astronomy necessarily involves sensing the light of astronomical objects along with the contributions of many natural sources ranging from the Earth's atmosphere to cosmological light. In addition, astronomers have long contended with artificial light pollution that further adds to the 'background' against which astronomical objects are seen. Understanding the brightness of the night sky is therefore fundamental to astronomy. The last comprehensive review of this subject was nearly a half-century ago, and we have learned much about both the natural and artificial night sky since. This Review considers which influences determine the total optical brightness of the night sky; the means by which that brightness is measured; and how night sky quality is assessed and monitored in the long term.

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“…Even the fastest computers do not make analytical modeling of higher-order multiple scattering simple, especially in the spherical-shell atmospheres required for twilight models. As a result, researchers have long used Monte Carlo and other techniques to reproduce multiple scattering during twilight [20][21][22][23][24][25][26][27][28], and many other 3D radiative transfer models can simulate twilight radiance distributions [29][30][31][32][33]. Almost as numerous are papers on twilight spectral radiances measured with photometers and radiometers [34][35][36][37], as well as research on naked-eye color matching [38][39][40] and on colorimeter and photographic measurements of object and sky colors during twilight [41][42][43][44].…”

Section: Introductionmentioning

confidence: 99%

Measuring and modeling twilight’s Belt of Venus

Lee

2015

Appl. Opt.

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The Belt of Venus (or antitwilight arch) is a reddish band often seen above the antisolar horizon during clear civil twilights, and immediately beneath it is the bluish-gray earth's shadow (or dark segment) cast on the atmosphere. Although both skylight phenomena have prompted decades of scientific research, surprisingly few measurements exist of their spectral, colorimetric, and photometric structure. Hyperspectral imaging of several clear twilights supplies these missing radiometric details and reveals some common spectral features of the antisolar sky at twilight: (1) color differences between the dark segment and the sunlit sky above the antitwilight arch are small or nil; (2) antisolar color and luminance extremes usually occur at different elevation angles; and (3) the two twilight phenomena are most vivid for modest aerosol optical depths. A second-order scattering model that includes extinction by aerosols and ozone provides some preliminary radiative transfer explanations of these twilight features' color and brightness.

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Modelling of the twilight sky brightness using a numerical solution of the radiation transfer equation

Cited by 10 publications

References 8 publications

Physically-based simulation of twilight phenomena

Physically-based simulation of twilight phenomena

Night Sky Brightness Measurement, Quality Assessment and Monitoring

Measuring and modeling twilight’s Belt of Venus

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