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The scattering inside the media can be determined by a phase function using importance sampling. Therefore, the Henyey–Greenstein phase function [6] — a non-isotropic phase function for simulating the scattering of materials like oceans, clouds or skin [4] — can be applied.
His work on the diffusion of the light in galaxies resulted in what is referred to as the Henyey-Greenstein phase function, [2] [3] first proposed in a paper he authored. [4] This scattering model has found use in other scientific disciplines. [5] The crater Henyey on the Moon is named after him, as is the asteroid called 1365 Henyey. [6]
Modeling photon propagation with Monte Carlo methods is a flexible yet rigorous approach to simulate photon transport. In the method, local rules of photon transport are expressed as probability distributions which describe the step size of photon movement between sites of photon-matter interaction and the angles of deflection in a photon's trajectory when a scattering event occurs.
The RTE is a differential equation describing radiance (, ^,).It can be derived via conservation of energy.Briefly, the RTE states that a beam of light loses energy through divergence and extinction (including both absorption and scattering away from the beam) and gains energy from light sources in the medium and scattering directed towards the beam.
The Henyey track is a path taken by pre-main-sequence stars with masses greater than 0.5 solar masses in the Hertzsprung–Russell diagram after the end of the Hayashi track. The astronomer Louis G. Henyey and his colleagues in the 1950s showed that the pre-main-sequence star can remain in radiative equilibrium throughout some period of its ...
The radiative transfer equation is a monochromatic equation to calculate radiance in a single layer of the Earth's atmosphere. To calculate the radiance for a spectral region with a finite width (e.g., to estimate the Earth's energy budget or simulate an instrument response), one has to integrate this over a band of frequencies (or wavelengths).
Year Name Authors References Language Short description 1983 BHCYL Craig F. Bohren and Donald R. Huffman [1]Fortran Mie solution (infinite series) to scattering, absorption and phase function of electromagnetic waves by a homogeneous cylinder.
In astronomy, a phase curve describes the brightness of a reflecting body as a function of its phase angle (the arc subtended by the observer and the Sun as measured at the body). The brightness usually refers the object's absolute magnitude , which, in turn, is its apparent magnitude at a distance of one astronomical unit from the Earth and Sun.