<i>Light Scattering in Planetary Atmospheres</i>

Соболев, В. В.; Chamberlain, Joseph W.

doi:10.1063/1.3023617

Cited by 83 publications

(153 citation statements)

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“…The reflection effect calculations were based on Sobolev (1975) and Charbonneau et al (1999). We assumed that the transiting planet was small compared to its host star, and so did not take fully into account the gradient in the stellar brightening with radius when calculating the stellar brightness blocked by the planet during transit.…”

Section: The Modelmentioning

confidence: 99%

An investigation into exoplanet transits and uncertainties

Ji¹,

Banks

Budding

et al. 2017

Astrophys Space Sci

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Section: The Modelmentioning

confidence: 99%

An investigation into exoplanet transits and uncertainties

Ji¹,

Banks

Budding

et al. 2017

Astrophys Space Sci

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“…The optical depth is the integral of the extinction coefficient, α ν , along the line of sight from the surface (r surf ) to infinity (Sobolev 1975).…”

Section: Integration Over Altitude Wavelength and Emission Anglementioning

confidence: 99%

Upper Limits on Gaseous CO at Pluto and Triton from High-Resolution Near-IR Spectroscopy

Young

Cook

Yelle

et al. 2001

Icarus

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“…Our physical parametrization for light scattering in a dusty atmosphere follows that of Sobolev (1975). It is assumed that light scattering can be parametrized in terms of extinction, a, single scatter albedo, h, and phase function, P. Extinction, a, describes the fraction of photons which interact with the host medium per unit path length; it is related to host medium number density, n, total cross section (for scattering and absorption), tr, the host medium mass density, p, and mass per host medium particle, m, by the relations a = no, = ptr/m.…”

Section: Physical Assumptions For Model Coma and Mathematical Formulamentioning

confidence: 99%

Multiple scattering of light in a spherical cometary atmosphere with an axisymmetric dust jet

Chick¹,

Gombosi²

1992

Icarus

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We have developed a numerical solution for the anisotropic multiple scattering of light in a cometary atmosphere. The atmosphere is assumed to be a spherical shell illuminated by parallel solar rays. The spatial variation of dust in the coma is symmetric about the Sun-comet axis. Multiple scattering of photons is determined by lambda iteration.We study two model dust profiles: (1) a spherically symmetric profile and (2) an axisymmetric dust jet at the comet's subsolar point. Calculation is made of the flux of visible energy impinging on the nucleus surface, the mean intensity of visible light throughout the coma, and an approximate solution for the flux of thermal radiation at the comet surface due to emission from dust particles in the coma. We determine conditions under which single and multiple scattering each become significant. Under all conditions examined, at no point on the nucleus surface does the radiant flux exceed the visible flux at the subsolar point of a bare nucleus. ~ t992 Academic Pres~, Inc.

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Light Scattering in Planetary Atmospheres

Cited by 83 publications

References 0 publications

An investigation into exoplanet transits and uncertainties

An investigation into exoplanet transits and uncertainties

Upper Limits on Gaseous CO at Pluto and Triton from High-Resolution Near-IR Spectroscopy

Multiple scattering of light in a spherical cometary atmosphere with an axisymmetric dust jet

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