Tables of Auxiliary Functions for the Nonconservative Rayleigh Phase Matrix in Semi-Infinite Atmospheres

Abhyankar, K. D.; Fymat, A. L.

doi:10.1086/190234

Cited by 28 publications

(10 citation statements)

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“…9 we compare our measurements with the analytic model results for Rayleigh scattering atmospheres from e.g. Chandrasekhar (1950), Coulson et al (1960) and Abhyankar & Fymat (1971).…”

Section: Introductionmentioning

confidence: 76%

Limb polarization of Uranus and Neptune

Schmid¹,

Joos²,

Tschan

2006

A&A

150

158

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Imaging polarimetry of Uranus and Neptune in the R, i, and z bands are presented. In all observations a radial limb polarization on the order of 1% was detected with a position angle perpendicular to the limb. The polarization is higher in both planets for the shorter wavelength bands. As a first approximation, the polarization seems to be equally strong along the entire limb. This is unlike Jupiter and Saturn, where significant limb polarization is only observed at the poles. We determined flux-weighted averages of the limb polarization and radial limb polarization profiles, and investigated the degradation and cancellation effects in the polarization signal due to the seeing-limited spatial resolution of our observations. Taking this into account we derived corrected values for the limb polarization in Uranus and Neptune. The results are compared with analytic models for Rayleigh scattering atmospheres for the semi-infinite case and finite layers with ground albedo. The comparison shows that the detected polarization is compatible with expectations. This indicates that limb-polarization measurements offer a powerful diagnostic tool for investigating the properties of scattering particles in the upper atmospheres of Uranus and Neptune, in particular if more sophisticated numerical modeling of the limb polarization becomes available. It is also concluded from the overall strength of the limb polarization that the disk-integrated polarization of Uranus and Neptune for large phase angles is high (p > 20%). This is of interest for future polarimetric detections of extra-solar planets with atmospheric properties similar to Uranus and Neptune.

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“…9 we compare our measurements with the analytic model results for Rayleigh scattering atmospheres from e.g. Chandrasekhar (1950), Coulson et al (1960) and Abhyankar & Fymat (1971).…”

Section: Introductionmentioning

confidence: 76%

Limb polarization of Uranus and Neptune

Schmid¹,

Joos²,

Tschan

2006

A&A

150

158

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“…Results for z = oe (H functions) are given by Stibbs and Weir (1959) and Abhyankar and Fymat (1971).…”

Section: Methods Of X and Y Functionsmentioning

confidence: 99%

“…The relevant H functions for Rayleigh scattering are given by Chandrasekhar (1950), Lenoble (1970) and Abhyankar and Fymat (1971); the latter two references include results for o3 < 1. X and Y functions for (5 = 1 are given by Sekera and Kahle (1966); results in terms of the Stokes parameters are given by Coulson et al (1960) for optical thicknesses not exceeding unity.…”

Section: Methods Of X and Y Functionsmentioning

confidence: 99%

Light scattering in planetary atmospheres

1974

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“…A detailed consideration of problems without parameter b 2 is presented in many papers (see, for example, Chandrasekhar 1960;Horak & Chandrasekhar 1961;Lenoble 1970;Abhyankar & Fymat 1971).…”

Section: Introductionmentioning

confidence: 99%

“…Let us multiply equation for H (1) (µ) by the value λzâ(µ 2 )/(z − µ) from the right side of equation and take the integration over µ in the interval (0,1). For brevity, we introduced λ = 3(1−q) 8 .…”

Section: Introductionmentioning

confidence: 99%

Depolarization of multiple scattered light in atmospheres due to anisotropy of small grains and molecules. II. The problems with sources

Силантьев

Alekseeva

Новиков

2015

Astrophys Space Sci

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In the previous paper we considered two classic problems -the diffuse reflection of the light beam from semi-infinite atmosphere, and the Milne problem. For both problems we used the technique of invariance principle. In this paper we consider the solution of the problem when in semi-infinite atmosphere the sources of unpolarized radiation are exist. Here we used the technique of the Green matrices. We consider only continuum radiation.

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Tables of Auxiliary Functions for the Nonconservative Rayleigh Phase Matrix in Semi-Infinite Atmospheres

Cited by 28 publications

References 0 publications

Limb polarization of Uranus and Neptune

Limb polarization of Uranus and Neptune

Light scattering in planetary atmospheres

Depolarization of multiple scattered light in atmospheres due to anisotropy of small grains and molecules. II. The problems with sources

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