Stokes vectors, Mueller matrices, and polarized scattered light

Bickel, William S.; Bailey, Wilbur M.

doi:10.1119/1.14202

Cited by 313 publications

(143 citation statements)

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“…whereŜ is the Müller matrix which is used to describe the modification of the photon's Stokes vector due to the interaction of a photon with the scattering/absorbing medium (dust grains; see Bickel & Bailey 1985, Bohren & Huffman 1983. For the albedo A follows:…”

Section: A Weighted Mean Optical Parameters Of Dust Grain Mixturesmentioning

confidence: 99%

MC3D–3D continuum radiative transfer, Version 2

Wolf

2003

Computer Physics Communications

104

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A revised and greatly improved version of the 3D continuum radiative transfer code MC3D is presented. It is based on the Monte-Carlo method and solves the radiative transfer problem self-consistently. It is designed for the simulation of dust temperatures in arbitrary geometric configurations and the resulting observables: spectral energy distributions, wavelength-dependent images, and polarization maps. The main objective is the investigation of "dust-dominated" astrophysical systems such as young stellar objects surrounded by an optically thick circumstellar disk and an optically thin(ner) envelope, debris disks around more evolved stars, asymptotic giant branch stars, the dust component of the interstellar medium, and active galactic nuclei. PACS: 95.30.Jx -Radiative transfer

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Section: A Weighted Mean Optical Parameters Of Dust Grain Mixturesmentioning

confidence: 99%

MC3D–3D continuum radiative transfer, Version 2

Wolf

2003

Computer Physics Communications

104

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“…I is the total detected light intensity which corresponds to addition of the two orthogonal component intensities, Q is the difference in intensity between horizontal and vertical polarization states, U is the portion of the intensity that corresponds to the difference between intensities of linear +45 • and −45 • polarization states, and V is the difference between intensities of right circular and left circular polarization states. In Stokes formalism, the following polarization parameters of any light beam are defined [3,[25][26][27]:…”

Section: Stokes-mueller Formalismmentioning

confidence: 99%

“…Mathematically, the propagation of the transverse EM wave (light) in free space can be represented by the transverse components of the associated electric fields as [3,[23][24][25]:…”

Section: Polarized Light Preliminaries and The Basic Polarization Parmentioning

confidence: 99%

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Turbid medium polarimetry in biomedical imaging and diagnosis

Ghosh

Banerjee

Soni

2011

Eur. Phys. J. Appl. Phys.

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Abstract. Studies on polarization properties of scattered light from a random medium like biological tissue have received considerable attention because polarization can be used as an effective tool to discriminate against multiply scattered light (acting as a gating mechanism) and thus can facilitate high resolution imaging through tissue. Further, the polarization properties of scattered light from tissue contain wealth of morphological and functional information of potential biomedical importance. However, in a complex random medium like tissue, numerous complexities due to multiple scattering and simultaneous occurrences of many scattering and polarization events present formidable challenges both in terms of accurate measurements and in terms of analysis of the tissue polarimetry signal. Several studies have therefore been conducted in the recent past to develop appropriate measurement procedures, suitable light propagation models and polarimetry signal analysis methods to overcome these difficulties. In this review, we focus on some of the recent key developments in this area. Specifically, we describe variety of theoretical and experimental tools, illustrated with selected results, aimed at evaluating the prospect of turbid medium polarimetry for both biomedical imaging and diagnosis.

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“…The modification of the Stokes vector due to the ith interaction can be described with the help of a special 4×4 Mueller matrixŜ(θ), where θ is the scattering angle (see also Bickel & Bailey 1985;Bohren & Huffman 1983).…”

Section: Scattering and Absorptionmentioning

confidence: 99%

Inverse raytracing based on Monte-Carlo radiative transfer simulations

Wolf

2001

A&A

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Abstract.A method for the detailed investigation of polarization maps and images obtained from high-resolution observations is described in this paper. It has been developed for the analysis of the environment of young stellar objects (YSO), ultra-compact HII regions (UCHII), and the optically thin light scattering region of active galactic nuclei (AGN). The method is based on a 3D Monte-Carlo radiative transfer (RT) code. The main principle of this method lies in the detailed investigation of the paths of test-photons in the considered medium. To demonstrate the efficiency and limit of this method, it is applied to a simple YSO configuration consisting of the central star, an optically thick disk, and an optically thin envelope.

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Stokes vectors, Mueller matrices, and polarized scattered light

Cited by 313 publications

References 0 publications

MC3D–3D continuum radiative transfer, Version 2

MC3D–3D continuum radiative transfer, Version 2

Turbid medium polarimetry in biomedical imaging and diagnosis

Inverse raytracing based on Monte-Carlo radiative transfer simulations

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