Inverse raytracing based on Monte-Carlo radiative transfer simulations

Details Inverse raytracing based on Monte-Carlo radiative transfer simulations Inverse raytracing based on Monte-Carlo radiative transfer simulations

Nov 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26a...379..690w&link_type=abstract

Astronomy and Astrophysics, v.379, p.690-696 (2001)

Astronomy and Astrophysics

Astrophysics

1

Radiative Transfer, Scattering, Polarization, Circumstellar Matter, Methods: Data Analysis, Methods: Numerical

Scientific paper

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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