Simulation of polarization maps. 1: Protostellar envelopes

Details Simulation of polarization maps. 1: Protostellar envelopes Simulation of polarization maps. 1: Protostellar envelopes

Apr 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...284..187f&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 284, no. 1, p. 187-209

Astronomy and Astrophysics

Astrophysics

93

Astronomical Maps, Computerized Simulation, Linear Polarization, Protostars, Stellar Envelopes, Stellar Models, Hydrodynamics, Interstellar Matter, Monte Carlo Method, Particle Size Distribution, Radiative Transfer

Scientific paper

We developed a Monte Carlo code for the computation of polarization maps. This code includes multiple scattering and allows the computation for arbitrary dust configurations. In our model, we consider both the radiation of the central energy source and the thermal emission of the circumstellar dust. As one of the first applications of our code, we present polarization maps for 2D hydrodynamical models (for two time steps of evolution: 32010 and 86222 yr) of a 1 solar mass rotating molecular clump which evolved into a protostar surrounded by a disk and envelope. For deriving the polarization patterns, we used two populations of the DL-MRN model - the diffuse Interstellar matter (ISM)-population (radii between 0.005 and 0.25 micrometers) and a population with only larger grains (radii between 0.1 and 1 micrometers). We calculated the polarization maps for 11 wavelength bands between 0.55 micrometers (V) and 1.3 mm. The computed maps agree with the typical features of the observed polarization maps of circumstellar regions around young stellar objects (YSOs). The grains in the optically thin lobes scatter the light only once. Therefore, the radiation from these lobes is strongly polarized and has a centro-symmetric polarization pattern. For the inner regions of the dust disk which are optically thick, the polarization vectors are aligned and parallel to the disk plane. In the optically thin outer disk regions, the pattern is centro-symmetric again. The computed maps give evidence that the particles are larger than assumed in the standard MRN model.

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