Radiative transfer models of non-spherical prestellar cores

We present 2D Monte Carlo radiative transfer simulations of prestellar cores. We consider two types of asymmetry: disk-like asymmetry, in which the core is denser towards the equatorial plane than towards the poles; and axial asymmetry, in which the core is denser towards the south pole than the nor...

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Main Authors: Stamatellos, D., Whitworth, A. P., Andre, P., Ward-Thompson, D.
Format: Text
Language:unknown
Published: arXiv 2004
Subjects:
Online Access:https://dx.doi.org/10.48550/arxiv.astro-ph/0404443
https://arxiv.org/abs/astro-ph/0404443
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spelling ftdatacite:10.48550/arxiv.astro-ph/0404443 2023-05-15T18:23:06+02:00 Radiative transfer models of non-spherical prestellar cores Stamatellos, D. Whitworth, A. P. Andre, P. Ward-Thompson, D. 2004 https://dx.doi.org/10.48550/arxiv.astro-ph/0404443 https://arxiv.org/abs/astro-ph/0404443 unknown arXiv https://dx.doi.org/10.1051/0004-6361:20034546 Assumed arXiv.org perpetual, non-exclusive license to distribute this article for submissions made before January 2004 http://arxiv.org/licenses/assumed-1991-2003/ Astrophysics astro-ph FOS Physical sciences article-journal Article ScholarlyArticle Text 2004 ftdatacite https://doi.org/10.48550/arxiv.astro-ph/0404443 https://doi.org/10.1051/0004-6361:20034546 2022-04-01T16:28:53Z We present 2D Monte Carlo radiative transfer simulations of prestellar cores. We consider two types of asymmetry: disk-like asymmetry, in which the core is denser towards the equatorial plane than towards the poles; and axial asymmetry, in which the core is denser towards the south pole than the north pole. We limit our treatment to cores with mild asymmetries, which are exposed directly to the interstellar radiation field or are embedded inside molecular clouds. The isophotal maps of a core depend strongly on the viewing angle. Maps at wavelengths longer than the peak of the SED (e.g. 850 micron) essentially trace the column-density. Thus, for instance, cores with disk-like asymmetry appear elongated when mapped at 850 micron from close to the equatorial plane. However, at wavelengths near the peak of the SED (e.g. 200 micron), the emissivity is more strongly dependent on the temperature, and therefore, at particular viewing angles, there are characteristic features which reflect a more complicated convolution of the density and temperature fields within the core. These characteristic features are on scales 1/5 to 1/3 of the overall core size, and so high resolution observations are needed to observe them. They are also weaker if the core is embedded in a molecular cloud (because the range of temperature within the core is then smaller), and so high sensitivity is needed to detect them. Herschel, to be launched in 2007, will in principle provide the necessary resolution and sensitivity at 170 to 250 micron. : 16 pages, 22 figures, accepted by A&A, also available (with high resolution figures) at http://www.astro.cf.ac.uk/pub/Dimitrios.Stamatellos/publications/ Text South pole DataCite Metadata Store (German National Library of Science and Technology) South Pole North Pole
institution Open Polar
collection DataCite Metadata Store (German National Library of Science and Technology)
op_collection_id ftdatacite
language unknown
topic Astrophysics astro-ph
FOS Physical sciences
spellingShingle Astrophysics astro-ph
FOS Physical sciences
Stamatellos, D.
Whitworth, A. P.
Andre, P.
Ward-Thompson, D.
Radiative transfer models of non-spherical prestellar cores
topic_facet Astrophysics astro-ph
FOS Physical sciences
description We present 2D Monte Carlo radiative transfer simulations of prestellar cores. We consider two types of asymmetry: disk-like asymmetry, in which the core is denser towards the equatorial plane than towards the poles; and axial asymmetry, in which the core is denser towards the south pole than the north pole. We limit our treatment to cores with mild asymmetries, which are exposed directly to the interstellar radiation field or are embedded inside molecular clouds. The isophotal maps of a core depend strongly on the viewing angle. Maps at wavelengths longer than the peak of the SED (e.g. 850 micron) essentially trace the column-density. Thus, for instance, cores with disk-like asymmetry appear elongated when mapped at 850 micron from close to the equatorial plane. However, at wavelengths near the peak of the SED (e.g. 200 micron), the emissivity is more strongly dependent on the temperature, and therefore, at particular viewing angles, there are characteristic features which reflect a more complicated convolution of the density and temperature fields within the core. These characteristic features are on scales 1/5 to 1/3 of the overall core size, and so high resolution observations are needed to observe them. They are also weaker if the core is embedded in a molecular cloud (because the range of temperature within the core is then smaller), and so high sensitivity is needed to detect them. Herschel, to be launched in 2007, will in principle provide the necessary resolution and sensitivity at 170 to 250 micron. : 16 pages, 22 figures, accepted by A&A, also available (with high resolution figures) at http://www.astro.cf.ac.uk/pub/Dimitrios.Stamatellos/publications/
format Text
author Stamatellos, D.
Whitworth, A. P.
Andre, P.
Ward-Thompson, D.
author_facet Stamatellos, D.
Whitworth, A. P.
Andre, P.
Ward-Thompson, D.
author_sort Stamatellos, D.
title Radiative transfer models of non-spherical prestellar cores
title_short Radiative transfer models of non-spherical prestellar cores
title_full Radiative transfer models of non-spherical prestellar cores
title_fullStr Radiative transfer models of non-spherical prestellar cores
title_full_unstemmed Radiative transfer models of non-spherical prestellar cores
title_sort radiative transfer models of non-spherical prestellar cores
publisher arXiv
publishDate 2004
url https://dx.doi.org/10.48550/arxiv.astro-ph/0404443
https://arxiv.org/abs/astro-ph/0404443
geographic South Pole
North Pole
geographic_facet South Pole
North Pole
genre South pole
genre_facet South pole
op_relation https://dx.doi.org/10.1051/0004-6361:20034546
op_rights Assumed arXiv.org perpetual, non-exclusive license to distribute this article for submissions made before January 2004
http://arxiv.org/licenses/assumed-1991-2003/
op_doi https://doi.org/10.48550/arxiv.astro-ph/0404443
https://doi.org/10.1051/0004-6361:20034546
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