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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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 |
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Astrophysics astro-ph FOS Physical sciences |
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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 |
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South Pole North Pole |
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South Pole North Pole |
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South pole |
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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 |
_version_ |
1766202547950845952 |