NDLI: Simulations of protostellar collapse using multigroup radiation hydrodynamics

Content Provider	EDP Sciences
Author	Neil Vaytet Gilles Chabrier Edouard Audit Benoît Commerçon Jacques Masson Jason Ferguson Franck Delahaye
Abstract	Context. Star formation begins with the gravitational collapse of a dense core inside a molecular cloud. As the collapse progresses, the centre of the core begins to heat up as it becomes optically thick. The temperature and density in the centre eventually reach high enough values where fusion reactions can ignite, and the protostar is born. This sequence of events entails many physical processes, of which radiative transfer is of paramount importance. Simulated collapsing cores without radiative transfer rapidly become thermally supported before reaching high enough temperatures and densities, preventing the formation of stars.Aims. Many simulations of protostellar collapse make use of a grey treatment of radiative transfer coupled to the hydrodynamics. However, interstellar gas and dust opacities present large variations as a function of frequency, which can potentially be overlooked by grey models and lead to significantly different results. In this paper, we follow up on a previous paper on the collapse and formation of Larson’s first core using multigroup radiation hydrodynamics (Paper I) by extending the calculations to the second phase of the collapse and the formation of Larson’s second core.Methods. We have made the use of a non-ideal gas equation of state as well as an extensive set of spectral opacities in a spherically symmetric fully implicit Godunov code to model all the phases of the collapse of a 0.1, 1, and 10 M_{⊙_{cloud cores.Results. We find that, for an identical central density, there are only small differences between the grey and multigroup simulations. The first core accretion shock remains supercritical while the shock at the second core border is found to be strongly subcritical with all the accreted energy being transfered to the core. The size of the first core was found to vary somewhat in the different simulations (more unstable clouds form smaller first cores) while the size, mass, and temperature of the second cores are independent of initial cloud mass, size, and temperature.Conclusions. Our simulations support the idea of a standard (universal) initial second core size of ~3 × 10^{-3^{AU and mass ~1.4 × 10^{-3^{M_{⊙_{. The grey approximation for radiative transfer appears to perform well in one-dimensional simulations of protostellar collapse, most probably because of the high optical thickness of the majority of the protostar-envelope system. A simple estimate of the characteristic timescale of the second core suggests that the effects of using multigroup radiative transfer may be more important in the long-term evolution of the protostar.}}}}}}}}
Page Count	15
File Format	HTM / HTML PDF
ISSN	00046361
Alternate Webpage(s)	https://www.aanda.org/articles/aa/abs/2013/09/aa21423-13/aa21423-13.html
e-ISSN	14320746
Journal	Astronomy & Astrophysics
Volume Number	557
DOI	10.1051/0004-6361/201321423
Language	English
Publisher	EDP Sciences
Publisher Date	2013-09-01
Access Restriction	Open
Rights Holder	© ESO, 2013
Subject Keyword	stars: formation methods: numerical hydrodynamics radiative transfer stars: protostars stars: formation / methods: numerical / hydrodynamics / radiative transfer / stars: protostars
Content Type	Text
Resource Type	Article
Subject	Astronomy and Astrophysics Space and Planetary Science

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