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Self-Consistent Theoretical Models of Collapsing Pre-Stellar Cores

Published online by Cambridge University Press:  21 March 2006

Valery I. Shematovich ,
Boris M. Shustov ,
Dmitri S. Wiebe ,
Yaroslav N. Pavlyuchenkov  and
Zhi-Yun Li
Valery I. Shematovich
Affiliation:
Institute of Astronomy of the Russian Academy of Sciences, 48 Pyatnitskaya str., 119017 Moscow, Russia email: [email protected]
Boris M. Shustov
Affiliation:
Institute of Astronomy of the Russian Academy of Sciences, 48 Pyatnitskaya str., 119017 Moscow, Russia email: [email protected]
Dmitri S. Wiebe
Affiliation:
Institute of Astronomy of the Russian Academy of Sciences, 48 Pyatnitskaya str., 119017 Moscow, Russia email: [email protected]
Yaroslav N. Pavlyuchenkov
Affiliation:
Institute of Astronomy of the Russian Academy of Sciences, 48 Pyatnitskaya str., 119017 Moscow, Russia email: [email protected]
Zhi-Yun Li
Affiliation:
Department of Astronomy, University of Virginia, P.O. Box 3818, Charlottesville, VA 22903, USA email: [email protected]
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Abstract

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We present a coupled dynamical and chemical model for collapsing pre-stellar cores (Li et al. 2002; Shematovich et al. 2003a,b; Pavlyuchenkov et al. 2003). It treats the dynamics of thermally and magnetically supported cores in 1D, with an extended chemical network incorporated. The latest version of the model includes UV-irradiation of the core envelope. We have also developed a 2D Monte Carlo model of radiative transfer to compute molecular line profiles for comparison with observations.

The model allowed us to constrain evolutionary scenarios for collapsing pre-stellar cores, to calculate molecular line profiles from the spatial distribution of chemical species and the velocity field, and to characterize the chemical properties of dense cores.

We have determined line profiles along multiple lines of sight through a given pre-stellar core. This allowed us to compare model predictions with the observational maps of molecular lines available for L1544 and other well studied cores. The comparison of synthetic and observed line profile maps contributed to the understanding of the velocity field and pattern of chemical differentiation observed in individual cores.

Keywords

line: profiles — ISM: magnetic fields — ISM: molecules — stars: formation — ISM: individual (L1544)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 1 , Symposium S231: Astrochemistry: Recent Successes and Current Challenges , August 2005 , pp. 37 - 46
Copyright
2006 International Astronomical Union