Abstract
We examine the problem of the collapse and fragmentation of molecular clouds with a Gaussian density distribution with high resolution, double precision numerical simulations using the GADGET-2 code. To describe the thermodynamic properties of the cloud during the collapse—to mimic the rise of temperature predicted by radiative transfer—we use a barotropic equation of state that introduces a critical density to separate the isothermal and adiabatic regimes. We discuss the effects of this critical density in the formation of multiple systems. We confirm the tendency found for Plummer and Gaussian models that if the collapse changes from isothermal to adiabatic at earlier times that occurs for the models with a lower critical density, the collapse is slowed down, and this enhances the fragments’ change to survive. However, this effect happens up to a threshold density below which single systems tend to form. On the other hand, by setting a bigger initial perturbation amplitude, the collapse is faster and in some cases a final single object is formed.
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Acknowledgments
J.L.C.C. thanks the Berkeley Center for Cosmological Physics for hospitality, and gratefully acknowledges support from a UC MEXUS-CONACYT Grant, and a CONACYT Grant No. 84133-F.
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Gómez-Ramírez, F., Klapp, J., Cervantes-Cota, J.L., Arreaga-García, G., Bahena, D. (2012). Collapse and Fragmentation of Gaussian Barotropic Protostellar Clouds. In: Klapp, J., Cros, A., Velasco Fuentes, O., Stern, C., Rodriguez Meza, M. (eds) Experimental and Theoretical Advances in Fluid Dynamics. Environmental Science and Engineering(). Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-17958-7_15
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DOI: https://doi.org/10.1007/978-3-642-17958-7_15
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