Abstract
The aim of this paper is to present a set of numerical simulations of a penetrating collision, in which a small gas core (the bullet) penetrates a larger gas core (the target). In the target core, the gravitational collapse is supposed to be ongoing before the collision. Each colliding core has a uniform density profile and rigid body rotation; besides the mass and size of the target core have been chosen to represent the observed molecular cloud core L1544. We modified the Lagrangian code \(\textit{Gagdet}2\) to identify when a gas particle can become an accretion center, and to inherit the mass and momentum of all the very close neighboring particles. Three collision models are here considered for pre-collision velocities \(v/c_0=\) \(2.5\), \(5.0\), and \(10\) Mach. The outcome of these collision models are presented only for two different values of the bullet’s radius, that is for \(R_0/4\), and \(R_0/2\) where \(R_0\) is the radius of the target core. Such collision models reveal how accretion centers are formed, with a spatial distribution that strongly depends on the pre-collision velocity. We thus show hereby that penetrating collisions may have a major and favorable influence in the star formation process.
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Acknowledgments
We would like to thank ACARUS-UNISON for the use of their computing facilities. This work has been partially supported by the Consejo Nacional de Ciencia y Tecnología of Mexico (CONACyT) under the project CONACyT-EDOMEX-2011-C01-165873.
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Arreaga-García, G., Klapp, J. (2015). Accretion Centers Induced in a Molecular Cloud Core After a Penetrating Collision. In: Klapp, J., Ruíz Chavarría, G., Medina Ovando, A., López Villa, A., Sigalotti, L. (eds) Selected Topics of Computational and Experimental Fluid Mechanics. Environmental Science and Engineering(). Springer, Cham. https://doi.org/10.1007/978-3-319-11487-3_41
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DOI: https://doi.org/10.1007/978-3-319-11487-3_41
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