Abstract
We investigate the details of protostellar mass accretion, \(\dot{M}\), during the collapse of isolated, initially uniformly rotating, low-mass cores, using hydrodynamic models of star formation. The assumption of rigid rotation is supported by recent observations that there is no apparent correlation between the level of turbulence and fragmentation in dense cores, suggesting that turbulence works mainly before gravitationally bound pre-stellar cores form and that their inner parts are likely to be velocity coherent. We perform high-resolution calculations using the Smoothed Particle Hydrodynamics (SPH) code GADGET-2, modified by the inclusion of sink particles. We compare our results with theoretical models of star formation based on gravoturbulent fragmentation and with observational data. We find that on the small scales of low-mass, dense cores the details of mass accretion and the statistical properties of the resulting stellar ensembles bear little dependence on whether the contracting gas is turbulent or rotating as a whole.
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Acknowledgments
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 and the Fondo Nacional de Ciencia, Tecnología e Innovación of Venezuela (FONACIT) under grant PC 201204710 (contract 112-1077).
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Klapp, J., Sigalotti, L.D.G., Zavala, M. (2014). Stellar Mass Accretion Rates from Fragmentation of a Rotating Core. In: Sigalotti, L., Klapp, J., Sira, E. (eds) Computational and Experimental Fluid Mechanics with Applications to Physics, Engineering and the Environment. Environmental Science and Engineering(). Springer, Cham. https://doi.org/10.1007/978-3-319-00191-3_14
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DOI: https://doi.org/10.1007/978-3-319-00191-3_14
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