Abstract
We present high-resolution hydrodynamical simulations aimed at following the gravitational collapse of a gas core, in which a turbulent spectrum of velocity is implemented only initially. We determine the maximal value of the ratio of kinetic energy to gravitational energy, denoted here by \((\frac{E_{\mathrm{kin}} }{E_{\mathrm{grav}}} )_{\max}\), so that the core (i) will collapse around one free-fall time of time evolution or (ii) will expand unboundedly, because it has a value of \(\frac{E_{\rm kin}}{E_{\mathrm{grav}}}\) larger than \(( \frac{E_{\mathrm{kin}}}{E_{\mathrm{grav}}} )_{\mathrm{max}}\). We consider core models with a uniform or centrally condensed density profile and with velocity spectra composed of a linear combination of one-half divergence-free turbulence type and the other half of a curl-free turbulence type. We show that the outcome of the core collapse are protostars forming either (i) a multiple system obtained from the fragmentation of filaments and (ii) a single primary system within a long filament. In addition, some properties of these protostars are also determined and compared with those obtained elsewhere.
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Notes
Defined as the ratio of the velocity magnitude to the sound speed, \(v/c_{0}\).
The possibility that other observations have values outside this range is still open.
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The author thankfully acknowledge the computer resources, technical expertise and support provided by the Laboratorio Nacional de Supercómputo del Sureste de México through the grant number O-2016/047.
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Arreaga-García, G. The extreme initial kinetic energy allowed by a collapsing turbulent core. Astrophys Space Sci 363, 157 (2018). https://doi.org/10.1007/s10509-018-3379-x
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DOI: https://doi.org/10.1007/s10509-018-3379-x