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Protostellar discs formed from turbulent cores

Walch, Stefanie, Naab, T., Whitworth, Anthony Peter, Burkert, A. and Gritschneder, M. 2010. Protostellar discs formed from turbulent cores. Monthly Notices of the Royal Astronomical Society 402 (4) , pp. 2253-2263. 10.1111/j.1365-2966.2009.16058.x

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We investigate the collapse and fragmentation of low-mass, trans-sonically turbulent pre-stellar cores, using smoothed particle hydrodynamics simulations. The initial conditions are slightly supercritical Bonnor–Ebert spheres, all with the same density profile, the same mass (MO= 6.1 M⊙) and the same radius (RO= 17 000 au), but having different initial turbulent velocity fields. 400 turbulent velocity fields have been generated, all scaled so that the mean Mach number is . Then, a subset of these (in total 11 setups), having a range of net angular momenta, j, has been evolved. The evolution of these turbulent cores is significantly different from the collapse of a rigidly rotating core. It is not strongly correlated with j. Instead, it is moderated by the formation of filamentary structures due to converging turbulent flows. A high fraction (9 out of 13, ∼69 per cent) of the individual protostars forming from turbulent cores are attended by resolved (R≥ 10 au) protostellar accretion discs, but only a very small fraction (1 out of 9, ∼11 per cent) of these discs is sufficiently cool and extended to develop non-linear gravitational instabilities and fragment. Protostars with discs show two distinct growth modes. They initially grow by direct gravitational collapse, followed by subsequent disc accretion.

Item Type: Article
Date Type: Publication
Status: Published
Schools: Advanced Research Computing @ Cardiff (ARCCA)
Physics and Astronomy
Subjects: Q Science > QB Astronomy
Uncontrolled Keywords: hydrodynamics; circumstellar matter; stars: formation; infrared: stars
Publisher: John Wiley
ISSN: 0035-8711
Last Modified: 04 Jun 2017 03:14

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