EPJ Web of Conferences
Volume 46, 2013Instabilities and Structures in Proto-Planetary Disks
|Number of page(s)||4|
|Section||Vortices and Self-Gravity|
|Published online||11 April 2013|
Triggered fragmentation in gravitationally unstable discs: forming fragments at small radii
1 Institut für Astronomie,
ETH Zürich, Wolfgang-Pauli-Strasse
2 Institut für Astronomie und Astrophysik, Universität Tübingen, Auf der Morgenstelle 10, 72076 Tübingen, Germany
3 School of Physics, University of Exeter, Stocker Road, Exeter, EX4 4QL, UK
a e-mail: email@example.com
We carry out three dimensional radiation hydrodynamical simulations of gravitationally unstable discs using to explore the movement of mass in a disc following its fragmentation. Compared to a more quiescent state before it fragments, the radial velocity of the gas increases by up to a factor of ≈ 2 – 3 after fragmentation. While the mass movement occurs both inwards and outwards, the inwards motion can cause the inner spirals to be suciently dense that they may become unstable and potentially fragment. Consequently, the dynamical behaviour of fragmented discs may cause subsequent fragmentation at smaller radii after an initial fragment has formed in the outer disc.
© Owned by the authors, published by EDP Sciences, 2013
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