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Cooling in protoplanetary accretion discs
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Growth of the gravitational instability in a high resolution (250000
SPH particles) 3D simulation of a protoplanetary accretion disc.
Mpeg animation (400x400, 2.5 Mb)
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Evolution of a protoplanetary accretion disc in which the cooling time is
sufficiently small for fragmentation to occur.
Gif animation (300x300, 2.1 MB)
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Central region of the above simulation (r < 12.5).
Gif animation (300x300, 2.1 Mb)
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The evolution of a protoplanetary disc with a mass equal to that of the central star.
Quicktime movie (600x600, 40 kb)
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The evolution of a self-gravitating disc undergoing a co-planar encounter with an
object with a mass equal to that of the disc and that is in a parabolic orbit.
Gif animation (400x420, 4 Mb)
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The locality of transport in self-gravitating protoplanetary discs, G. Lodato, W.K.M. Rice, MNRAS,
351, 630, 2004
Substellar companions and isolated planetary mass objects from protostellar disc fragmentation,
W.K.M. Rice, P.J. Armitage, I.A. Bonnell, M.R. Bate, S.V. Jeffers, S.G. Vine,
MNRAS, 346, L36, 2003
The effect of cooling on
the global stability of self-gravitating accretion discs, W.K.M. Rice,
P.J. Armitage, M.R. Bate, I.A. Bonnell, MNRAS, 339, 1025, 2003
Astrometric signatures of
self-gravitating protoplanetary discs, W.K.M. Rice, P.J. Armitage, M.R.
Bate, I.A. Bonnell, MNRAS, in press
Numerical simulations made use of the UK
Astrophysical Fluids Facility.
Ken Rice's homepage
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