James R. Murray

SPH simulations of tidally unstable accretion discs in cataclysmic variables

We numerically study the precessing disk model for superhump in the SU~UMa subclass of cataclysmic variables, using a two dimensional SPH code specifically designed for thin disk problems. Two disk simulations for a binary with mass ratio

Simulations of superhumps and superoutbursts

q=\frac{3}{17}

Superhumps in low‐mass X‐ray binaries

(similar to OY~Car) are performed, in order to investigate the Lubow (1991 a,b) tidal resonance instability mechanism. In the first calculation, a disk evolves under steady mass transfer from

Dust distribution in protoplanetary disks Vertical settling and radial migration

L_1

The precession of eccentric discs in close binaries

. In the second simulation, mass is added in Keplerian orbit to the inner disk. The two disks follow similar evolutionary paths. However the

Comprehensive simulations of superhumps

L_1

The effect of a planet on the dust distribution in a 3D protoplanetary disk

stream-disk interaction is found to slow the disks radial expansion and to circularise gas orbits. The initial eccentricity growth in our simulations is exponential at a rate slightly less than predicted by Lubow (1991a). We do not observe a clearing of material from the resonance region via the disks tidal response to the

Tilted accretion discs in cataclysmic variables: tidal instabilities and superhumps

m=2

Three-dimensional smoothed particle hydrodynamics simulations of radiation-driven warped accretion discs

component of the binary potential as was described in Lubow (1992). Instead the

Magnetically warped discs in close binaries

m=2