Coupling Chemical Evolution with SPH

Coupling Elastic Solids with SPH Fluids

We propose a method for handling elastic solids in SPH fluids. Our approach samples triangulated surfaces of solids using boundary particles. To prevent fluid particle tunneling in case of large expansions, additional boundary particles are adaptively generated to prevent gaps and undesired leakage. Furthermore, as an object compresses, particles are adaptively removed to avoid unnecessary comp...

SPH code for dynamical and chemical evolution of disk galaxies

Coupling SPH with a 1-D Boussinesq-type wave model

The high computational cost of SPH remains problematic in dealing with wave propagation, especially when the domains considered are large. In order to overcome this difficulty, we propose to couple 2-D SPH with a 1-D Finite Difference Boussinesq-type model. The latter deals with wave propagations for most of the spatial domain, whereas SPH computations focus on the shoreline or close to off-sho...

Chemical evolution with radial mixing

Models of the chemical evolution of our Galaxy are extended to include radial migration of stars and flow of gas through the disc. The models track the production of both iron and α elements. A model is chosen that provides an excellent fit to the metallicity distribution of stars in the Geneva–Copenhagen survey (GCS) of the solar neighbourhood, and an acceptable fit to the local Hess diagram. ...

Contact line hydrodynamics with SPH

Surface tension effects can dominate multi-phase flows when the length scales of the problem are small. The resulting Capillary forces at a phase interface between two immiscible fluids are proportional to the local curvature of the flow and try to minimize the interfacial area. A more complex situation occurs when three phases are in contact or when two phases are in contact with a wall. The s...