Mass transfer in white dwarf-neutron star binaries
We use a modified Smoothed Particle Hydrodynamics scheme called Oil-on-Water. It treats stellar body (Water) separately from the atmosphere (Oil). This allows us to model arbitrarily small mass transfer rates. The present project improves on the original research by (Church et al, 2009). Key references are: (Bobrick, Davies and Church, 2017), (Church et al, 2009), (Lajoie & Sills, 2011).
Figure: Density section in the orbital plane for a 0.15M⊙ He white dwarf in a binary with a 1.4M⊙ neutron star with eccentricity of 0.04. The snapshot is taken after 13 orbital periods since the beginning of the simulation. The figure is from Bobrick et al. (2017).