Gravitational wave emission from accreting magnetised neutron stars.

With their high spin rates, accreting neutron stars in low-mass X-ray binaries are a potentially detectable source of gravitational radiation. In this project, we aim to model such accreting neutron stars with a view to identifying mechanisms whereby mass asymmetries may develop, which would then produce a long-lived continuous gravitational wave signal. Of particular interest will be the role of the magnetic field in channelling the accretion flow, and modifying the heating and cooling within the star, to see what level of mass asymmetry may result.