Oscillations of rapidly rotating stratified neutron stars

Understand

We use time-evolutions of the linear perturbation equations to study the oscillations of rapidly rotating neutrons stars.

• Our models account for the buoyancy due to composition gradients and we study, for the first time, the nature of the resultant g-modes in a fast spinning star.
• We provide detailed comparisons of non-stratified and stratified models.
• This leads to an improved understanding of the relationship between the inertial modes of a non-stratified star and the g-modes of a stratified system.