Dynamical tides in binary neutron stars 

Neutron stars (NSs) are fascinating objects because they have so high interior densities that cannot be reproduced by any terrestrial laboratories. Tidal interactions in binary NSs thus offer us a unique window to study physics at such extreme densities. 

While most studies on tides in binary NSs consider the "equilibrium tide", or the large-scale deformation of the NS, my studies nonetheless focus on the "dynamical tides", or the excitation of internal oscillation modes in the NS. A mode can be supported by buoyancy due to internal composition gradient (g-mode), or by Coriolis force due to rotation (r-mode). Studying the dynamical tides thus allows us to learn about NSs from physics beyond the NS's bulk properties.