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.