Isolated Neutron Stars (NS) are intriguing sources of continuous gravitational waves (GW) that have yet to be detected. To emit GWs, a star typically requires a mass-energy distribution that deviates from axial symmetry with respect to its rotational axis. This deviation often stems from the non-axisymmetric distribution of magnetic energy, which arises from the coupled magnetic and thermal...
Detection of Gravitational wave events involving neutron stars (NS) provides an excellent scenario for understanding the NS interior. In a binary system, the excitation of NS oscillation modes, such as rotational r-mode and fundamental f-mode, can draw energy from the orbital energy and introduce a phase shift in the observed GW waveform. The ignorance of such dynamical mechanisms can bias the...
The finite size of neutron stars in binary systems has an observable effect on the binary evolution due to tidal interactions. These tidal interactions in circular binaries result in an adiabatic evolution, where the frequency of tidal excitations coevolves with the orbital frequency. However, in case the orbit is eccentric, there is a periodic sharp pulse of external tidal force, which...
