Vibrational modes or instabilities in neutron stars revealing internal structure.Neutron star oscillations are the vibrational modes of the densest observable objects in the universe. These stars, with masses comparable to the Sun compressed into a sphere of about 20 kilometers in diameter, can ring like a bell when disturbed by starquakes, accretion, or mergers. The frequencies of these oscillations depend on the star's internal structure, including the equation of state of nuclear matter at densities far beyond what can be probed in terrestrial laboratories.
The theoretical framework for stellar oscillations was developed in the 1960s, but the first observational evidence for neutron star oscillations came in the 1990s from X-ray observations of quasi-periodic oscillations in accreting neutron stars. The field gained momentum with the detection of gravitational waves from neutron star mergers, which are expected to excite oscillations.
The oscillations are driven by various restoring forces: pressure (like sound waves), gravity (like surface waves on a star), and even the strong nuclear force. They manifest as periodic variations in the star's luminosity, rotation, or gravitational wave emission. Different modes—such as radial, non-radial, pressure (p-modes), gravity (g-modes), and shear (s-modes)—probe different layers of the star, from the crust to the superfluid core. By measuring their frequencies and damping times, astronomers can infer the star's mass, radius, and composition.
Neutron star oscillations are used to constrain the equation of state of dense nuclear matter, which is essential for understanding nuclear physics, supernovae, and the behavior of matter at extreme densities. They also provide a way to test general relativity in strong gravitational fields.
The frequencies of neutron star oscillations can range from a few hertz to over a kilohertz, meaning some modes vibrate more than a thousand times per second—far faster than any musical instrument.
| f_ISCO | variable | orbital frequency at ISCO — fréquence hertz |
| M | variable | mass of the central object — masse kilogram |
| c | constante | speed of light in vacuum — vitesse de la lumière = 299792458 metre per second |
| G | constante | Newton's constant of universal gravitation — constante gravitationnelle = 6.67430e-11 cubic metre per kilogram per second squared |
| ψ | variable | perturbation amplitude — fonction d'onde |
| A | variable | initial amplitude — amplitude |
| ω_I | variable | imaginary part of frequency (decay rate) — taux de désintégration per second |
| ω_R | variable | real part of frequency (oscillation frequency) — fréquence angulaire per second |
| φ | variable | phase offset — phase |
