Tidal interactions are primarily driven by the gravitational forces exerted between celestial bodies, such as planets, moons, and stars.

The Moon's gravitational pull on Earth's oceans is the primary cause of tides on our planet.

Tidal bulge refers to the deformation of a celestial body's shape caused by tidal forces, resulting in a bulge on the side facing the interacting body.

Tidal locking occurs when the gravitational interaction between two celestial bodies causes their rotation and orbital periods to become synchronized, resulting in one side of the body always facing the other.

Io, a moon of Jupiter, is an example of a tidally locked moon, where one side of the moon always faces Jupiter due to tidal interactions.

Stellar pulsations refer to the periodic variations in a star's luminosity due to oscillations in its interior, causing the star to expand and contract.

Stellar oscillations are primarily driven by the energy released from nuclear fusion reactions in the star's core, which cause the star to expand and contract.

Radial modes are a type of stellar oscillation where the star pulsates radially, expanding and contracting along its radius.

Non-radial modes are a type of stellar oscillation where the star pulsates in a non-radial pattern, causing it to deform in various shapes.

Torsional modes are a type of stellar oscillation that involves the twisting or shearing of the star's interior, causing the star to oscillate in a twisted pattern.

Photometry, which involves measuring the variations in a star's brightness, is the primary method used to study stellar oscillations.

Studying stellar oscillations can provide information about a star's mass, radius, age, composition, rotation, and magnetic fields.

The Kepler Space Telescope was specifically designed to study stellar oscillations and detect exoplanets.

Astroseismology is the study of stellar oscillations, which provides insights into the internal structure and properties of stars.

Tidal interactions can affect the evolution of celestial bodies through tidal heating, tidal dissipation, and tidal locking, influencing their internal structure, rotation, and orbital characteristics.