selfgravitational

Selfgravitation refers to the gravitational attraction between the parts of a single body, as opposed to the gravitational attraction between separate bodies. This concept is particularly relevant in astrophysics and celestial mechanics, where it helps explain the behavior of large, massive objects such as stars, planets, and galaxies.

In the context of a celestial body, selfgravitation is the force that holds the body together. For example, the gravitational pull of a star's mass keeps its gases and other materials from escaping into space. This force is what gives stars their spherical shape and determines their stability.

Selfgravitation also plays a crucial role in the formation and evolution of celestial bodies. In the early stages of a star's life, for instance, the gravitational attraction between its parts causes it to collapse under its own weight, leading to nuclear fusion and the birth of a star.

The study of selfgravitation involves complex mathematical models and simulations, as it requires accounting for the distribution of mass within a body and the resulting gravitational field. These models are essential for understanding phenomena such as stellar oscillations, planetary ring dynamics, and the structure of galaxies.

In summary, selfgravitation is a fundamental concept in astrophysics that describes the gravitational attraction between the parts of a single body. It influences the shape, stability, and evolution of celestial objects, and its study is crucial for understanding the universe's structure and dynamics.