|
Gravitational compression is a phenomenon in which gravity, acting on the mass of an object, compresses it, reducing its size and increasing the object's density. At the center of a planet or star, gravitational compression produces heat by the Kelvin–Helmholtz mechanism. This is the mechanism that explains how Jupiter continues to radiate heat produced by its gravitational compression.〔(【引用サイトリンク】 Jupiter )〕 The most common reference to gravitational compression is with respect to stellar evolution. The Sun and other main-sequence stars are produced by the initial gravitational collapse of a molecular cloud. Assuming the mass of the material is large enough, gravitational compression reduces the size of the core, increasing its temperature until hydrogen fusion can begin. This hydrogen-to-helium fusion reaction releases energy that balances the inward gravitational pressure and the star becomes stable for millions of years. No further gravitational compression occurs until the hydrogen is nearly used up, reducing the thermal pressure of the fusion reaction. At the end of the Sun's life, gravitational compression will turn it into a white dwarf.〔 〕 At the other end of the scale are massive stars, which burn their fuel very quickly, ending their lives as supernovae, after which further gravitational compression will produce either a neutron star〔 〕 or a black hole〔 〕 from the remnants. For planets and moons, equilibrium is reached when the compression due to gravity is balanced by a pressure gradient in the opposite direction due to the strength of the material, at which point gravitational compression ceases. ==References== 〔 抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』 ■ウィキペディアで「Gravitational compression」の詳細全文を読む スポンサード リンク
|