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IMF not only describes the formation and evolution of individual stars, it also serves as an important link that describes the formation and evolution of galaxies. [1] The IMF is often given as a probability density function (PDF) that describes the probability of a star that has a certain mass during its formation. [2]
Westerhout 51 nebula in Aquila - one of the largest star factories in the Milky Way (August 25, 2020). Star formation is the process by which dense regions within molecular clouds in interstellar space—sometimes referred to as "stellar nurseries" or "star-forming regions"—collapse and form stars. [1]
Representative lifetimes of stars as a function of their masses The change in size with time of a Sun-like star Artist's depiction of the life cycle of a Sun-like star, starting as a main-sequence star at lower left then expanding through the subgiant and giant phases, until its outer envelope is expelled to form a planetary nebula at upper right Chart of stellar evolution
Composite image showing young stars in and around molecular cloud Cepheus B.. This is a list of star-forming regions located in the Milky Way Galaxy and in the Local Group.Star formation occurs in molecular clouds which become unstable to gravitational collapse, and these complexes may contain clusters of young stars and regions of ionized gas called H II regions.
Star formation; Object classes; Interstellar medium; Molecular cloud; Bok globule; Dark nebula; Young stellar object; Protostar; Pre-main-sequence star; T Tauri star; Herbig Ae/Be star; Herbig–Haro object; Theoretical concepts; Accretion; Initial mass function; Jeans instability; Kelvin–Helmholtz mechanism; Nebular hypothesis; Planetary ...
Typical boundary conditions set the values of the observable parameters appropriately at the surface (=) and center (=) of the star: () =, meaning the pressure at the surface of the star is zero; () =, there is no mass inside the center of the star, as required if the mass density remains finite; () =, the total mass of the star is the star's ...
Gravitational collapse of a massive star, resulting in a Type II supernova. Gravitational collapse is the contraction of an astronomical object due to the influence of its own gravity, which tends to draw matter inward toward the center of gravity. [1] Gravitational collapse is a fundamental mechanism for structure formation in the universe.
In particular, 24μ infrared (MIPS) emission shows where a new generation of stars heats the remains of the supernova remnant that induced their formation. In contrast to star formation in density-wave theories, which are limited to disk-shaped galaxies and produce global spiral patterns, SSPSF applies equally well to spirals, to irregular ...