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Place a stub template at the very end of the article, after the "External links" section, any navigation templates, and the category tags. As usual, templates are added by including their name inside double braces, e.g. {{Stellar-evolution-stub}} .
Stellar evolution is the process by which a star changes over the course of its lifetime and how it can lead to the creation of a new star. Depending on the mass of the star, its lifetime can range from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the current age of the ...
Print/export Download as PDF; Printable version; In other projects Wikimedia Commons; Wikidata item; ... Pages in category "Stellar evolution"
"Stellar Ships" or "Star Ships" (Russian name "Zvezdnye Korabli", Russian: Звёздные корабли) is a short story by the Soviet writer and paleontologist Ivan Yefremov written in 1944 and first published in 1948 in the USSR.
In stellar astronomy, the Algol paradox is a paradoxical situation when elements of a binary star seem to evolve in discord with the established theories of stellar evolution. [1] A fundamental feature of these theories is that the rate of evolution of stars depends on their mass: The greater the mass, the faster this evolution, and the more ...
The horizontal branch (HB) is a stage of stellar evolution that immediately follows the red-giant branch in stars whose masses are similar to the Sun's. Horizontal-branch stars are powered by helium fusion in the core (via the triple-alpha process) and by hydrogen fusion (via the CNO cycle) in a shell surrounding the core.
The usual endpoint of stellar evolution is the formation of a compact star.. All active stars will eventually come to a point in their evolution when the outward radiation pressure from the nuclear fusions in its interior can no longer resist the ever-present gravitational forces.
The SSM is used to test the validity of stellar evolution theory. In fact, the only way to determine the two free parameters of the stellar evolution model, the helium abundance and the mixing length parameter (used to model convection in the Sun), are to adjust the SSM to "fit" the observed Sun.