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Stellar structure codes (meaning computer programs calculating the model's variables) either interpolate in a density-temperature grid to obtain the opacity needed, or use a fitting function based on the tabulated values. A similar situation occurs for accurate calculations of the pressure equation of state.
The scope of the list is still restricted to the main sequence spectral types: M, K, F, G, A, B and O. It may be later expanded to other types, such as S , D or C . The Alpha Centauri star system is the closest star system to the Sun .
Pages Related to Stellar properties, Pages using the word stellar in a physics context. Stellar aberration; Stellar age estimation; Stellar archaeology; Stellar astronomy; Stellar atmosphere; Stellar birthline; Stellar black hole; Stellar cartography; Stellar chemistry; Stellar chonography; Stellar classification; Stellar cluster; Stellar ...
Theoretical calculations of stellar structure and the evolution of stars produce plots that match those from observations. This type of diagram could be called temperature-luminosity diagram , but this term is hardly ever used; when the distinction is made, this form is called the theoretical Hertzsprung–Russell diagram instead.
In astronomy, the main sequence is a classification of stars which appear on plots of stellar color versus brightness as a continuous and distinctive band. Stars on this band are known as main-sequence stars or dwarf stars , and positions of stars on and off the band are believed to indicate their physical properties, as well as their progress ...
An HR Diagram of PMS stars with different masses. The Hayashi Track is depicted as vertical lines, while the Henyey are horizontal. Higher mass stars spend very little time on the Hayashi Track, while the lowest mass stars never reach the Heyney Track, with a gradient seen of time spent on each track as the mass increases.
This stellar model, technically the spherically symmetric quasi-static model of a star, has stellar structure described by several differential equations derived from basic physical principles. The model is constrained by boundary conditions , namely the luminosity , radius, age and composition of the Sun, which are well determined.
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.