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Stellar density is the average number of stars within a unit volume. It is similar to the stellar mass density, which is the total solar masses (M Sun ) found within a unit volume. Typically, the volume used by astronomers to describe the stellar density is a cubic parsec (pc 3 ).
Parts-per-million chart of the relative mass distribution of the Solar System, each cubelet denoting 2 × 10 24 kg. This article includes a list of the most massive known objects of the Solar System and partial lists of smaller objects by observed mean radius. These lists can be sorted according to an object's radius and mass and, for the most ...
Download as PDF; Printable version; ... Pages Related to Stellar properties, Pages using the word stellar in a physics context. ... Stellar density; Stellar disk ...
Stellar structure models describe the internal structure of a star in detail and make predictions about the luminosity, the color and the future evolution of the star. Different classes and ages of stars have different internal structures, reflecting their elemental makeup and energy transport mechanisms.
IMF and PDMF can be linked through the "stellar creation function". [2] Stellar creation function is defined as the number of stars per unit volume of space in a mass range and a time interval. In the case that all the main sequence stars have greater lifetimes than the galaxy, IMF and PDMF are equivalent.
A Hess diagram plots the relative density of occurrence of stars at differing color–magnitude positions of the Hertzsprung–Russell diagram for a given galaxy or resolved stellar population. The diagram is named after R. Hess who originated it in 1924. [1] Its use dates back to at least 1948. [2]
In a solar model, as described in stellar structure, one considers the density (), temperature T(r), total pressure (matter plus radiation) P(r), luminosity l(r) and energy generation rate per unit mass ε(r) in a spherical shell of a thickness dr at a distance r from the center of the star.
R136 has around 200 times the stellar density of a typical OB association such as Cygnus OB2. [8] The central R136 concentration of the cluster is about 2 parsecs across, although the whole NGC 2070 cluster is much larger. [8] R136 is thought to be less than 2 million years old.