stellar model: A table of numbers representing the conditions in various layers within a star.
stellar parallax (p): A measure of stellar distance. (See parallax.)
stony meteorite: A meteorite composed of silicate (rocky) material.
Stellar models suggest that the star formed during the collapsing of a molecular cloud, and that after 10 million years, its internal energy generation was derived entirely from nuclear reactions.
A stellar model in which the rotational and magnetic axes are not coincident. Magnetic stars are generally assumed to be oblique rotators of this kind.
Obliquity ...
A stellar model in which energy is transported by radiation throughout the whole star and the ratio of the radiation pressure to the gas pressure is assumed to be constant. [H76]
Eddy Currents ...
The stellar models used here came from two separate sources. Both are available via the web from the Strasbourg (France) Data Center.
Analytic stellar models using polytropes are relatively easy to build, as polytropes can be inserted into the equation of hydrostatic equilibrium
dP/dr = -ρ d(Φ)/dr
and the Poisson equation ...
Theoretical stellar astronomy includes various forms of stellar modeling as well as models of specific phenomena which have been observationally associated with stars (such as magnetic reconnection models for stellar flares or Raymond-Smith models ...
According to stellar models, the maximum mass a brown dwarf can have is . Young brown dwarfs which are gravitationally contracting can release substantial amounts of gravitational energy, but older stars radiate from remnant internal heat only.
Stellar models have been able to predict the mass of stars for about 50 years, so based upon the spectrum of a star, its mass can be accurately determined. So with the mass and period, the semi-major axis (r) can be calculated.
The mass, radius, surface gravity, and rotation period can then be estimated based on stellar models.
This relationship was derived from the observations of the masses of various types of main sequence stars, but it has also been demonstrated by the calculation of stellar models of main sequence stars.
Recently the Padova models (actually the isochrones from Bertelli et al. 1994 A&AS 97, 851 with the Worthey stellar models) became similarly available. The STScI group also has a WWW library of young population models.
the line strengths of different lines, it is possible to estimate properties such as temperature and pressure and density in the gas, as well as how much the layers of gas in the star are mixed. We can compare the observed values to stellar models to ...
 See also: Model, Star, Light, Temperature, Energy
  
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