The Death of Stars
Like the Sun

(Section Not Complete)

Life and Death of Stars

Stellar Evolution

The following figure illustrates three categories of post main sequence evolution.

The adjacent image illustrates the conditions necessary for hydrogen shell burning.

The figure below shows the three branches of giant stars expected for evolved clusters.

The figure below illustrates schematically the typical evolution after the AGB region, through planetary nebula emission and finally to a white dwarf. This animation illustrates the same thing.

DATABASE of GENEVA STELLAR EVOLUTION MODELS: "An extensive and homogenous database of stellar evolution models for masses between 0.8 and 120 solar masses at different metallicities is available. In general the models include evolutionary phases from the main sequence up to the end of carbon burning for massive stars. Horizontal branch and early asymptotic giant branch models are also provided. The metallicities covered are Z=0.001, 0.004, 0.008, 0.020 (=Z_solar), and Z=0.04.

In addition to the evolutionary grids we also provide Fortran codes for the calculation of isochrones and stellar population burst models.

Recent models now cover also pre-main sequence phases. Predictions regarding the spectral evolution of massive stars can be obtained from the so-called "combined stellar structure and atmosphere models" (CoStar)."

A (somewhat flaky) DOS program (StarClock) written in Pascal that implements graphic HR diagram evolution based on the above tables can be found at http://www.sci.muni.cz/~ondra/sclock/sclock.html.



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