Stellar Astrophysics
Hydrogen generally determines a star's nuclear lifetime because it is used as the main source of fuel in a main sequence star. It constitutes much of the star's core and is surrounded by what is known as a helium shell. Hydrogen becomes helium in the nuclear reaction that takes place within stars; when the hydrogen has been exhausted, the star moves on to another phase of its life and begins burning the helium.
where M is the mass of the star, X is the fraction of the star (by mass) that is composed of the fuel, L is the star's luminosity, Q is the energy released per mass of the fuel from nuclear fusion (the chemical equation should be examined to get this value), and F is the fraction of the star where the fuel is burned (F is generally equal to .1 or so). As an example, the Sun's nuclear time scale is approximately 10 billion years.
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Read more about this topic: Nuclear Timescale