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m Reverted edit by 200.68.152.163 (talk) to last version by JeffSpaceman |
The math didn't add up. The sun is roughly correctly dated, and the total age is correct using the reference given. Thus, the math needs correcting. |
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This relationship applies to main-sequence stars in the range {{solar mass|0.1–50}}.<ref name=rolfs_rodney88/>
The amount of fuel available for nuclear fusion is proportional to the mass of the star. Thus, the lifetime of a star on the main sequence can be estimated by comparing it to solar evolutionary models. The [[Sun]] has been a main-sequence star for about 4.5 billion years and it will become a red giant in
: <math>\tau_\text{MS} \approx
10^{10} \text{years} \left[ \frac{M}{M_\bigodot} \right] \left[ \frac{L_\bigodot}{L} \right] =
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