Main sequence: Difference between revisions

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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 becomestart to expand rapidly towards a red giant in 56.5 billion years,<ref name=apj418>{{cite journal |last=Sackmann |first=I.-Juliana |author2=Boothroyd, Arnold I. |author3=Kraemer, Kathleen E. |title=Our Sun. III. Present and Future |journal=Astrophysical Journal |date=November 1993 |volume=418 |pages=457–468 |doi=10.1086/173407 |bibcode=1993ApJ...418..457S|doi-access=free }}</ref> for a total main-sequence lifetime of roughly 10¹⁰ years. Hence:<ref name=hansen_kawaler94>{{cite book |first=Carl J. |last=Hansen |author2=Kawaler, Steven D. |date=1994 |title=Stellar Interiors: Physical Principles, Structure, and Evolution |page=[https://archive.org/details/stellarinteriors00hans/page/28 28] |publisher=Birkhäuser |isbn=978-0-387-94138-7 |url-access=registration |url=https://archive.org/details/stellarinteriors00hans/page/28}}</ref>

: <math>\tau_\text{MS} \approx

10^{10} \text{years} \left[ \frac{M}{M_\bigodot} \right] \left[ \frac{L_\bigodot}{L} \right] =