So, I saw this question (which is quite old) and that's all well and good, but what if I need to (very) roughly calculate the luminosity of a star from the end of the main sequence? Let's assume that this is a non-extreme mass star (K-A) and can use $10M^{-2.5}$ To calculate (roughly) when the star will exit the main sequence. Would there be a way to include the expansion into a red giant? What about simulating the planetary nebula? Simplify as much as is needed.
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$\begingroup$ Now that there's an answer posted to address all aspects of this question, I don't think closing and preventing answer posts is necessary or even productive. voting to leave open $\endgroup$– uhohFeb 18 at 22:28
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Rough reaction for stars between 0.5 and 2.5 solar masses: We first need to know the initial(ZAMS) luminosity, the luminosity at the end of the main sequence(TAMS) and the MS lifetime: $$L_\text{ZAMS}=0.7×M^4$$
$$L_\text{TAMS}=3×L_\text{ZAMS}$$
$$T=9×M^{-2.6}\text{ (in Gyr)}$$
Reg giant stage: luminosity exponentially increases from the TAMS luminosity to about 3500×solar luminosity(at the tip of RGB) lasts about 10% of main sequence
Helium burning:luminosity exponentially increases from 50 to 150×solar luminosity, lasts about 100 Myr
AGB: luminosity increases exponentially from 150×solar luminosity to 10000×mass of star(in solar masses)×solar luminosity, lasts 20 Myr
Planetary nebula: roughly constant luminosity at 10000×mass of star(in solar masses)×solar luminosity, lasts roughly 30000yr
For other mass ranges it gets much more complicated.
Calculations: https://www.desmos.com/calculator/l2nelshpnx
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2$\begingroup$ Ive updated the formatting. In English don't use a dot to separate thousands, because the dot is used as a decimal point (ie 10.001 = 10001/1000, not ten thousand and one) What is the meaning of "L" and "M" in 150L to 10000M×solar luminosity? $\endgroup$– James KFeb 14 at 8:27
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