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Using the Stefan-Boltzmann Law, best written as L = 4*pi*R^2*sigma*T^4

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. Using the Stefan-Boltzmann Law, best written as L = 4*pi*R^2*sigma*T^4,
calculate a star’s temperature if its luminosity is 4 x 1026watts and its radius is 7 x 108m.

-Stefan-Boltzmann Law: Energy emitted by a square meter on an object’s surface =×temperature4, whereis a constant of nature.

2. Use an ML relation of M^3.5.

What is the luminosity (in the solar units) of a three-solar-mass star? Round your answer to one decimal place.

 
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