In this problem, we derive the mass luminosity relation. There are three equations to be looked at. According to the equation of radiation transport which talks about the energy carried by a photon, the luminosity Lis R LxT¹4 Next, using the condition of hydrostatic equilibrium, we can relate the pressure P inside a star with mass M and radius R as Px M² RA If we also assume that stellar matter behaves as an ideal gas, then Px pT where p x M/R³ is the density of matter inside the star. Using these equations, derive the mass luminosity relation L x M³. Note that this is only a crude analysis. Empirical data suggests that L x M3.5.

In this problem, we derive the mass luminosity relation. There are three equations to be looked at. According to the equation of radiation transport which talks about the energy carried by a photon, the luminosity Lis R LxT¹4 Next, using the condition of hydrostatic equilibrium, we can relate the pressure P inside a star with mass M and radius R as Px M² RA If we also assume that stellar matter behaves as an ideal gas, then Px pT where p x M/R³ is the density of matter inside the star. Using these equations, derive the mass luminosity relation L x M³. Note that this is only a crude analysis. Empirical data suggests that L x M3.5.

College Physics

11th Edition

ISBN:9781305952300

Author:Raymond A. Serway, Chris Vuille

Publisher:Raymond A. Serway, Chris Vuille

Chapter1: Units, Trigonometry. And Vectors

Section: Chapter Questions

Problem 1CQ: Estimate the order of magnitude of the length, in meters, of each of the following; (a) a mouse, (b)...

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