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Unformatted text preview: r from the central star? b) Now suppose the density, emission coecient and absorption coecient show the following scalings: = r2 j = j 2 n u = 2 2 These radiation coecients are approximately those for thermal emission at h kT . Calculate the intensity for an arbitrary lineofsight, that means not only through the center. Hint: It is beneFcial to use the integration variable x = tan i the calculation of the optical depth. c) inally calculate the ux by integration over all possible linesofsight. Assume the distance D to the star is much larger than the size of the system, so you can replace the solidangle integration by one over the apparent surface. We are interested only in the spectral form. Can you reproduce the quietphase spectrum of the star mentioned in the research paper? 1994A&A. ..282. .547M...
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 Fall '08
 RABE
 Physics, Work

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