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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: = r-2 j = j 2 n u = 2 -2 These radiation coecients are approximately those for thermal emission at h kT . Calcu-late the intensity for an arbitrary line-of-sight, 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 lines-of-sight. Assume the distance D to the star is much larger than the size of the system, so you can replace the solid-angle integration by one over the apparent surface. We are interested only in the spectral form. Can you reproduce the quiet-phase spectrum of the star mentioned in the research paper? 1994A&A. ..282. .547M...
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