This preview has intentionally blurred sections. Sign up to view the full version.
View Full Document
Unformatted text preview: r from the central star? b) Now suppose the density, emission coe³cient and absorption coe³cient show the following scalings: ρ = ρ r2 j ν = j ρ 2 α n u = α ρ 2 ν2 These radiation coe³cients are approximately those for thermal emission at hν ¿ 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 φ 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...
View
Full Document
 Fall '08
 RABE
 Physics, Work, Fundamental physics concepts, isotropic distribution function, gas density scale, radio ﬂux measurements, spherically symmetric wind

Click to edit the document details