Next: Polarization efficiency: size/shape/orientation effects Up: Optical properties of cosmic Previous: The 2175? feature . To model the interstellar polarization one needs to calculate the forward-transmitted radiation for an ensemble of non-spherical aligned dust grains. ... Let non-polarized stellar radiation passes through a dusty cloud with a homogeneous magnetic field. ... The angle between the line of sight and the magnetic field is ( ). ... where the angle is connected with and ( ). ...

Physics of Magnetic Stars, 2007, pp. 262-270 Line profile variability and the possible magnetic field in the spectra of supergiant Leo A.F. Kholtygin1 , G.A. Chountonov2 , S.N. Fabrika2 , T.E. Burlakova Kang Dong-il3 , G.A. Galazutdinov2,4 , M.V. Yushkin2 1 2 2,3 ... Astronomy and Space Science Institute, Optical Astronomy Division, 61-1, Whaam-Dong, YuseongGu, Daejeon, 305-348, Korea 1 Intro duction Line profiles in sp ectra of OB stars are usually strongly variable (Morel et al ...