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Unformatted text preview: 9. Radiative transfer in moving media 9.1 Radiative transfer for spectral lines In the preceding chapters we have separately derived equations and techniques to describe the dynamical evolution of matter and the transport of radiation. In practise, the two are coupled problems, because the radiating medium may move with different velocities or in different directions in different parts of the emission region. The effect will be most prominent for spectral lines. In the following we will discuss the (easier) case of pure emission and absorption and neglect scattering. Lines have a natural minimal width with a profile called a Lorentzian that can be understood using classical physics. Emission corresponds to an energy loss for the emitter or to a damping of its state. Consider a damped harmonic oscillator, whose energy decrease with a time constant . Then the amplitude is x ( t ) = x exp( t ) exp( 2 t ) t (9 . 1) We derive the line profile by a FourierTransformation x ( ) = 1 2 integraldisplay  x ( t ) exp( t ) dt = x 2 1 2 + ( ) (9 . 2) and the spectral power as P ( )  x  2 = 1 2 x 2 parenleftBig 2 parenrightBig 2 + ( ) 2 (9 . 3) The line may be further broadened by the Doppler effect on account of the isotropic thermal motion of the emitters, described by a Gaussian, or on account of bulk motion. In some cases we may disentangle the effect of thermal motion and bulk motion. Suppose an observer, located at vectorr , sees line radiation from gas at vectorr . It is useful to introduce a path length coordinate along the lineofsight. vectorr = vectorr + vectore k s (9 . 4) At each location a line is emitted (and absorbed) with a width, that is determined by the thermal velocity of the emitters, v th , and a Doppler shift on account of the bulk flow with velocity vector V ....
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This note was uploaded on 02/29/2012 for the course PHYS 227 taught by Professor Rabe during the Fall '08 term at Rutgers.
 Fall '08
 RABE
 Physics, Radiation

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