![]() | Annu. Rev. Astron. Astrophys. 1996. 34:
155-206 Copyright © 1996 by Annual Reviews. All rights reserved |
2.3. Small-Scale Field Structures
Any unresolved field structures will lead to beam depolarization and
thus to polarizations significantly below the theoretical
limit of P0
75%.
This effect is independent of wavelength and can be used
to estimate the spatial scale and strength of field irregularities
using observations at short wavelengths, where Faraday effects are weak.
At longer wavelengths, varying field orientations along the line of
sight give rise to dispersion in rotation measures (Faraday
dispersion), which also leads to depolarization
(Burn 1966).
Faraday dispersion is expected to arise from small
H II regions (of 1 pc
in size) in the thin galactic disk
(Ehle & Beck 1993)
as well as from larger scale fluctuations
(
10-100 pc) in the
diffuse ionized medium of the thick disk
(e.g. Krause 1993,
Neininger et al 1993).
This effect makes the Faraday rotation angle no longer proportional to
2 because
the effective Faraday depth decreases with increasing
. It was recently
discovered that at wavelengths
greater than or equal to 10 cm, galaxies are generally not
transparent topolarized radio waves
(Sukumar & Allen
1991,
Beck 1991,
Horellou et al 1992).
Even at
6 cm complete Faraday
depolarization may occur in spiral arms or in the plane of edge-on
galaxies.
To obtain full rotation measures, only observations in the
Faraday-thin regime (
6 cm) should be used
Vallée 1980,
Beck 1993).
Rotation measures between longer
wavelengths are lower and are weighted to regions near to the observer.
Variations in Faraday depth may also lead to
a spatial variation of the observed RM,
which complicates the interpretation of observations.
On the other hand, Faraday depolarization allows the
study of layers at different depths sampled at different wavelengths
(EM Berkhuijsen et al, in preparation).