Table 1
Parameters used to model the synchrotron polarization data for an example bin in M 51 located in the innermost radial ring (2.4–3.6 kpc) at an azimuth centered on 100°.
| Disk | Halo | |
|
|
||
| Mode ratios | B2/B0 = (−33) / (−46) | Bh1/Bh0 = (76) / (23) |
| pm [ °] | p0 = −20, p2 = − 12 | ph0 = −43, ph1 = − 45 |
| βm [ °] | β2 = − 8 | βh1 = 44 |
|
|
||
| ne [cm-3] | 0.11 | 0.01 |
| ncr [cm-3]* | const. | const. |
| L [pc] | 800 | 5000 |
| d [pc]** | 40 | 240 |
| α | 2.0 | 1.5 |
Notes. The fitted model parameters appearing in the upper panel for the regular magnetic field of Eq. (26)are adopted from Fletcher et al. (2011) with central values reported only. The thermal electron density (ne) and path length (L) for the disk and halo are gathered from Fletcher et al. (2011) and Berkhuijsen et al. (1997).
The cosmic ray density is treated as a constant of proportionality between the
synchrotron emissivity and the square of the total transverse magnetic field
(μG)
as 
with constant
c =
0.1.
The turbulent cell size d in the disk and halo is obtained from Eq.
(27)with an RM dispersion
σRM,D fixed to
the observed value of 15
rad m-2 within a telescope beam of linear diameter
D =
600 pc. The rms value for the strength of the turbulent magnetic
field along the line of sight 
has
been assumed, where the value for 
is obtained
via consideration (6) with
in the disk and
in the halo.
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