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Table 2

Simulation parameters and results.

Model Dim MF NS Halo M gas Seed Parity p in p out τ e Comments
[1010 M⊙] [  °  ] [  °  ] [Gyr] [μG]
X1s-0.5 2D • ° ° 0.57 WN S0/A0 −11.6 −4.7 0.374 1.44 see Fig. 3
X1s 2D • ° ° 1.14 WN S0a −11.0 −4.6 0.503 3.75 see Figs. 4, 5
X1s-1.5 2D • ° ° 1.70 WN S0a −10.8 −4.6 0.547 6.34
X1s-2.0 2D • ° ° 2.27 WN S0 −10.7 −4.3 0.593 9.07
X2s-halo 2D • ° • 1.14 WN S0a −11.7 −4.8 0.358 4.05
X3s-VF 2D • ° ° 1.14 VF A0→S0 −11.0 −4.5 0.539 3.75
N1s/d-HF 3D • ° ° 1.14 HF S0 −11.0 −3.2 – 3.75
3D • • ° 1.14 S0 −9.9 −2.6 – 2.52
N1s/d-VF 3D • ° ° 1.14 VF, S0 −11.0 −6.1 0.409 3.75
3D • • ° 1.14 S0 −9.9 −2.7 0.407 2.65 see Fig. 12
N2d-noD 3D °b • ° 1.14 HF+VF A0 −1.7 −1.6 – 0.82c see Fig. 7
N2d-MRI 3D ° • ° 1.14 HF+VF A0 −0.4 −0.5 – 4.25 see Fig. 7
N3d-VF 3D • • ° 1.14 VF S0/A0 −10.2 −3.4 – 3.46 see Figs. 7, 9,  10

Notes. All 2D runs are axisymmetric; mean-field (MF) effects include those described in Sect. 2.2; runs including “NS” evolve the Navier-Stokes equation. The “halo” dynamo is shown as a dashed line in Fig. 2. The column labelled Mgas gives the normalisation for the disc mass. For seed fields we used white noise (WN) with 0.15 nG rms amplitude, net-vertical field (VF) of 0.1 nG, or net-horizontal field (HF) of 0.01 μG. Pitch angles are given for the inner disc (i.e., where the magnetic field strength peaks) and for the outer disc (average for R > 10 kpc) separately. Growth rates are for the magnetic field during an interval for which exponential growth can be identified.

(a)

Subdominant A0 outside R ≃ 10 kpc;

(b)

includes ηt, and νt;

(c)

obtained outside R ≃ 15 kpc.

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