# Can the Dynamo of Spiral-arm Galaxies Be Explained by Anisotropic Conductivity?

Paul Gomez, Franck Plunian, Thierry Alboussière

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## To cite this version:

Paul Gomez, Franck Plunian, Thierry Alboussière. Can the Dynamo of Spiral-arm Galaxies Be Explained by Anisotropic Conductivity?. The Astrophysical Journal, 2025, 981 (2), pp.164. 10.3847/1538-4357/adb1e2. hal-05396299

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Submitted on 3 Dec 2025

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Distributed under a Creative Commons Attribution 4.0 International License
Can the dynamo of spiral-arm galaxies be explained by anisotropic conductivity ?

PAUL GOMEZ,¹ FRANCK PLUNIAN,² AND THIERRY ALBOUSSIÈRE¹

¹ Université Lyon 1, ENS de Lyon, CNRS, Laboratoire de Géologie de Lyon, Lyon 69622, France; paul.gomez@univ-lyon1.fr, thierry.alboussiere@ens-lyon.fr

² Université Grenoble Alpes, University of Savoie Mont Blanc, CNRS, IRD, Université Gustave Eiffel, ISTERRE, 38000 Grenoble, France; franck.plunian@univ-grenoble-alpes.fr

ABSTRACT

The possibility of generating a magnetic field by dynamo effect with anisotropic electrical conduc-
tivity rather than turbulent flow has been demonstrated theoretically (Plunian & Alboussière 2020)
and experimentally (Alboussière et al. 2022). If the electrical conductivity is anisotropic, the electrical
currents will flow preferentially in certain directions rather than others, and a simple differential rota-
tion will suffice to generate a magnetic field. In a galaxy with spiral arms, it is reasonable to assume
that the electrical conductivity will be twice larger along the arms than in the perpendicular direction,
suggesting the possibility of an anisotropic dynamo. However, a further geometrical criterion must
be satisfied to obtain a dynamo (Plunian & Alboussière 2022). It is given by Ω' · sin p > 0, where
p is the pitch angle of the spiral arms, with p ∈ [-π/2, π/2], and Ω' is the radial shear of the angular
velocity. We find that the usual spiral arms galaxies, which satisfy |Ω'| < 0, do not satisfy this dynamo
condition because they have trailing arms instead of leading arms. Even the galaxy NGC 4622, which
has both trailing and leading arms, does not satisfy this dynamo condition either. This is confirmed
by numerical simulations of the induction equation. Thus, for all the spiral arms galaxies known to
date, the anisotropy of the spiral arms cannot explain the existence of galactic magnetic fields until
further notice.

Keywords: dynamo—anisotropy—spiral-arms galaxies—differential rotation

1. INTRODUCTION

Galactic magnetic fields have been observed for
decades, raising questions about their role in the for-
mation and behaviour of galaxies. They are composed
of a large-scale coherent part and a small-scale random
part due to turbulence. A typical time-scale for turbu-
lent magnetic diffusion in galaxies is 10⁸ years. This
corresponds to about one tenth of the age of a galaxy,
implying that a physical mechanism is needed to explain
why galactic magnetic fields are still present. Assuming
that a galaxy can be modelled by a rotating plasma,
the dynamo effect is a good candidate to explain the
generation of galactic magnetic fields (Brandenburg &
Subramanian 2005; Beck et al. 2019). Since the pio-
neering work of Krause & Rädler (1980), an alpha-effect
due to small-scale helical turbulence, conjugated to a
strong differential rotation, has been proposed as the
main dynamo mechanism.

The magnetic Reynolds number is defined by

$$
R_m = \sigma \mu U L, \tag{1}
$$

where σ is the electrical conductivity of the fluid, μ
its magnetic permeability, U and L two characteristic
values of velocity and length scale. This dimensionless
number can be understood as the ratio of the magnetic
diffusion time by the flow turn over time, implying that
a necessary condition for dynamo action is R_m > 1. In
galaxies R_m ≈ 10¹⁸ – 10²⁰ (Schekochihin et al. 2002;
Brandenburg & Subramanian 2005), much higher than
that required for dynamo action. However, a question
arises: is the dynamo still efficient at high R_m or, in
other words, is the dynamo of fast type (Childress &
Gilbert 2008). A fast dynamo corresponds to a strictly
positive kinematic growth rate of the magnetic field,
as opposed to a slow dynamo for which the magnetic
growth rate vanishes in the limit of a high R_m. The tur-
bulent alpha-effect is suspected to quench at high R_m
due to non-linear effects, challenging the usual dynamo
mechanism advocated to explain the galactic magnetic
field. (Rincon 2019).

Another possibility for generating a magnetic field by
dynamo effect has recently been proposed (Alboussière
et al. 2020; Plunian & Alboussière 2020). It is based on large-scale differential rotation and anisotropic electrical conductivity. Turbulence is not necessary for this dynamo mechanism to work. Assuming complete axisymmetry, it has been shown that an anisotropic dynamo can occur provided the differential rotation is higher than some threshold depending on the properties of the anisotropy (Plunian & Alboussière 2020). For an angular velocity with a smooth radial profile, an asymptotic approach has shown that the anisotropic dynamo is fast (Plunian & Alboussière 2022), then proving to be an interesting candidate for a galactic dynamo. The anisotropic dynamo action has also been demonstrated experimentally (Alboussière et al. 2022). Although the geometry of this experiment is different from that of a galaxy, they both share a logarithmic spiral anisotropy of electrical conductivity.

In this paper, we study the possibility for a spiral arms galaxy to work as an anisotropic dynamo. In section 2, the modeling of the anisotropic dynamo is explained. In section 3, some results of simulations are shown, for several rotation profiles and several arms configurations, trailing, leading arms or a combination of both.

## 2. MODELING

### 2.1. The pitch angle $p$

The shape of galactic spiral arms can be approximated by logarithmic spirals (Seigar & James 1998) with a constant pitch angle $p$, although in reality this can vary by a few degrees (Savchenko & Reshetnikov 2013). Following Davis et al. (2012), the absolute value of $p$ is defined as the smallest angle between the azimuthal direction and the tangential direction of the spiral, at a given radius. In addition, the sign of $p$ defines the chirality of the spiral. A clockwise outwards or anticlockwise inwards winding corresponds to $p > 0$, a clockwise inwards or anticlockwise outwards winding to $p < 0$, as illustrated in Fig.1.

Denoted by $q$, the unit vector normal to the spiral is defined by

$$q = \cos p \mathbf{e}_r + \sin p \mathbf{e}_\theta. \quad (2)$$

with $p \in [-\frac{\pi}{2}, \frac{\pi}{2}]$, and where $(\mathbf{e}_r, \mathbf{e}_\theta, \mathbf{e}_z)$ is the cylindrical coordinate system. Depending on the chirality and the pitch angle, the galaxies arms are either trailing arms or leading arms as illustrated in Fig. 1. A leading arm has its outer tip pointing in the direction of the galaxy's rotation, whereas the outer tip of a trailing arm points in the opposite direction of rotation.

### 2.2. Anisotropic electrical conductivity

In galaxies, the electron density is greater in the spiral arms than in the interarm regions by a factor two (Gutiérrez & Beckman 2010). However, the Spitzer resistivity does not depend on the electron density (Spitzer Jr & Härm 1953) and then cannot lead to an anisotropic electrical conductivity. A candidate for such anisotropy can be the different abundance of HII regions within the spiral arm and inter-arm regions (Knapen 1998). Another option could be to rely on the turbulent diffusivity which is most effective in the spiral arms.

<figure><img src="image_3.png" /><figcaption>**Figure 1.** Examples of leading and trailing arms, with positive or negative pitch angles $p$. In (a) and (b) the galaxy rotates clockwise. In (d) and (c) the galaxy rotates counterclockwise.</figcaption></figure>

We define an anisotropic effective electrical conductivity as a tensor (Ruderman & Ruzmaikin 1984),

$$[\sigma_{ij}] = \sigma_{\perp} \delta_{ij} + (\sigma_{\parallel} - \sigma_{\perp}) q_i q_j, \quad (3)$$

where $\sigma_{\parallel}$ and $\sigma_{\perp}$ are the electric conductivity in the directions parallel and perpendicular to $q$. We do not have an estimate for the ratio $\sigma_{\perp}/\sigma_{\parallel}$, but the key point is that it must be strictly larger than unity. For the numerical applications, we choose $\sigma_{\perp}/\sigma_{\parallel} = 2$.

We note that the conductivity model given by (3) implies that the conductivity is axisymmetric, which is obviously not the case, since the spiral arms break this axisymmetry. It is, however, the simplest and probably the most dynamo capable model we can think of,
for studying the possibility of an anisotropic dynamo in galaxies.

### 2.3. Induction equation

The induction equation can be written as

$$ \partial_t \mathbf{B} = \nabla \times (\mathbf{U} \times \mathbf{B}) - \mu_0^{-1} \nabla \times ([\sigma_{ij}]^{-1} \nabla \times \mathbf{B}), \quad (4) $$

where $\mathbf{B}(r,t)$ is the magnetic induction, $\mathbf{U} = U(r)e_\theta$, and $\mu_0$ the vacuum magnetic permeability.

Since the velocity is stationary, and assuming axisymmetry, we look for a magnetic induction in the form

$$ \mathbf{B} = \mathbf{B}(r, z) \exp(\gamma t), \quad (5) $$

leading to the resolution of a 2D eigenvalue problem. In (5), $\gamma > 0$ is the signature of dynamo action, the dynamo threshold corresponding to $\gamma = 0$.

### 2.4. A necessary condition for dynamo action

In Plunian & Alboussière (2022), an asymptotic expression of the magnetic growthrate $\gamma$ for $R_m \gg 1$ and $\sigma_\perp \gg \sigma_\parallel$, has been derived,

$$ \gamma \approx r_0 \cdot \Omega'(r_0) \cdot \cos p \cdot \sin p - K^2, \quad (6) $$

where $\Omega'(r)$ is the radial derivative of the angular velocity $\Omega(r) = U(r)/r$, $K$ a dimensionless number, and $r_0$ a value of $r$ at which the asymptotic expansion leading to (6) has been made.

For $p \in [-\pi/2, \pi/2]$, a necessary condition for anisotropic dynamo action is therefore that there must be at least one value of $r$ such that

$$ \Omega' \cdot \sin p > 0. \quad (7) $$

Then, applying (7) to cases (a-d), and depending whether the absolute value of the angular velocity $|\Omega|$ is decreasing ($|\Omega'| < 0$) or increasing ($|\Omega'| > 0$), the sign of $\Omega' \cdot \sin p$ can be determined (see Tab.1). We find that if $|\Omega(r)|$ decreases (respectively increases), the dynamo is only possible in cases (b) and (d) (respectively in cases (a) and (c)).

### 2.5. Application to usual spiral arms galaxies

The central part of a galaxy, called the bulge, is made of a high concentration of stars. In the vast majority of spiral arms galaxies observed so far, the azimuthal velocity $U(r)$ is a solid body rotation within the bulge, and flat outside the bulge (Rubin et al. 1982; Sofue & Rubin 2001). This corresponds to an angular velocity $\Omega(r)$ which is constant within the bulge and whose absolute

<table><caption>**Table 1.** Sign of $\Omega' \cdot \sin p$ for the cases (a-d) depicted in Fig. 1.</caption><thead><tr><th></th><th>Ω</th><th>p</th><th>|Ω'|</th><th>Ω'</th><th>Ω' · sin p</th></tr></thead><tbody><tr><td>Trailing (a)</td><td>-</td><td>-</td><td>+</td><td>-</td><td>+</td></tr><tr><td>Leading (b)</td><td>-</td><td>+</td><td>-</td><td>+</td><td>-</td></tr><tr><td>Trailing (c)</td><td>+</td><td>+</td><td>-</td><td>+</td><td>+</td></tr><tr><td>Leading (d)</td><td>+</td><td>-</td><td>-</td><td>-</td><td>+</td></tr></tbody></table>

<figure><img src="image_4.png" /></figure>

<figure><img src="image_5.png" /><figcaption>**Figure 2.** (a) Left: Illustration of the trailing and leading arms of the NGC 4622 galaxy. (b) Right: The black dots and red triangles correspond to observations of the azimuthal velocity $U(r)$ by respectively Buta et al. (2003) and Byrd & Howard (2019). The full curve is a fit of the red triangles, corresponding to $U(r)$, and the dashed curve to $\Omega(r) = U(r)/r$.</figcaption></figure>

value decreases outside, corresponding to $|\Omega'| \le 0$. From Tab.1, only the cases (b) and (d) are likely to behave as anisotropic dynamos. They both correspond to a leading arms geometry (Fig.1). However, all galaxies observed so far have trailing arms (Pasha & Smirnov 1982), so they are unlikely to be the seat of an anisotropic dynamo.

### 2.6. NGC 4622: an unusual spiral arms galaxy

The spiral arms galaxy NGC 4622 possesses one trailing arm surrounded by two leading arms (Byrd & Howard 2019), as illustrated in Fig. 2a. The trailing arm corresponds to case (a), and the two leading arms to case (b). In addition, according to Fig. 2b, the azimuthal velocity is flat for the trailing arm ($|\Omega'| < 0$) and increasing in absolute value for the leading arms ($|\Omega'| > 0$), leading in both cases to $\Omega' \cdot \sin p < 0$. Once again, it is therefore unlikely that the galaxy NGC 4622 is the seat of an anisotropic dynamo.

## 3. NUMERICAL SIMULATIONS
In order to verify the theoretical conclusions of sections 2.5 and 2.6, we now carry out numerical simulations.

### 3.1. Velocity profiles

The geometry of a spiral-arm galaxy is approximated by a cylinder of height $h$ and radius $R \gg h$. The radius of the galactic bulge is denoted $r_b$. Most spiral arms galaxies have dimensions $r_b \sim h \approx 0.2$ to $2$ kpc and $R \approx 10$ to $50$ kpc (Mollá et al. 2000; Möllenhoff 2004; Zhao et al. 2004). In the simulations we take $r_b = h$ and $R/r_b = 50$. For the NGC 4622 galaxy, according to Buta et al. (2003), $r_b \approx 8.8$ arcsec, $R \approx 52$ arcsec, and $h \sim 1.93$ arcsec (5 kpc = 29.7 arcsec). In the simulations we take $R/h = 27$ and $r_b/h = 4.6$.

We consider four azimuthal velocity profiles, $U_K$, $U_F$, $U_S$ and $U_{4622}$. The first two, $U_K$ and $U_F$, correspond to a velocity profile which is a solid body rotation within the bulge, and respectively Keplerian or flat outside the bulge. The last two, $U_S$ and $U_{4622}$, are smooth functions of $r$ closed to solid rotation for $r \ll r_b$, and (i) asymptotically flat in the limit $r \gg 1$ for $U_S$, (ii) corresponding to the observations of NGC 4622 given by the red triangles in Fig. 2b for $U_{4622}$.

They are given by

$$U_K(r) = \begin{cases} U_0 r/r_b & \text{for } 0 \le r \le r_b \\ U_0 \sqrt{r_b/r} & \text{for } r_b \le r \le R \end{cases}, \quad (8)$$

$$U_F(r) = \begin{cases} U_0 r/r_b & \text{for } 0 \le r \le r_b \\ U_0 & \text{for } r_b \le r \le R \end{cases}, \quad (9)$$

$$U_S(r) = U_0 \tanh\left(\frac{ar}{r_b}\right) \quad \text{for } 0 \le r \le R, \quad (10)$$

$$U_{4622}(r) = U_0 (br + cr^2 + dr^3 + er^4) \quad \text{for } 0 \le r \le R. \quad (11)$$

In (10), we set $U_S(r_b) = U_0$, implying that $a = 3.8$. The parameters $r_b$ and $U_0$ are the characteristic scale and velocity by which the induction equation (4) is normalized, the problem then depending only on the magnetic Reynolds number

$$R_m = \sigma_{\perp} \mu_0 U_0 r_b, \quad (12)$$

where $\mu_0$ is the magnetic permeability of void. As an example, shown in Fig. 3a, taking $U_0 = 233$ km s$^{-1}$ and $r_b = 1$ kpc in (9) and (10) leads to a reasonable approximation of the velocity profile measured in NGC 7331 (Begeman 2006). The corresponding angular velocity $\Omega(r) = U(r)/r$ is given in Fig. 3b. Although not represented, the value of $\Omega_S$ at $r = 0$ is equal to 885.4 km s$^{-1}$ kpc$^{-1}$.

In (11), the coefficients $b, c, d, e$ are derived from a 4th order polynomial regression in order to fit the data

<figure><img src="image_6.png" /><figcaption>**Figure 3.** (a) Top: Azimuthal velocity $U(r)$. (b) Bottom: Angular velocity $\Omega(r) = U(r)/r$. They are given for the three profiles Keplerian (K), Flat (F) and Smooth (S), and from observations of the galaxy NGC 7331 (Begeman 2006). For $r \ge 1$, the Flat and Smooth curves coincide.</figcaption></figure>

by Byrd & Howard (2019) given by the red triangles in Fig. 2b. They are given by $b = 7.523 \times 10^{-2}$ arcsec$^{-1}$, $c = -4.896 \times 10^{-3}$ arcsec$^{-2}$, $d = 1.244 \times 10^{-4}$ arcsec$^{-3}$, and $e = -9.805 \times 10^{-7}$ arcsec$^{-4}$. In Fig. 2b, the full curve corresponds to $U(r)$ given by (11) with $U_0 = 330$ km s$^{-1}$, and the dashed curve to $\Omega(r) = U(r)/r$. We note that $\Omega' = 0$ for $r \approx 30$ arcsec (Byrd & Howard 2019).

### 3.2. Values taken for the pitch angle

According to Buta et al. (1992), in the galaxy NGC 4622, the pitch angle is $p = -3.8^{\circ}$ (respectively $p = 7.5^{\circ}$) for the part corresponding to the trailing arm (respectively leading arms). For the other spiral arms galaxies the pitch angle varies between $10^{\circ}$ to $50^{\circ}$ (Seigar et al. 2006), and we take the mean value $p = 28^{\circ}$.

### 3.3. Poloidal-Toroidal decomposition

The simulations are performed using Freefem++, a partial differential equation solver that employs the finite element method (Hecht 2012). We use a poloidal-toroidal decomposition of $B$,

$$B = \nabla \times (P(r, z)e_{\theta}) + T(r, z)e_{\phi}, \quad (13)$$

such that the solenoidality condition $\nabla \cdot B = 0$ is necessarily satisfied.

The problem is axisymmetric. In the $(r, z)$-plane the galaxy is modeled by a rectangle of dimensions $h \times R$, and the computational domain is a semi-disc of radius
<figure><img src="image_7.png" /><figcaption>**Figure 4.** (a) Left: Meshing domain for numerical simulations. (b) Right: Isovalues of the poloidal and toroidal components of the magnetic field for Smooth, Keplerian and Flat azimuthal velocity profiles at different $R_m$. The axis of rotation is represented by the vertical black line. The radial limit of the bulge is represented by the vertical red line. The conducting domain lies between the two horizontal orange lines. Increasing $R_m$ we see that the magnetic mode evolves from quadrupolar (left), octopolar (middle), and to a higher mode (right).</figcaption></figure>

$R'$ (see Fig. 4a). The electrical conductivity tensor is defined by (3) in the rectangle, and zero elsewhere. The corresponding boundary conditions are

$$T(r=0) = P(r=0) = T(z = \pm \frac{h}{2}, r \le R) = 0, \quad (14)$$

the last condition insuring that at the border of the conducting domain, the normal component of the current density vanishes. For $\rho = R'$ with $\rho = \sqrt{r^2 + z^2}$, we impose

$$T(\rho = R') = \left(\frac{\partial P}{\partial r} - \frac{P}{R'}\right) (r = R') = 0, \quad (15)$$

meaning that the magnetic field matches with a dipolar magnetic field at the limit of the computational domain $\rho = R'$.

### 3.4. Growth rates

In Fig. 5, the magnetic growthrate $\gamma$ is plotted versus $R_m$ for each velocity profiles (8-11). As predicted in sections 2.5 and 2.6, dynamo ($\gamma > 0$) is only possible if we replace $U_S$, $U_K$, $U_F$ and $U_{4622}$ by their opposites (or if we replace the pitch angle by its opposite). For $U_S$, $U_K$, $U_F$ it means that only the leading arms configuration can lead to dynamo action. For $U_{4622}$, only the configuration with a leading arm surrounded by trailing arms can lead to a dynamo. Increasing the value of

<figure><img src="image_8.png" /></figure>

<figure><img src="image_9.png" /><figcaption>**Figure 5.** (a) Top: Growth rate $\gamma$ versus $R_m$ for $U_K$, $U_F$, $U_S$ (dashed curves) and $-U_K$, $-U_F$, $-U_S$ (solid curves). (b) Bottom: Growth rate $\gamma$ versus $R_m$ for $U_{4622}$ (dashed curve) and $-U_{4622}$ (solid curves). In the inset, the isovalues of the poloidal component of the magnetic field are plotted for $R_m = 3176$.</figcaption></figure>

$\sigma_{\perp}/\sigma_{\parallel}$ does not change this qualitative conclusion (as illustrated in Fig. 6 of Appendix for $U = U_S$).

From Fig. 5, we note that the dynamo threshold $R_m^c$, above which $\gamma > 0$, is much higher for $-U_{4622}$ ($R_m^c = 3176$) than for $-U_S$, $-U_K$ and $-U_F$ ($R_m^c = 106, 120$ and $142$). Also the value of $\gamma$ is smaller by about two orders of magnitude, for $-U_{4622}$. This agrees well with (6) as, for NGC 4622, $p$ and $\Omega'$ are about 10 times smaller than in the three other cases.

For $-U_S$, $-U_K$ and $-U_F$ there are magnetic mode transitions, from quadrupolar to octopolar at $R_m = 359, 510$ and $680$ respectively, and from octopolar to a higher degree at $R_m = 901, 1295$ and $1763$ respectively. For $-U_{4622}$, the magnetic eigenmode is quadripolar and generated in the outer part of the conducting domain, corresponding to the leading arms (Fig. 5b). A 3D
representation of the magnetic field lines is shown in Appendix (Fig. 8) for $U = -U_S$ and $U = -U_{4622}$.

### 3.5. Characteristic time

In the high-$R_m$ limit, and in all four cases $-U_S, -U_K, -U_F$ and $-U_{4622}$, the growthrate does not decrease toward zero, which is the signature of fast dynamo action (Fig. 5). As shown in Plunian & Alboussière (2022), the dynamo takes place (i) at a characteristic radius where the shear is maximum, located here at $r \sim r_b$, and (ii) with a characteristic time which is the turnover time at that scale, here $\tau \sim |\Omega(r_b)^{-1}|$. With a characteristic velocity $U \sim 10^2$ km s$^{-1}$ (Persic et al. 1996) and a characteristic bulge's radius $r_b \sim 1-10$ kpc, we find that spiral-arm galaxies have a characteristic turnover time $\tau \sim 10^7 - 10^8$ years which is a fraction of spiral-arm galaxy's age.

### 3.6. Characteristic scale

We note that the larger the $\Omega$, the smaller the vertical magnetic structures (Fig. 4), in agreement with the fast dynamo model of Plunian & Alboussière (2022). The characteristic scale of magnetic structures is of order $R_m^{-1/2}r_b$. At this scale the magnetic diffusion time is equal to the turnover time.

## 4. CONCLUSION

In this paper, we studied the question of whether a dynamo effect in a spiral-arm galaxy can be a simple consequence of the existence of its spiral arms. The answer could be yes, provided the arms would be leading and not trailing as usually observed in galaxies, or provided the shear would increase with $r$ ($|\Omega'| > 0$), which is usually also not observed in galaxies. Having both leading arms and an increasing shear with $r$ would not lead to dynamo either. Therefore, based on current observations,

we do not find any possibility to have a galactic magnetic field generated only by a simple differential rotation, without requiring an effect of turbulence e.g. an alpha-effect. This does not mean that the geometry of the arms plays no role. In fact, it remains true that electric currents flow preferentially along the spiral arms of the galaxy, corresponding to an anisotropic electrical conductivity effect. Therefore a complete model of a galactic dynamo should include at least the three effects: differential rotation, effect of turbulence like an alpha-effect, and an anisotropic effect. We can also think of large-scale fluctuations in azimuthal velocity, so that the sign of $\Omega'$ is modified at certain points. It would then be possible for the anisotropic dynamo to take hold. In NGC 4622, the sign of $\Omega'$ is indeed changed at $r = 30$ arcsec. However, it is accompanied by the transformation of the trailing arms into leading arms, which again rules out the possibility of an anisotropic dynamo. From these observations, we can suggest that the anisotropic dynamo effect induced by shear leads to a selection principle: if the condition (7) applied, then the fast dynamo would produce a strong magnetic field, inducing strong Lorentz forces that would reorganize the differential rotation and/or pitch angle until condition (7) is no longer satisfied. This remains to be demonstrated in more detailed dynamical numerical simulations.

## ACKNOWLEDGEMENT

1 We acknowledge the support of the Programme et Équipements Prioritaire pour la Recherche (PEPR Origins) for its financial support. Numerical simulations were carried out using Freefem++ (Hecht 2012) and 3D modelling was done using Paraview software (Ahrens et al. 2005).

2

3

4

5

6

## APPENDIX

In Fig. 6a, the growthrate is plotted versus $R_m$ for $U = -U_S$ and several values of $\sigma_{\perp}/\sigma_{\parallel} > 1$. In Fig. 6b, the critical magnetic Reynold number is plotted versus $\sigma_{\perp}/\sigma_{\parallel}$.

The magnetic pitch angle $p_B$, is defined by

$$p_B = \arctan \left( \frac{B_r}{B_{\theta}} \right). \qquad (1)$$

In Fig. 7a, the radially averaged magnetic pitch angle $\bar{p}_B$ is plotted versus $Rm$, for $U = -U_K, -U_S, -U_F$, and $\sigma_{\perp}/\sigma_{\parallel} = 10^6$. In the limit of large $Rm$, $\bar{p}_B$ approaches asymptotically the motion pitch angle $p$, as already observed in spiral-arms galaxies (Van Eck et al. 2015; Beck 2016). In Fig. 7b, for $U = -U_S$ and $R_m = 200$, the magnetic pitch angle $p_B$ is plotted versus $r$ for different values of $\sigma_{\perp}/\sigma_{\parallel}$.

In Fig. 8, a 3D representation of the magnetic field is plotted for (a) $U = -U_S$ (respectively (b) $U = -U_{4622}$) and $R_m = 350$ (respectively $R_m = 3180$).
<figure><img src="image_10.png" /><figcaption>**Figure 6.** For $U = -U_S$ and different values of $\sigma_{\perp}/\sigma_{\|}$, (a) Left: the growth rate is plotted versus $R_m$. (b) Right: The critical $R_m$ above which dynamo occurs, is plotted versus $\sigma_{\perp}/\sigma_{\|}$.</figcaption></figure>

<figure><img src="image_11.png" /><figcaption>**Figure 7.** (a) Left: The radial mean of the magnetic pitch angle $\bar{p}_B$ is plotted versus $Rm$, for $U = -U_K, -U_S, -U_F$, and $\sigma_{\perp}/\sigma_{\|} = 10^6$. (b) Right: For $U = -U_S$ and $R_m = 200$, the magnetic pitch angle $p_B$ is plotted versus $r$ for different values of $\sigma_{\perp}/\sigma_{\|}$.</figcaption></figure>

<figure><img src="image_12.png" /><figcaption>**Figure 8.** A 3D representation of the magnetic field lines for (a) Left: $U = -U_S$ and $R_m = 350$, (b) Right: $U = -U_{4622}$ and $R_m = 3180$. The green and blue colors correspond to opposite signs of $B_z$. The red lines are perpendicular to $q$, so in the direction of the spiral arms, assuming axisymmetry. In both figures, the outer grey circular ribbon marks the radial edge of the conducting domain. In the right figure, the inner grey circular ribbons marks the transition between the leading and trailing arms.</figcaption></figure>
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