### Transition from axi- to nonaxisymmetric dynamo modes in spherical convection models of solar-like stars:

The associated paper can be found here https://arxiv.org/abs/1803.05898.

Visualization of the magnetic field from a rotating simulation.

### Effects of a subadiabatic layer on convection and dynamos in spherical wedge simulations:

The associated paper can be found here https://arxiv.org/abs/1803.05898.

Visualization of the flow from a rotating simulation MHD2 with Ω
= 3Ω_{⊙}. The streamlines are colour-coded by the
magnitude of the radial velocity *U*_{r}. The colour
contours at the periphery and on the planes at different depths show
the vertical velocity.

Same as above but for a non-rotating simulation HD2.

Visualization of the magnetic field from a rotating simulation MHD2
with Ω = 3Ω_{⊙}. The streamlines are
colour-coded by the magnitude of the azimuthal magnetic
field *B*_{φ}. The colour contours at the periphery
and on the planes at different depths show the azimuthal magnetic
field.

### Extended subadiabatic layer in overshooting convection:

Vertical velocity *U*_{z} and magnetic field
*B*_{z} near the surface (*z* = 0.98*d*),
resolution 1152^{3} grid points:

### Magnetic flux concentrations from turbulent stratified
convection:

See also the associated paper.

Vertical velocity *U*_{z} and magnetic field
*B*_{z} near the surface (*z* = 0.98*d*),
resolution 1024^{3} grid points:
(mp4, 561MB).

### Non-axisymmetric magnetic fields in a convective dynamo
simulation:

See also the associated paper.

Longitudinal magnetic field
*B*_{φ}
near the surface (*r* = 0.98*R*), Rm ≈ 28 (128
× 256 × 512 grid points):
(AVI, 30MB).

### Stratified convection with imposed horizontal magnetic field:

Vertical velocity *U*_{z} near the surface (*z* =
0.98*d*), Re ≈ 100 (1024 × 512 × 256 grid points):
(AVI, 11 MB).

Magnetic field component *B*_{y} near the surface
(*z* = 0.98*d*), Rm ≈ 5 (1024 × 512 × 256
grid points):
(AVI, 11 MB).

Magnetic field component *B*_{y} near the surface
(*z* = 0.98*d*), Rm ≈ 5 (1024 × 512 × 256
grid points):
(AVI, 15 MB).

Magnetic field component *B*_{y} averaged over the
*y* coordinate, Rm ≈ 5 (1024 × 512 × 256
grid points):
(AVI, 2 MB).

Magnetic field component *B*_{y} averaged over the
*y* coordinate, Rm ≈ 20 (1024 × 512 × 256
grid points):
(AVI, 2 MB).

### Cyclic magnetic activity due to turbulent convection in
spherical wedge geometry:

See also the associated paper.

Longitudinal magnetic field
*B*_{φ}
near the surface (*r* = 0.98*R*):
(AVI, 68MB).

### Effects of stratification in spherical shell convection:

See also the associated paper.

Vertical velocity *U*_{r} near the surface in
20 simulations

### Large-scale cyclones in rotating turbulent convection:

See also the associated paper.

Vertical velocity *U*_{z} in the prephery of the domain:
(AVI, 15MB),
Re ≈ 101, Co ≈ 7.5 (512^{2} × 256 grid points).

### Reynolds stress and heat transport in spherical shell convection:

See also the associated paper.

Snapshots of *U*_{r} near the surface from two runs:
±75 degrees latitude, 90 degrees longitude (here duplicated four-fold).

Intermediate rotation with anti-solar differential rotation, *U*_{r}:
(AVI, 8MB), Re ≈ 57, Co ≈ 1.3 (128 × 512
× 256 grid points).

Rapid rotation with solar like differential rotation, *U*_{r}:
(AVI, 5MB), Re ≈ 44, Co ≈ 6.9 (128 × 512
× 256 grid points).

### Convection with imposed field:

Imposed vertical field, *B*_{z}:
(AVI, 8MB), Re ≈ 45, Pm = 1 (256^{2} × 192 grid
points).

Imposed horizontal field, *B*_{x}:
(AVI, 6MB), Re ≈ 45, Pm = 1 (256^{2} × 192 grid
points).

### Magnetorotational instability driven dynamos at low magnetic Prandtl numbers:

See also the associated paper.

Velocity component *U*_{x}:
(AVI, 25MB), Re ≈ 8970, Pm = 0.1 (512^{3} grid points).

### Angular momentum transport in convectively unstable shear flows:

See also the associated paper.

Vertical velocity:
(Quicktime, 30MB), Re ≈ 648 (1024^{3} grid points)

### Convective dynamos in spherical wedge geometry:

See also the associated paper.

Vertical velocity *U*_{r} near the surface:
(Quicktime, 40MB),
(DivX, 3MB), Rm ≈ 45.

Azimuthal magnetic field component *B*_{φ} near the surface:
(Quicktime, 28MB),
(DivX, 3MB), Rm ≈ 45.

Azimuthally averaged magnetic field component *B*_{φ}:
(Quicktime, 20MB), Rm ≈ 30.

### Large-scale dynamos in rigidly rotating turbulent convection:

See also the associated paper.

Magnetic field component *B*_{x}:
Rm ≈ 90
(DivX 18MB) (512^{2} × 256 grid points).

Vertical velocity *U*_{z}:
Re ≈ 45
(DivX 16MB) (512^{2} × 256 grid points).

### Large-scale dynamos in turbulent convection with shear:

See also the associated paper.

Large-scale magnetic fields in turbulent convection with shear:
Rm ≈ 74 (DivX 26MB)
(256^{3} grid points),
Rm ≈ 121 (DivX 16MB)
(512^{3} grid points).

Vertical magnetic field at the top of the convectively unstable layer
in shearing convection
DivX
(35MB)

### Vorticity dynamo:

See also the associated paper.

Streamwise velocity component from a simulation of nonhelically forced
turbulence with shear (512^{3} grid points):
DivX
(7MB)

### Dynamo benchmark:

Quicktime movies:
Model B
Model C