How will solar magnetism evolve in the future?

The solar magnetic field is generated and sustained through an internal dynamo. In stars, this process is determined by the combined action of turbulent convective motions and the differential rotation profile. It can sometimes lead to magnetic cyclic variabilities, like in the Sun with the 11 years cycle. Traces of magnetic cycles have been detected for other solar-like stars as well, ranging from a few years to a few tens of years. How are these cycles controlled? During their life, the rotation of stars is subject to complex evolution. Recent 3D numerical simulations of solar-like stars show that different regimes of differential rotation can be characterized with the Rossby number. In particular, anti-solar differential rotation (fast poles, slow equator) may exist for high Rossby number (slow rotators). If this regime occurs during the main sequence, and in general for slow rotators, we may wonder how the magnetic generation through dynamo process will be impacted, more especially if our Sun is in such a transition. In particular, can slowly rotating stars have magnetic cycles?
We present a numerical multi-D study with the STELEM and ASH codes to understand the magnetic field generation of solar-like stars under various differential rotation regimes, and focus on the existence of magnetic cycles.
We find that short cycles are favoured for small Rossby numbers (fast rotators), and long cycles for intermediate (solar-like) Rossby numbers. Slow rotators (high Rossby number) are found to produce only steady dynamo with no cyclic activity in most cases considered. Magnetic cycles can be produced with anti-solar differential rotation only if the alpha effect is fine tuned for this purpose.
A detection of magnetic cycles for such stars (or lack of thereof) would therefore be a tremendous constrain on deciphering what type of dynamo is actually acting in the Sun and solar-like stars. In addition, the future out-of-the-ecliptic observations of Solar Orbiter will give fantastic constraints on the magnetic field of the solar polar caps, and thus on which type of dynamo  (𝛼𝛺 vs Babcock-Leighton for instance) our Sun is the most likely to operate. Combined together, these will allow to better understand the physics in action in the complex present-day solar dynamo.