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Flux tube emergence
Magnetic flux tubes formed at the base of the convective region should rise under Magnetic buoyancy. They rise at the Alfven speed, too rapidly to exchange angular momentum with their surroundings, and so conservation of angular momentum requires that they rise parallel to the rotation axis. The latitude at which they emerge depends on their initial distance from the rotation axis. i.e. the depth of the convective region.For the same rotation rate, stars with a deeper convective region should exhibit higher latitude spots.
Fully convective stars still exhibit flares and starspots, but this mechanism does not work for them.
Where do flux tubes emerge in fully convective stars?
For a given convective region depth, the latitude of emergence depends on whether buoyancy or Coriolis forces dominate.
$$\frac{F_{cor}}{F_{Buoy}} \approx \frac{2\rho u_A \omega}{(\rho_e-\rho_i)g} = \frac{2\rho u_A
\omega}{(p_e-p_i)\Lambda} = \frac{4 \mu u_A \omega \Lambda}{B_i^2} = \frac{4 \omega \Lambda}{u_A}$$
Coriolis forces will dominate and starspots will appear at greater latitudes if:
$$B < B_m \equiv 4(\mu \rho)^{1/2} \omega \Lambda$$ ( \(B \sim 10^5 G\) for our sun)