  We investigate to what extent the current helicity distribution observed in
solar active regions is compatible with solar dynamo models. We use an advanced
2D mean-field dynamo model with dynamo action largely concentrated near the
bottom of the convective zone, and dynamo saturation based on the evolution of
the magnetic helicity and algebraic quenching. For comparison, we also studied
a more basic 2D mean-field dynamo model with simple algebraic alpha quenching
only. Using these numerical models we obtain butterfly diagrams for both the
small-scale current helicity and the large-scale magnetic helicity, and compare
them with the butterfly diagram for the current helicity in active regions
obtained from observations. This comparison shows that the current helicity of
active regions, as estimated by $-A \cdot B$ evaluated at the depth from which
the active region arises, resembles the observational data much better than the
small-scale current helicity calculated directly from the helicity evolution
equation. Here $B$ and $A$ are respectively the dynamo generated mean magnetic
field and its vector potential.
