  Results of evolutionary modelling of subdwarf B stars are presented. For the
first time, we explore the core and near-core mixing in the subdwarf B stars
using new algorithms available in the MESA code: the predictive mixing scheme
and the convective premixing scheme. We show how both methods handle the
problems with determination of convective boundary, discrepancy between core
masses obtained from asteroseismology and evolutionary models, and
long-standing problems related to the core-helium-burning phase such as
splitting of the convective core and the occurrence of breathing pulses. We
find that the convective premixing scheme is the preferable algorithm. The
masses of the convective core in case of the predictive mixing and the combined
convective and semiconvective regions in case of the convective premixing
scheme are higher than in the models with only the Ledoux criterion, but they
are still lower than the seismic-derived values. Both algorithms are promising
and alternative methods of studying models of subdwarf B stars.
