  We study the hadron-quark phase transition in the interior of neutron stars.
For the hadronic sector, we use a microscopic equation of state involving
nucleons and hyperons derived within the Brueckner-Hartree-Fock many-body
theory with realistic two-body and three-body forces. For the description of
quark matter, we employ the Dyson-Schwinger approach and compare with the MIT
bag model. We calculate the structure of neutron star interiors comprising both
phases and find that with the Dyson-Schwinger model, the hadron-quark phase
transition takes place only when hyperons are excluded, and that a
two-solar-mass hybrid star is possible only if the nucleonic equation of state
is stiff enough.
