Recent neutron star observations combined with the nuclear constraints suggest that QCD matter quickly stiffens at density close to nuclear matter density. We argue that the stiffening is triggered by a transition from nuclear to quark matter. The concept of quarkyonic matter captures relevant features necessary to understand the stiffening. We present an ideal model of quarkyonic matter and apply it to isospin symmetric and a matter of neutral baryons including the strangeness. We argue how the quark description mitigates the hyperon problems in neutron star constraints.