  First-order phase transitions, like the liquid-gas transition, proceed via
formation of structures such as bubbles and droplets. In strongly interacting
compact star matter, at the crust-core transition, but also at the hadron-quark
transition in the core, these structures form different shapes dubbed "pasta
phases". We describe two methods to obtain one-parameter families of hybrid
equations of state (EoS) which mimic the thermodynamic behavior of pasta phases
in between a low-density hadron and a high-density quark matter phase, thus
generalizing the Maxwell construction. The first method replaces the behavior
of pressure vs. chemical potential in a finite region around the critical
%chemical potential pressure of the Maxwell construction by a polynomial
interpolation. The second method uses extrapolations of the hadronic and quark
matter EoS beyond the Maxwell point to define a mixing of both with weight
functions bounded by finite limits around the Maxwell point. We apply both
methods to the case of a hybrid EoS with a strong first order transition that
entails the formation of a third family of compact stars and the corresponding
mass twin phenomenon. We investigate for both models the robustness of this
phenomenon against variation of the single parameter, the pressure increment at
the critical chemical potential which quantifies the deviation from the Maxwell
construction. We also show sets of results for other compact star observables
than mass and radius, namely the moment of inertia and the baryon mass.
