  In this work, we study the effects that interacting quark matter has on the
stellar structure of strange and charm quark stars. Additionally, their
stability against radial pulsations is analyzed using a first-order formalism
for adiabatic general relativistic oscillations. Besides, the early stage of
stellar evolution of neutron stars after the supernovae explosion, i.e.
protoneutron stars, is investigated by considering the possibility of a
first-order phase transition to quark matter rich in leptons, where the
dynamics of conversion between phases is studied within a thermal nucleation
model. For each kind of compact star mentioned we use for the quark phase the
equation of state calculated within cold perturbative QCD (pQCD), parametrized
only by its renormalization scale. We note that the original pQCD framework is
manipulated appropriately to include neutrinos and extended to add heavy quarks
to the original system composed only by up, down and strange quark flavors.
