  This paper is devoted to discuss the difference in the thermodynamic entropy
budget {\it per baryon} in each type of stellar object found in Universe. We
track and discuss the actual {\it decrease} of the stored baryonic
thermodynamic entropy from the most primitive molecular cloud up to the final
fate of matter in the black holes, passing through evolved states of matter as
found in white dwarfs and neutron stars. We then discuss the case of actual
stars of different masses throughout their {\it evolution}, clarifying the role
of virial equilibrium condition for the decrease of the entropy and related
issues. Finally, we discuss how gravity ultimately drives composition, hence
structural changes along the stellar evolution all the way until the ultimate
collapse to black holes, which may increase dramatically their entropy because
of the gravitational contribution itself.
