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External fields in Migromian dynamics (MD or MOND, Milgrom 1983) break theStrong Equivalence Principle (SEP) and change the dynamics of self-boundstellar systems moving in space-varying background gravitational fields. Westudy two kinds of re-virialisation of the stellar systems: the violent phasetransition and the adiabatic phase transition for systems moving on radialorbits, where the external field evolves from strong to weak and whosecorresponding dynamics changes from Newtonian to Milgromian. We find that thetime scale for the phase tranformation from Newtonian to Milgromian gravitylies only within one to a few crossing times for low density globular clusterswith masses ranging from $10^4\msun$ to $10^6\msun$. Thus a globular clustercan appear frozen in the Newtonian regime despite being in the Milgromianregime for not longer than a few crossing times. We also study the kinematicsand anisotropy profiles of the systems. The velocity dispersions of the systemsare larger after the phase transitions, especially for the outer regions of thestellar systems. Moreover, the isotropic systems become radially anisotropic,especially for the outer parts, after the process caused by the dynamical phasetransition. Deeper Milgromian systems have more radially anisotropic velocitydispersion functions. We also find that the final profiles of density, velocitydispersion and anisotropy do not depend on the details of the phase transition.I.e., the mass distribution and kinematics of the end-states of the globularclusters do not depend on the rapidity of the transition from Newtonian toMilgromian gravity. Thus, the transition from the Newtonian to the Milgromianregime naturally induces a significant radially anisotropic velocitydistribution in a globular cluster.

The dynamical phase transitions of stellar systems and the corresponding kinetimacs