Possible dynamical stabilization of relativistic supermassive stars by a shadow gravitational potential

It is shown that the repulsive shadow potential, introduced recently in theories of gravitation by Chiang, Dykla and Hwang, can stabilize, from a dynamical point of view, supermassive stars of mass M approximately less than or equal to 108 M/sub mass/. The value of the strength of this repulsive interaction necessary to ensure dynamical stability on the main sequence is found to be compatible with data concerning supermassive stars. For stars of mass higher than 108 M/sub mass/, a well developed space-time geometric theory of gravitation with shadow effect is necessary to come to a decision regarding their dynamical stability