Static trace free Einstein equations and stellar distributions

We construct models of static spherical distributions of the perfect fluid in trace free Einstein gravity theory. The equations governing the gravitational field are equivalent to standard Einstein's equations; however, their presentation is manifestly different, which motivates the question whether new information would emerge due to the nonlinearity of the field equations. The incompressible fluid assumption does not lead to the well known Schwarzschild interior metric of Einstein gravity, and a term denoting the presence of a cosmological constant is present on account of the integration process. The Schwarzschild interior is regained as a special case of a richer geometry. On the other hand, when the Schwarzschild geometry is prescribed, a constant density fluid emerges consistent with the standard equations. A complete model of an isothermal fluid sphere with pressure and density obeying the inverse square law is obtained. Corrections to the model previously presented in the literature by Saslaw et al. are exhibited. The isothermal ansatz does not yield a constant gravitational potential in general, but both potentials are position dependent. Conversely, it is shown that assuming a constant g_{r r} gravitational potential does not yield an isothermal fluid in general as is the case in standard general relativity. The results of the standard Einstein equations are special cases of the models reported here. Noteworthy is the fact that whereas the previously reported isothermal solution was only of cosmological interest, the solution reported herein admits compact objects by virtue of the fact that a pressure free hypersurface exists. Finally we analyze the consequences of selecting the Finch-Skea metric as the seed solution. The density profiles match; however, there is a deviation between the pressure profiles with the Einstein case although the qualitative behavior is the same. It is shown in detail that the model satisfies elementary requirements for physical plausibility such as a positive density and pressure, existence of a hypersurface of vanishing pressure, a subluminal sound speed, satisfaction of the weak, strong, and dominant energy conditions, as well as the Buchdahl mass-radius compactness requirement.