In Energy-Momentum Squared Gravity, stellar equilibrium equations for perfect fluids retain the standard TOV form in effective variables and reduce to an autonomous planar dynamical system for linear equations of state.
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In quadratic-EMSG the self-acceleration of self-gravitating bodies vanishes at 1PN order and total linear momentum is conserved, consistent with binary-pulsar bounds.
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Covariant Tolman-Oppenheimer-Volkoff equations in Energy-Momentum Squared Gravity
In Energy-Momentum Squared Gravity, stellar equilibrium equations for perfect fluids retain the standard TOV form in effective variables and reduce to an autonomous planar dynamical system for linear equations of state.
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Dynamics of the $N$-body system in energy-momentum squared gravity: II. Existence of a Self-Acceleration
In quadratic-EMSG the self-acceleration of self-gravitating bodies vanishes at 1PN order and total linear momentum is conserved, consistent with binary-pulsar bounds.