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tokens: component to the width. Dynamical studies of galaxies typically use Newton’s gravity. However, it has been argued that once galactic masses are considered, relativistic effects arising from large masses (rather than large velocities) may become important (Deur 2009 , 2017 , 2019 ). Their physical origin is that in general relativity (GR), gravity fields self-interact. In this article, we explore whether these effects can explain the relation in MLS2016 without requiring dark matter or modifying gravitation as we currently know it. The article is organized as follows. We first outline the self-interaction effects in GR, then discuss in Section 3 the empirical tight dependence of observed acceleration on baryonic mass in disk (i.e., lenticular and spiral) galaxies. In Section 4 , we use GR’s equations to compute the correlation. These CPU-intensive calculations allow us to study only a few galaxies, modeled as bulgeless disks. To cover the full range of disk galaxy morphologies, including those with a significant bulge, in Section 5 we develop two dynamical models of disk galaxies in different but complementary ways: uniform sampling (Section 5.1 ) and random sampling (Section 5.2 ) of the galactic parameter space. In Section 6 we show the results from these models and compare them to observations. Finally, in Section 7 , we summarize our findings and their importance. 2. Self-interaction Effects in GR Field self-interaction makes GR nonlinear. The phenomenon is neglected when Newton’s law of gravity is used, as is typically done in dynamical studies of galaxies or galaxy clusters. However, such a phenomenon becomes significant once the masses involved are large enough. Furthermore, it is not suppressed by low velocity—unlike some of the more familiar relativistic effects—as revealed by, e.g., the inspection of the post-Newtonian equations (Einstein et al. 1938 ). In fact, the same phenomenon exists for the strong nuclear interaction and is especially prominent for slow-moving quark systems (heavy hadrons), in which case, it produces the well-known quark confining linear potential. The connection between self-interaction and nonlinearities is seen, e.g., by using the polynomial form of the Einstein–Hilbert Lagrangian (see, e.g., Salam 1974 ; Zee 2013 ),where g μν is the metric, R μν is the Ricci tensor, T μν is the energy-momentum tensor, M is the system mass, and G is the gravitational constant. In the natural units () used throughout this article, . The polynomial is obtained by expanding g μν around a constant metric η μν of choice, with the gravitational field. The brackets are shorthand for sums over Lorentz-invariant terms (Deur 2017 ). For example, the n = 0 term is explicitly given by the Fierz–Pauli Lagrangian (Fierz Pauli 1939 ):While Equation ( 1 ) is often used to study quantum gravity—with questions raised regarding its applicability in that context, see, e.g., Padmanabhan ( 2008 )—we stress that the calculations and results