Description
The newly introduced Quantum Modified Inertia (QMI) framework is a relativistic theory of motion incorporating both upper and lower bounds on proper time. A mathematical consequence of these bounds is the emergence of corresponding upper and lower acceleration limits.
Focusing on the lower bound, a characteristic minimum acceleration naturally emerges from the analysis. Applied to galactic dynamics, the resulting modified-inertia model accounts for the rotation curves of systems such as the Milky Way (MW) and the dwarf galaxy DDO 52 while incorporating realistic baryonic contributions. Although the model differs significantly from MOND, it analytically recovers the radial acceleration relation and the baryonic Tully–Fisher relation, while remaining consistent with local Solar System constraints from the Cassini mission. These results suggest that bounding inertial dynamics can significantly reduce the need for cold dark matter, at least on galactic scales.
Building on this work, in collaboration with the UTINAM laboratory, we aim to refine in QMI the stellar mass-to-light ratio and the modelling of the MW rotation curve by accounting for several structural features of the Galaxy, including the thickness of the disk, the central bar, and the disk warp. The implications for celestial mechanics, as well as model-specific signatures that could enable the detection of the minimum-acceleration bound using metrological or interferometric techniques, will also be discussed.
Link to the original publication: https://rdcu.be/fuT30