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Gravity anomaly from laboratory experiments to astrophysics

Riccardo Scarpa, Renato Falomo, Aldo Treves

Abstract

Modifications to Newtonian dynamics at low accelerations have long been proposed as an alternative to dark matter to explain galaxy rotation curves. More recently, similar corrections have been invoked to interpret anomalies in Cavendish-type laboratory experiments and in the dynamics of wide binary stars, although the latter remain affected by ongoing observational debate. We show that, if deviations from Newtonian gravity occur in the low-acceleration regime, the available data are broadly consistent with a MOND-like interpretation. In this framework, wide binary systems appear to extend the Tully-Fisher relation, well established for galaxies, to much smaller mass scales. Taken together, departures from Newtonian predictions at low accelerations in galaxies, wide binaries, and laboratory experiments may point to a common physical scenario.

Gravity anomaly from laboratory experiments to astrophysics

Abstract

Modifications to Newtonian dynamics at low accelerations have long been proposed as an alternative to dark matter to explain galaxy rotation curves. More recently, similar corrections have been invoked to interpret anomalies in Cavendish-type laboratory experiments and in the dynamics of wide binary stars, although the latter remain affected by ongoing observational debate. We show that, if deviations from Newtonian gravity occur in the low-acceleration regime, the available data are broadly consistent with a MOND-like interpretation. In this framework, wide binary systems appear to extend the Tully-Fisher relation, well established for galaxies, to much smaller mass scales. Taken together, departures from Newtonian predictions at low accelerations in galaxies, wide binaries, and laboratory experiments may point to a common physical scenario.
Paper Structure (4 sections, 2 equations, 3 figures)

This paper contains 4 sections, 2 equations, 3 figures.

Table of Contents

  1. Introduction
  2. MOND basics
  3. Joining the Three Regimes
  4. Discussion and Conclusions

Figures (3)

  • Figure 1: Observed (black squares) versus Newtonian acceleration as derived from galaxy rotation curves from binned average of the data by Lelli17. The deviation from the Newtonian value (dashed black line) is clearly apparent. The red line is the Klein interpolation function. The blue diamonds represent the acceleration probed by wide binary systems from Chae24 (see text).
  • Figure 2: Observed $G$ boost, defined as $(a_{\rm obs}-a_{N})/a_{N}$ as a function of the Newtonian acceleration $a_N$. Points with error bars (1$\sigma$) are from galaxy rotation curves Lelli17. Filled squares with error bars are from the WBS analysis by Chae24. Note that value at acceleration $\sim 10^{-11}\ \mathrm{m\,s^{-2}}$ is a lower limit due to the selection of WBS (see text). The Klein function, calibrated on laboratory measurements (stars), describes galaxies, WBS, and laboratory data. The standard MOND interpolation function is also shown for comparison.
  • Figure 3: The baryonic Tully-Fisher relation for nearby spiral galaxies (filled circles) from the "accurate distance sample" of Lelli17, compared to the result for the wide binary stars (open square) from Hernandez23. The red line shows the MOND relation $V^4=Ga_0 M$ that describes remarkably very well both observations of galaxies and stars in spite of 10 order of magnitude difference in mass.