Limits on a Gravitational Field Dependence of the Proton--Electron Mass Ratio from H$_2$ in White Dwarf Stars

TL;DR

This study uses H$_2$ spectra from white dwarf stars to test if the proton-electron mass ratio varies with gravity, finding no significant dependence within current measurement uncertainties.

Contribution

It provides the first constraints on proton-electron mass ratio variation in strong gravitational fields using white dwarf spectra.

Findings

No significant $/$ variation detected.

Constraints are $/ = (-2.7 1 4.7_{ m stat} 1 0.2_{ m sys}) imes 10^{-5}$ for GD133.

Constraints are $/ = (-5.8 1 3.8_{ m stat} 1 0.3_{ m sys}) imes 10^{-5}$ for G29-38.

Abstract

Spectra of molecular hydrogen (H$_2$) are employed to search for a possible proton-to-electron mass ratio ($\mu$) dependence on gravity. The Lyman transitions of H$_2$, observed with the Hubble Space Telescope towards white dwarf stars that underwent a gravitational collapse, are compared to accurate laboratory spectra taking into account the high temperature conditions ($T \sim 13\,000$ K) of their photospheres. We derive sensitivity coefficients $K_i$ which define how the individual H$_2$ transitions shift due to $\mu$-dependence. The spectrum of white dwarf star GD133 yields a $\Delta\mu/\mu$ constraint of $(-2.7\pm4.7_{\rm stat}\pm 0.2_{\rm sys})\times10^{-5}$ for a local environment of a gravitational potential $\phi\sim10^4\ \phi_\textrm{Earth}$, while that of G29$-$38 yields $\Delta\mu/\mu=(-5.8\pm3.8_{\rm stat}\pm 0.3_{\rm sys})\times10^{-5}$ for a potential of $2 \times 10^4$ $\phi_\textrm{Earth}$.