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Hidden in the Light: Magnetically Induced Afterglow from Trapped Chameleon Fields

Holger Gies, David F. Mota, Douglas J. Shaw

TL;DR

This work proposes a magnetically induced afterglow as a unique laboratory signature of chameleon scalar fields, whose mass depends on ambient density and can trap chameleons in a vacuum chamber. By solving the coupled photon–chameleon dynamics and applying boundary conditions that reflect chameleons at chamber walls, it shows that trapped chameleons can reconvert to photons in a magnetic field, producing a detectable afterglow over macroscopic timescales. The authors quantify afterglow yields and half-lives for representative setups (GammeV, optimized configurations, and BMV), derive experimental bounds on the coupling scale $M$, and compare with astrophysical constraints, demonstrating that laboratory searches can probe cosmologically relevant parameter ranges. The results indicate that afterglow searches are a powerful, complementary tool for probing high-energy scalar sectors in the lab and may enable reconstruction of the scalar potential $V(\phi)$ by exploiting vacuum-density variations. Overall, the paper highlights the practical potential of current and near-future optical experiments to explore chameleon fields and to bridge laboratory physics with cosmological questions.

Abstract

We propose an afterglow phenomenon as a unique trace of chameleon fields in optical experiments. The vacuum interaction of a laser pulse with a magnetic field can lead to a production and subsequent trapping of chameleons in the vacuum chamber, owing to their mass dependence on the ambient matter density. Magnetically induced re-conversion of the trapped chameleons into photons creates an afterglow over macroscopic timescales that can conveniently be searched for by current optical experiments. We show that the chameleon parameter range accessible to available laboratory technology is comparable to scales familiar from astrophysical stellar energy loss arguments. We analyze quantitatively the afterglow properties for various experimental scenarios and discuss the role of potential background and systematic effects. We conclude that afterglow searches represent an ideal tool to aim at the production and detection of cosmologically relevant scalar fields in the laboratory.

Hidden in the Light: Magnetically Induced Afterglow from Trapped Chameleon Fields

TL;DR

This work proposes a magnetically induced afterglow as a unique laboratory signature of chameleon scalar fields, whose mass depends on ambient density and can trap chameleons in a vacuum chamber. By solving the coupled photon–chameleon dynamics and applying boundary conditions that reflect chameleons at chamber walls, it shows that trapped chameleons can reconvert to photons in a magnetic field, producing a detectable afterglow over macroscopic timescales. The authors quantify afterglow yields and half-lives for representative setups (GammeV, optimized configurations, and BMV), derive experimental bounds on the coupling scale , and compare with astrophysical constraints, demonstrating that laboratory searches can probe cosmologically relevant parameter ranges. The results indicate that afterglow searches are a powerful, complementary tool for probing high-energy scalar sectors in the lab and may enable reconstruction of the scalar potential by exploiting vacuum-density variations. Overall, the paper highlights the practical potential of current and near-future optical experiments to explore chameleon fields and to bridge laboratory physics with cosmological questions.

Abstract

We propose an afterglow phenomenon as a unique trace of chameleon fields in optical experiments. The vacuum interaction of a laser pulse with a magnetic field can lead to a production and subsequent trapping of chameleons in the vacuum chamber, owing to their mass dependence on the ambient matter density. Magnetically induced re-conversion of the trapped chameleons into photons creates an afterglow over macroscopic timescales that can conveniently be searched for by current optical experiments. We show that the chameleon parameter range accessible to available laboratory technology is comparable to scales familiar from astrophysical stellar energy loss arguments. We analyze quantitatively the afterglow properties for various experimental scenarios and discuss the role of potential background and systematic effects. We conclude that afterglow searches represent an ideal tool to aim at the production and detection of cosmologically relevant scalar fields in the laboratory.

Paper Structure

This paper contains 14 sections, 78 equations, 1 figure.

Table of Contents

  1. Introduction
  2. Chameleon Theories
  3. Chameleon trapping and photon afterglow
  4. Signatures of the afterglow
  5. General Signatures and Example I: the GammeV set-up
  6. Example II: An Optimized Experimental set-up
  7. Example III: The BMV set-up
  8. Experimental Bounds on Chameleon Models
  9. Background and systematic effects
  10. Standard Reflection of Photons
  11. Extinction of Chameleon Particles by a Medium
  12. Quality of the Vacuum
  13. Conclusions
  14. Interference effects

Figures (1)

  • Figure 1: Sensitivity limits for the scale $M$ specifying the inverse chameleon-photon coupling vs. the chameleon mass for the BMV Robilliard:2007bq (red dotted line) and GammeV GammeV (blue solid line) experiments as well as a hypothetical optimized experimental set-up (green dashed line); The experimental parameter values are detailed in the main text. The top left panel corresponds to an afterglow measurement with a duration $t_{\text{exp}}$ of one day, the top right panel corresponds to one minute and the lower figure to one second. The gain in sensitivity is less than an order of magnitude by waiting a day rather than a minute.