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The Impact of Dark Matter on Gravitational Wave Detection by Space-based Interferometers

Yuezhe Chen, Pan-Pan Wang, Bo Wang, Rui Luo, Cheng-Gang Shao

Abstract

The existence of dark matter is supported by multiple astrophysical observations, yet its particle nature remains unknown. The development of gravitational wave astronomy, especially with future space-based detectors such as LISA, provides new opportunities to study the interactions between dark matter and compact-object systems. This review summarizes the main dark matter candidates and their macroscopic distributions, and highlights three mechanisms through which dark matter can affect gravitational wave observations: (1) modifications to compact-object orbits and the dynamics of systems such as extreme mass-ratio inspirals, including dark matter spikes, dynamical friction, and potential perturbations; (2) gravitational lensing effects induced by the spatial distribution of dark matter, altering waveform amplitudes and phases; and (3) direct couplings between ultralight dark matter fields and detectors. As low-frequency gravitational wave detection techniques are proposed and continue to develop, these effects may offer a novel avenue for probing the properties of dark matter, and combining precise waveform modeling with multi-messenger observations could reveal insights into its microscopic structure.

The Impact of Dark Matter on Gravitational Wave Detection by Space-based Interferometers

Abstract

The existence of dark matter is supported by multiple astrophysical observations, yet its particle nature remains unknown. The development of gravitational wave astronomy, especially with future space-based detectors such as LISA, provides new opportunities to study the interactions between dark matter and compact-object systems. This review summarizes the main dark matter candidates and their macroscopic distributions, and highlights three mechanisms through which dark matter can affect gravitational wave observations: (1) modifications to compact-object orbits and the dynamics of systems such as extreme mass-ratio inspirals, including dark matter spikes, dynamical friction, and potential perturbations; (2) gravitational lensing effects induced by the spatial distribution of dark matter, altering waveform amplitudes and phases; and (3) direct couplings between ultralight dark matter fields and detectors. As low-frequency gravitational wave detection techniques are proposed and continue to develop, these effects may offer a novel avenue for probing the properties of dark matter, and combining precise waveform modeling with multi-messenger observations could reveal insights into its microscopic structure.
Paper Structure (19 sections, 24 equations, 2 figures, 3 tables)

This paper contains 19 sections, 24 equations, 2 figures, 3 tables.

Table of Contents

  1. Introduction
  2. Dark Matter Candidates and Probing
  3. Weakly Interacting Massive Particles
  4. Ultralight Dark Matter
  5. Axions
  6. Scalar Field Dark Matter
  7. Vector Field Dark Matter
  8. Dark Matter Halos — NFW, Burkert, and Hernquist Models
  9. Self-Interacting Dark Matter
  10. Probes of Dark Matter
  11. Dark Matter Effects on Gravitational Waves
  12. Effects of Dark Matter on Gravitational Wave Sources
  13. Effects of Dark Matter on EMRIs
  14. Effects of Dark Matter on Compact Binary Systems
  15. Effects of Dark Matter on Supermassive Black Hole Mergers and Primordial Black Holes
  16. ...and 4 more sections

Figures (2)

  • Figure S1: Schematic illustration of the effects of DM on GWs from their generation to detection. The white solid and dashed curves represent GWs emitted by the source with and without the influence of DM, respectively. The blue and red solid curves denote the corresponding GW signals after propagation through the Universe, where they may be further modified by DM-induced gravitational lensing. This figure is intended as a conceptual illustration of the different stages at which DM can affect GW observations, rather than a quantitative prediction. The impact of DM on GW detectors is not explicitly shown. The three space-based detectors orbiting the Sun, from top to bottom, are LISA, TianQin, and Taiji.
  • Figure S2: EMRI waveforms under constant DM models. Solid (dashed) lines show GW waveforms with (without) dynamical friction effects included.The main panel displays the waveform comparison over the entire inspiral evolution, which spans a very long timescale characteristic of EMRIs. The inset windows show zoomed-in waveform segments at the early, intermediate, and late stages of the inspiral, respectively, highlighting the local phase evolution and the cumulative impact of dynamical friction.