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On probing self interacting dark matter models through the absorption of gravitational waves

Víctor Fonoll

Abstract

In the forthcoming years, the study of the fundamental interactions between gravitational waves (GWs) and matter will be crucial in order to understand what the new generations of GWs detectors will tell us. We present the inverse bremsstrahlung (IB) absorption of GWs as a novel approach to GWs physics that can help set constraints on different physical models. We study the absorption of GWs in scattering processes of interacting dark matter. The observation of GWs of a given frequency sets constraints on its absorption efficiency. In the case of interacting dark matter, this can translate to constraints on its mass-coupling space, or in its temperature. For this, we parametrize the absorption of GWs in DM halos and in IGM, at low and very high redshifts. We find the arising constraints to be less stringent than existing ones.

On probing self interacting dark matter models through the absorption of gravitational waves

Abstract

In the forthcoming years, the study of the fundamental interactions between gravitational waves (GWs) and matter will be crucial in order to understand what the new generations of GWs detectors will tell us. We present the inverse bremsstrahlung (IB) absorption of GWs as a novel approach to GWs physics that can help set constraints on different physical models. We study the absorption of GWs in scattering processes of interacting dark matter. The observation of GWs of a given frequency sets constraints on its absorption efficiency. In the case of interacting dark matter, this can translate to constraints on its mass-coupling space, or in its temperature. For this, we parametrize the absorption of GWs in DM halos and in IGM, at low and very high redshifts. We find the arising constraints to be less stringent than existing ones.
Paper Structure (7 sections, 8 equations, 1 figure)

This paper contains 7 sections, 8 equations, 1 figure.

Table of Contents

  1. Introduction
  2. Absorption of GWs in ULDM self-scattering
  3. Characterization of the mediums of propagation
  4. Absorption in DM halos
  5. Background absorption
  6. Prospects for constraints on self-interacting DM
  7. Final remarks

Figures (1)

  • Figure 1: Left: Mass and coupling parameter space. Solid lines represent the values by which $\tau = 1$ at observed frequencies $f_0 =10^{-20}$ Hz (orange) and $f_0 =10^{-25}$ Hz (red). Additional existing constraints are plotted. In the red-shaded region $\tau \gg 1$. In yellow, physically preferred regions are highlighted. The original plot is from ref. BEC. Right: Parameter space for the temperature of DM and frequency of observation. We take physically preferred values $(m, \lambda) \approx (10^{-4}\;\text{eV}, 10^{-19})$. The plots set upper constraints on $T_{DM}$ at present for a given frequency of observation and differenet redshifts of emission $z_{em}$.