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Sharpening the dark matter signature in gravitational waveforms I: Accretion and eccentricity evolution (2402.13053v2)

Published 20 Feb 2024 in gr-qc, astro-ph.CO, and hep-ph

Abstract: Dark matter overdensities around black holes can alter the dynamical evolution of a companion object orbiting around it, and cause a dephasing of the gravitational waveform. Here, we present a refined calculation of the co-evolution of the binary and the dark matter distribution, taking into account the accretion of dark matter particles on the companion black hole, and generalizing previous quasi-circular calculations to the general case of eccentric orbits. These calculations are validated by dedicated N-body simulations. We show that accretion can lead to a large dephasing, and therefore cannot be neglected in general. We also demonstrate that dark matter spikes tend to circularize eccentric orbits faster than previously thought.

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Citations (4)
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Summary

  • The paper provides a refined theoretical model for dark matter accretion in binary systems, demonstrating its significant impact on inspiral dynamics.
  • The paper reveals that dark matter spikes influence eccentricity evolution, leading to faster circularization than previous models predicted.
  • The paper employs N-body simulations to validate dynamic friction feedback mechanisms, highlighting observable phase shifts in gravitational waveforms.

Accretion and Eccentricity in Binary Systems within Dark Matter Spikes: A Detailed Analysis

The paper "Sharpening the dark matter signature in gravitational waveforms I: Accretion and eccentricity evolution" presents an in-depth exploration of the effects of dark matter (DM) surrounding black holes on gravitational waveforms. It explores the dynamical interactions between binary systems and dark matter spikes, placing particular emphasis on the processes of dark matter accretion onto black holes and the evolution of orbital eccentricity. These phenomena have crucial implications for the paper of gravitational waves, especially in preparation for future space-based detectors such as LISA and Taiji.

Key Contributions

  1. Accretion of Dark Matter: The paper provides a refined theoretical framework to account for the accretion of DM particles by a black hole within a binary system. It presents a nuanced model considering the increase in mass of the orbiting companion due to accretion, directly affecting the inspiral dynamics. This model, validated via NN-body simulations, incorporates the accretion cross-section and interaction details, painting a comprehensive picture of particle capture by black holes.
  2. Eccentricity Evolution: Contrary to some previous assumptions that gravitational interactions simplify to near-circular orbits, this paper tackles the general case of eccentric orbits. It sheds light on how dark matter spikes influence the orbit's trajectory, correcting earlier models that did not adequately account for phase-space distributions. The paper highlights that while gravitational radiation typically circularizes orbits, dark matter interactions can modify this evolution, leading to faster circularization than previously expected.
  3. Feedback Mechanisms: Incorporating dynamical friction feedback, the authors extend their analysis to account for the redistribution of DM particles due to gravitational scattering. This feedback influences both the density profile of the DM spike and the gravitational waveform's phase, offering potential observational signatures detectable by advanced gravitational wave detectors.

Numerical Validation and Results

The authors utilize sophisticated NN-body simulations to validate their theoretical models of accretion and gravitational interactions within DM spikes. Their results underscore the significant phase shift in gravitational waveforms arising from dark matter dynamics. Accretion alone could induce a large dephasing, greatly impacting waveform analyses.

They further demonstrate that dynamic friction, traditionally assumed to eccentrify orbits based on simplistic models, may instead promote more rapid circularization when viewed through the lens of a dynamically evolving DM distribution. The paper finds these interactions also alter the gravitational wave signals in ways that depend sensitively on initial orbital conditions and the properties of the DM spike.

Theoretical and Practical Implications

The refined models of accretion and eccentricity evolution have substantial implications for both theory and observational astronomy. On a theoretical level, they challenge the assumption that intermediate and extreme mass ratio inspirals (IMRIs and EMRIs) within DM spikes can be simplified to quasi-circular dynamics. Practically, these findings suggest that future gravitational wave detectors can utilize waveform dephasing to probe the properties of dark matter around black holes, offering a unique window into the elusive nature of dark matter distribution and dynamics.

The proposed advancements in understanding the interplay between DM and binary systems validate the need for accounting for these factors in accurately modeling and interpreting gravitational wave signals. Ultimately, these insights provide a stepping stone towards employing gravitational wave astronomy as a tool for exploring the dark matter landscapes surrounding black holes, further enriching our understanding of the cosmos. Future work will need to integrate these findings into detector sensitivity models to refine the search for DM signatures in observed gravitational wave events.

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