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arxiv: 2511.16244 · v3 · submitted 2025-11-20 · 🌌 astro-ph.CO · gr-qc

Constraining interacting dark energy models with black hole superradiance

Zhen-Hong Lyu , Rong-Gen Cai , Shao-Jiang Wang , Xiang-Xi Zeng This is my paper

Pith reviewed 2026-05-17 21:04 UTC · model grok-4.3

classification 🌌 astro-ph.CO gr-qc
keywords interacting dark energydark matterblack hole superradianceultralight bosonsastrophysical constraints
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0 comments X

The pith

Black hole superradiance constrains the coupling between dark energy and dark matter.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper shows that interactions between dark energy and dark matter change the effective mass of ultralight bosons, which then changes how fast those bosons grow through superradiance around spinning black holes. This effect offers an astrophysical test of the interaction strength that does not rely on measurements of the large-scale universe. The authors examine one case where dark energy mediates an extra force between dark matter particles and another where dark energy particles themselves become superradiant because of dense dark matter near supermassive black holes. Statistical limits on the coupling are extracted from existing black hole data, though the bounds remain weak for now.

Core claim

The DE-DM interaction alters the effective mass of the superradiant ultralight boson, thereby modifying its superradiant instability rate around spinning black holes. This connection is developed in two scenarios: a dark fifth force mediated by the DE field inside the DM sector, and a direct superradiance of the DE field itself triggered by effective-mass enhancement from dense DM spikes around supermassive black holes. Statistical analysis of black hole observations then yields limits on the DE-DM coupling strength.

What carries the argument

Superradiant instability of ultralight bosons around spinning black holes whose growth rate is shifted by DE-DM interaction-induced changes in boson effective mass.

Load-bearing premise

The interaction must change the boson mass by enough to produce a measurable change in the instability timescale, and dense dark matter spikes must exist around supermassive black holes in the second scenario.

What would settle it

A sufficiently large sample of precisely measured black hole spins and masses that shows no deviation from the instability rates predicted by the non-interacting case, even after accounting for selection effects.

read the original abstract

The recent preference for a dynamical dark energy (DE) from the Dark Energy Spectroscopic Instrument seems to call for interactions between DE and dark matter (DM), either from direct DE-DM interaction or indirect interaction induced by modified gravity. Therefore, an independent probe for these kinds of DE-DM interactions would be appealing from observational aspects. In this paper, we propose the black hole superradiance as a novel astrophysical probe for field-theoretic interacting DE-DM models, providing complementary constraints independent of large-scale cosmological observations. The core principle is that the DE-DM interaction can alter the effective mass of the superradiant ultralight boson, thereby modifying its superradiant instability rate around spinning black holes. We explore this connection through two distinct scenarios: a model where the DE field mediates a dark fifth force within the DM sector, affecting the superradiance from DM particles; and a novel mechanism where the DE field itself becomes superradiant due to the effective mass enhancement induced by dense DM spikes around supermassive black holes. By applying a statistical framework to black hole observations in both scenarios, we derive constraints on the fundamental DE-DM coupling strength. Although the current constraints are rather loose due to small samples and inaccurate measurements, our work provides new astrophysical constraints on these interacting DE-DM scenarios and establishes a new synergy between black hole physics and cosmology for probing the fundamental nature of the dark sector.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript proposes black hole superradiance as a novel probe for interacting dark energy-dark matter models. Through two scenarios—one involving a DE-mediated fifth force affecting DM superradiance and another where the DE field superradiates due to effective mass shifts from DM spikes around supermassive black holes—the authors apply a statistical framework to black hole observations to constrain the DE-DM coupling strength. The constraints are described as loose owing to limited sample sizes and measurement inaccuracies.

Significance. Should the central claims hold, this work offers an independent astrophysical avenue to test DE-DM interactions, complementing cosmological data. It merits recognition for introducing this synergy between superradiance physics and cosmology, and for outlining a statistical approach to derive bounds, even if currently limited by data quality. The application of established superradiance to these models is a strength.

major comments (2)
  1. [§4 (second scenario)] The assumption of dense DM spikes around SMBHs to induce sufficient effective mass enhancement for the DE field to superradiate is load-bearing but not fully justified. The manuscript does not show that the interaction strength bounds are compatible with the spike densities required (e.g., rho_DM sufficient for m_eff to meet omega < m Omega_H on relevant timescales), nor derives the coupled dynamics that might alter spike formation under the same coupling.
  2. [§3.1] In the first scenario, the modification to the superradiance rate from the fifth force is described qualitatively; a quantitative expression linking the coupling to the instability timescale would strengthen the claim that constraints are independent of cosmological fits.
minor comments (2)
  1. [Abstract] Clarify what 'inaccurate measurements' refers to specifically, as this impacts the interpretation of the loose constraints.
  2. [Throughout] Ensure consistent notation for the effective mass shift and coupling parameter across sections.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their positive evaluation of the significance of our work and for the constructive major comments. We address each point below and indicate the revisions we will implement to improve the manuscript.

read point-by-point responses

  1. Referee: [§4 (second scenario)] The assumption of dense DM spikes around SMBHs to induce sufficient effective mass enhancement for the DE field to superradiate is load-bearing but not fully justified. The manuscript does not show that the interaction strength bounds are compatible with the spike densities required (e.g., rho_DM sufficient for m_eff to meet omega < m Omega_H on relevant timescales), nor derives the coupled dynamics that might alter spike formation under the same coupling.

    Authors: We thank the referee for identifying this key assumption. In the revised manuscript we will expand the discussion in §4 to justify the adopted DM spike profiles by reference to the standard adiabatic-growth calculations in the literature. We will add explicit estimates showing that the DM densities needed to produce the required effective-mass shift (such that the superradiance condition ω < m Ω_H is satisfied on astrophysically relevant timescales) lie within the range of spike densities expected for SMBHs in the 10^6–10^9 M_⊙ interval. For the coupled dynamics, a full self-consistent derivation of how the DE–DM interaction modifies spike formation would require dedicated numerical simulations that lie beyond the scope of the present work. We will therefore add a concise paragraph acknowledging this limitation while noting that, for the weak couplings consistent with our derived bounds, the back-reaction remains perturbative and does not invalidate the leading-order spike assumption. revision: partial

  2. Referee: [§3.1] In the first scenario, the modification to the superradiance rate from the fifth force is described qualitatively; a quantitative expression linking the coupling to the instability timescale would strengthen the claim that constraints are independent of cosmological fits.

    Authors: We agree that an explicit formula would strengthen the presentation. In the revised version we will insert, in §3.1, a quantitative derivation of the modified superradiance growth rate that incorporates the fifth-force correction arising from the DE–DM coupling. The resulting expression will relate the instability timescale directly to the coupling strength, thereby making clearer that the derived bounds are independent of cosmological parameter fits. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation applies established superradiance physics to new interaction models

full rationale

The paper claims to use black hole superradiance as an independent astrophysical probe for field-theoretic DE-DM interactions by modifying the effective boson mass and instability rate. Constraints are obtained by applying a statistical framework to external black hole observations in two scenarios. No quoted step shows a prediction or result reducing by construction to a parameter fitted inside the same work, nor does any load-bearing premise rest solely on a self-citation chain. The central claims rely on external superradiance formulas, observational data, and stated assumptions about DM spikes, rendering the derivation self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 1 invented entities

The proposal rests on standard superradiance theory plus domain assumptions about how DE-DM interactions modify boson masses and the existence of DM spikes; no new free parameters are introduced beyond the coupling strength being constrained.

free parameters (1)
  • DE-DM coupling strength
    The fundamental parameter whose value is bounded by the superradiance observations in both scenarios.
axioms (2)
  • standard math Ultralight bosons undergo superradiant instability around spinning black holes when their Compton wavelength matches the black hole size
    Standard result in black hole physics invoked as the starting point for the modified-mass calculation.
  • domain assumption DE-DM interaction produces an effective mass shift for the superradiant boson
    Core modeling assumption stated in the abstract for both scenarios.
invented entities (1)
  • Dense DM spikes around supermassive black holes no independent evidence
    purpose: To provide the local density enhancement that raises the effective mass of the DE field in the second scenario
    Postulated structure required for the novel superradiance mechanism of the DE field itself.

pith-pipeline@v0.9.0 · 5569 in / 1530 out tokens · 59222 ms · 2026-05-17T21:04:43.429751+00:00 · methodology

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Forward citations

Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

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  2. Stellar Superradiance and Low-Energy Absorption in Dense Nuclear Media

    hep-ph 2025-12 unverdicted novelty 6.0

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