[论文解读] Telling tails and quasi-resonances in the vicinity of Dymnikova regular black hole

Bekir Can Lütfüoğlu, Javlon Rayimbaev+3 more|arXiv (Cornell University)|Jan 25, 2026

Black Holes and Theoretical Physics被引用 0

一句话总结

该论文分析在 Dymnikova 规则黑洞中对大质量标量场的准规范模、晚期尾波及灰体因子，发现大质量下存在准共振且质量抑制辐射。

ABSTRACT

We investigate quasinormal modes, late-time tails, and grey-body factors for massive scalar perturbations in the background of the Dymnikova regular black hole. By applying both the time-domain integration and the WKB method with Padé improvements, we show that the spectrum of massive fields differs qualitatively from the massless case. The oscillation frequency of the dominant mode grows with the field mass $μ$, while the damping rate decreases, suggesting the existence of quasi-resonances at sufficiently large $μ$. In the time domain, the late-time signal exhibits oscillatory tails with a power-law envelope, whose decay rate matches analytic expectations. Grey-body factors are also computed, showing strong suppression of radiation when mass is increased. Taken together, these results indicate that massive fields provide distinctive signatures of regular black holes and may serve as probes of near-horizon quantum corrections in the Dymnikova geometry.

研究动机与目标

• Motivate the study of massive field perturbations in regular, quantum-corrected black holes.
• Explore how mass alters the quasinormal spectrum and late-time behavior in the Dymnikova geometry.
• Assess how a massive scalar field probes near-horizon quantum corrections through observable signatures.

提出的方法

• Solve the Klein–Gordon equation on the Dymnikova background and derive the master wave equation with an effective potential V_l(r).
• Employ time-domain integration with Gundlach–Price–Pullin style evolution and Prony fitting to extract frequencies.
• Apply the WKB method with Padé improvements (6th order and above, e.g., [3/3]) to estimate quasinormal modes.
• Use the tortoise coordinate to cast the problem into a Schrödinger-like form and impose purely ingoing/outgoing boundary conditions for QNMs.
• Compare time-domain results with WKB–Padé predictions to validate accuracy and identify regimes where WKB remains reliable.
• Discuss the relation between QNMs and grey-body factors and use this to infer transmission coefficients for massive fields.

实验结果

研究问题

• RQ1 Do quasinormal modes and their damping rates for a massive scalar field differ qualitatively from the massless case in the Dymnikova black hole?
• RQ2 Do quasi-resonances (arbitrarily long-lived modes) appear for sufficiently large field mass μ in this geometry?
• RQ3 How does the late-time tail of a massive field differ from the massless power-law decay, and what is its asymptotic form in the Dymnikova background?
• RQ4 How are grey-body factors for massive fields affected by increasing mass in this regular black-hole spacetime?

主要发现

• Increasing field mass μ increases the real part of the dominant quasinormal frequency.
• Increasing μ decreases the damping rate, suggesting the presence of quasi-resonances at sufficiently large μ.
• Late-time tails of massive perturbations become oscillatory with a power-law envelope, with an asymptotic decay Phi(t) ~ t^{-7/8} sin(μ t + φ) for the Dymnikova black hole.
• Grey-body factors are strongly suppressed as the field mass grows, indicating reduced emission of massive particles.
• WKB–Padé calculations provide accurate estimates for l=1 and higher and align with time-domain results, while large μ regions require time-domain methods due to potential shape changes.
• The results support the view that massive fields offer distinctive signatures of regular (quantum-corrected) black holes and probe near-horizon corrections in the Dymnikova geometry.