Quasi-periodic Eruptions from Recurrent Satellite Black Hole Transits through Magnetized Galactic Nucleus Accretion Disks
Abstract
Quasi-periodic eruptions (QPEs) are recurrent soft X-ray flares from galactic nuclei, but their origin remains uncertain. The delayed ultraviolet (UV) counterpart detected in ZTF19acnskyy provides a new constraint on viable models. We present a two-channel model in which a satellite black hole (sBH) repeatedly crosses a nuclear accretion disk threaded by a large-scale magnetic field. Gravitational focusing and dynamical drag generate hot, optically thick ejecta whose expansion and photon diffusion power the soft X-ray QPE. For fiducial Bondi-scale parameters, the model yields a characteristic X-ray duration of ∼103 s and luminosity of ∼1042 erg s−1. For ZTF19acnskyy, the model reproduces the observed day-scale X-ray duration and energetics. Simultaneously, the sBH motion compresses and bends the background magnetic field, triggering in-disk reconnection. The reconnection channel provides the energy budget and photon-diffusion delay required for the variable UV component. Unfavorable magnetic fields or diffusion times longer than the QPE recurrence period can weaken or smear out the UV signal, potentially explaining the lack of clear UV counterparts in other QPE sources.
Related
- A Unified Timescale Relation for Quasi-Periodic Eruptions and Repeated Nuclear Transients
- Extreme Mass Ratio Inspirals in Light of Quasi-periodic Eruptions: Milli-Hertz Gravitational Wave Background
- The Delay Time Distribution of Quasi-Periodic Eruptions
- Magnetized Accretion Flows with Low Angular Momentum Around Supermassive Black Holes
- Strong Black Hole Natal Kicks in Magnetized Accretion-Powered Explosions
BibTeX
@misc{wang2026quasiperiodic,
title = {{Quasi-periodic Eruptions from Recurrent Satellite Black Hole Transits through Magnetized Galactic Nucleus Accretion Disks}},
author = {Na Wang and Jing-Tong Xing and Tong Liu and Ya-Ping Li and Shuang-Liang Li},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2608.19796},
eprint = {2608.19796},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2608.19796},
note = {CC0},
}
RIS
TY - UNPB
TI - Quasi-periodic Eruptions from Recurrent Satellite Black Hole Transits through Magnetized Galactic Nucleus Accretion Disks
AU - Na Wang
AU - Jing-Tong Xing
AU - Tong Liu
AU - Ya-Ping Li
AU - Shuang-Liang Li
PY - 2026
DA - 2026/09/18
PB - arXiv
DO - 10.48550/arxiv.2608.19796
UR - https://arxiv.org/abs/2608.19796
AB - Quasi-periodic eruptions (QPEs) are recurrent soft X-ray flares from galactic nuclei, but their origin remains uncertain. The delayed ultraviolet (UV) counterpart detected in ZTF19acnskyy provides a new constraint on viable models. We present a two-channel model in which a satellite black hole (sBH) repeatedly crosses a nuclear accretion disk threaded by a large-scale magnetic field. Gravitational focusing and dynamical drag generate hot, optically thick ejecta whose expansion and photon diffusion power the soft X-ray QPE. For fiducial Bondi-scale parameters, the model yields a characteristic X-ray duration of ∼10^3 s and luminosity of ∼10^42 erg s^−1. For ZTF19acnskyy, the model reproduces the observed day-scale X-ray duration and energetics. Simultaneously, the sBH motion compresses and bends the background magnetic field, triggering in-disk reconnection. The reconnection channel provides the energy budget and photon-diffusion delay required for the variable UV component. Unfavorable magnetic fields or diffusion times longer than the QPE recurrence period can weaken or smear out the UV signal, potentially explaining the lack of clear UV counterparts in other QPE sources.
ER -