Numerical Simulations of the interaction between winds from tidal disruption event and supermassive black hole circumnuclear medium
Abstract
The interaction between winds from tidal disruption event (TDE) and the circumnuclear medium (CNM) around supermassive black holes is believed to contribute to the radio emission of non-jetted TDEs. This model has been studied both analytically and numerically. In previous works, the properties of wind are usually set to be angle-independent. It is not clear to what extent the results deviate from those in the case where TDE wind properties are angle-dependent. We perform numerical simulations to investigate the effects of the angular distribution of wind properties on the radio light curve in the wind-CNM interaction model. We find that given that the wind mass and kinetic energy fixed, the radio light curve in the optically thin waveband significantly depends on the angle-dependence of wind properties. Even when the swept-up CNM mass is still less than the wind mass, a slight deceleration can affect the light curve. Changing the angular dependence of the wind properties causes the deceleration to vary across angles. Consequently, the final light curve--the time evolution of radiation integrated over all angles--would differ significantly from that predicted in models with a spatially uniform wind injection. This can result in a slower rise or a faster decline (depending on the CNM profile) than the analytical prediction, and can even turn the rise phase into a long-lasting plateau. Therefore, it is essential to carefully take into account the angular dependence of wind properties to study the wind-CNM interaction.
Related
- The study of the circumnuclear environment of accreting supermassive black holes with realistic X-ray spectral models
- High-energy neutrinos from shocked circumnuclear material around optically-bright and infrared-only tidal disruption events
- Tidal Disruption of Blanets by Supermassive Black Holes: From Test Particles to Planetary-Mass Bodies in Kerr Spacetime
- Electromagnetic alignment and jet precession around supermassive black holes: Quasi-periodic oscillations in tidal disruption events
- Rates of tidal disruption events from constrained cosmological simulations of the local Universe: population properties and implications for transient surveys
BibTeX
@misc{bu2026numerical,
title = {{Numerical Simulations of the interaction between winds from tidal disruption event and supermassive black hole circumnuclear medium}},
author = {De-Fu Bu and Yu-Heng Sheng and Liang Chen and Guo-Bin Mou and Hao-Jie Xia and Xiao-Hong Yang},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.38317},
eprint = {2610.38317},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.38317},
note = {CC BY-NC-ND 4.0},
}
RIS
TY - UNPB
TI - Numerical Simulations of the interaction between winds from tidal disruption event and supermassive black hole circumnuclear medium
AU - De-Fu Bu
AU - Yu-Heng Sheng
AU - Liang Chen
AU - Guo-Bin Mou
AU - Hao-Jie Xia
AU - Xiao-Hong Yang
PY - 2026
DA - 2026/10/28
PB - arXiv
DO - 10.48550/arxiv.2610.38317
UR - https://arxiv.org/abs/2610.38317
AB - The interaction between winds from tidal disruption event (TDE) and the circumnuclear medium (CNM) around supermassive black holes is believed to contribute to the radio emission of non-jetted TDEs. This model has been studied both analytically and numerically. In previous works, the properties of wind are usually set to be angle-independent. It is not clear to what extent the results deviate from those in the case where TDE wind properties are angle-dependent. We perform numerical simulations to investigate the effects of the angular distribution of wind properties on the radio light curve in the wind-CNM interaction model. We find that given that the wind mass and kinetic energy fixed, the radio light curve in the optically thin waveband significantly depends on the angle-dependence of wind properties. Even when the swept-up CNM mass is still less than the wind mass, a slight deceleration can affect the light curve. Changing the angular dependence of the wind properties causes the deceleration to vary across angles. Consequently, the final light curve--the time evolution of radiation integrated over all angles--would differ significantly from that predicted in models with a spatially uniform wind injection. This can result in a slower rise or a faster decline (depending on the CNM profile) than the analytical prediction, and can even turn the rise phase into a long-lasting plateau. Therefore, it is essential to carefully take into account the angular dependence of wind properties to study the wind-CNM interaction.
ER -