Numerical Simulations of the Circularized Accretion Flow in Population III Star Tidal Disruption Events. I. The Accretion Flow and the Wind

TL;DR

This paper uses radiative hydrodynamic simulations to study the accretion flow and wind properties in Population III star tidal disruption events, revealing strong winds and high accretion rates that influence observable features.

Contribution

It provides the first detailed simulation-based analysis of the accretion flow and wind characteristics in Pop III star TDEs, highlighting the impact of winds on accretion and radiation.

Findings

Black hole accretion rate is highly super-Eddington.

A strong radiation-driven wind is produced.

Only 25-35% of fallback debris is accreted by the black hole.

Abstract

Tidal Disruption Events (TDEs) have recently been proposed as potential probes for Population III stars. However, the properties of the accretion flow and the wind from the Pop III star TDE system are not clear. By performing radiative hydrodynamic simulations, we study the 'circularized' accretion flow of the Pop III star TDE system. The masses of the black hole (BH) and the disrupted star are $10^6$ and $300$ solar masses, respectively. We focus on the properties of the wind. We find that the black hole accretion rate is highly super-Eddington. A strong wind is driven by radiation pressure. Due to the presence of a strong wind, only $25\%$--$35\%$ of the fallback debris is accreted by the BH. The remaining part is taken away by the wind. The kinetic power of the wind can be as high as $10^{46} {\rm \ erg \ s^{-1}}$. The properties of the wind obtained in this paper may be useful for understanding the radiation properties of Pop III star TDEs in the context of the wind 'reprocessing' model.