Modeling Reconstructed Images of Jets Launched by SANE Super-Eddington Accretion Flows Around SMBHs with the ngEHT

TL;DR

This study models the radio emission of jets from super-Eddington accretion disks around SMBHs resulting from TDEs, showing their detectability with ngEHT and potential superluminal appearance.

Contribution

It introduces detailed GRRMHD simulations of TDE jets and assesses their observability with ngEHT, highlighting the impact of black hole spin and jet properties.

Findings

Jets from super-Eddington disks can be detected up to 100 Mpc with ngEHT.

Detection depends on black hole spin and jet composition, with closer distances needed for weaker or non-spinning jets.

TDE jets may appear superluminal if the black hole is rapidly rotating and viewed face-on.

Abstract

Tidal disruption events (TDEs) around super massive black holes (SMBHs) are a potential laboratory to study super-Eddington accretion disks and sometimes result in powerful jets or outflows which may shine in the radio and sub millimeter bands. In this work, we model the thermal synchrotron emission of jets from general relativistic radiation magneto-hydrodynamics (GRRMHD) simulations of a BH accretion disk/jet system which assumes the TDE resulted in a magnetized accretion disk around a BH accreting at $\sim 12-25$ times the Eddington accretion rate. Through synthetic observations with the Next Generation Event Horizon Telescope (ngEHT) and an image reconstruction analysis, we demonstrate that TDE jets may provide compelling targets, within the context of the models explored in this work. In particular, we find that jets launched by a SANE super-Eddington disk around a spin $a_*=0.9$ reach the ngEHT detection threshold at large distances (up to 100 Mpc in this work). A two-temperature plasma in the jet or weaker jets, such as a spin $a_*=0$ model, requires a much closer distance as we demonstrate detection at 10 Mpc for limiting cases of $a_*=0,\,\mathcal{R}=1$ or $a_*=0.9,\, \mathcal{R}=20$. We also demonstrate that TDE jets may appear as superluminal sources if the BH is rapidly rotating and the jet is viewed nearly face on.