Simultaneous JWST, NuSTAR, and VLA Monitoring of Sgr A*: A Unified Picture of the Variable IR, X-ray and Radio Emission

TL;DR

This study presents simultaneous IR, X-ray, and radio observations of Sgr A* revealing correlated flares and proposing a unified physical model involving magnetic flux ejections and reconnection to explain the variable emission across wavelengths.

Contribution

It introduces a comprehensive physical scenario linking IR, X-ray, and radio variability in Sgr A* through magnetic flux rope ejections and reconnection processes.

Findings

Detection of a strong X-ray flare coincident with a near-IR flare.

Radio brightening observed about an hour after the IR and X-ray flares.

Proposed physical mechanism involving inverse Compton scattering and magnetic flux ejection.

Abstract

Flux variability is a fundamental channel of information from Sgr A* because of its direct probe of processes occurring within an accretion disk under strong gravity. We present simultaneous IR, X-ray and radio observations of Sgr A* on 2024 Apr 05 using JWST, NuSTAR, and VLA. We report the detection of a strong X-ray flare with a luminosity of $\sim5.2x10^{35}$ erg/s coincident with a bright near-IR flare, and a brightening in radio about an hour later. We investigate the candidate physical mechanisms for the X-ray flare emission and conclude that this can best be explained by inverse Compton scattering of near-IR flare radiation. We propose a dynamic scenario analogous to a coronal mass ejection in which a magnetic flux rope is ejected from Sgr A*'s inner accretion flow with a current sheet extending down from the rope to the bulk of the accretion flow. Reconnection within the sheet produces oppositely directed flows of accelerated particles moving upwards towards the rope and downwards towards the accretion flow. Infrared radiation from the approaching energetic electrons is enhanced by beaming and up-scattered by thermal electrons in the accretion flow to produce the strong X-ray flare. Meanwhile, the relativistic electrons moving in the opposite direction away from the disk experience weaker magnetic fields so radiate at longer wavelengths by feeding into the magnetic flux tube and adiabatically cooled during its subsequent expansion. This physical picture attempts to unify the origin of the variable emission from Sgr A* at IR, X-ray and radio/submm wavelengths.