Relativistic Signatures at the Galactic Center

TL;DR

This paper investigates the physical processes behind the variable emission from Sgr A* at the Galactic Center by modeling the accretion disk's emission near a rotating black hole's event horizon.

Contribution

It introduces a method to analyze time-variable spectral features of Sgr A* and presents preliminary models of emission near the black hole's marginally stable orbit.

Findings

Preliminary modeling of emission spectra near the black hole.

Insights into the variability mechanisms of Sgr A*.

Methodology for analyzing spectral features over time.

Abstract

Studies of the inner few parsecs at the Galactic Centre provide evidence of a supermassive black hole, associated with the unusual, variable radio and infrared source Sgr A*. Our major aim is the study and analysis of the physical processes responsible for the variable emission from the compact radio source Sgr A*. In order to understand the physics behind the observed variability, we model the time evolution of the flare emitting region by studying light curves and spectra of emission originating at the surface of the accretion disk, close to the event horizon, near the marginally stable orbit of a rotating black hole. Here we discuss the methods used in the analysis of the time-variable spectral features and subsequently present preliminary modeling results.