Here are some of the simulations that I have been doing for my current research work on Black hole accretion and shadow imaging. These were produced by ‘BRAHMA’ code which is written in C++ and Python. It is currently under heavy development for multiple reserach projects. It solves general relativistic radiative transfer and simulatenosly does raytracing to solve geodesic equations in arbitrary spacetimes.

Hotspot Model

A shearing hotspot around a Schwarzschild Black hole. Recent observations o four galactic center’s Supermassive Black hole, Satittarius A* displays strong variability through flaring events. These can be explained by a region of localised medium of plasma, or hotspot in the accretion disk. Here, the position of hotspot changes with time.

RIAF Model

                      

Radiatively Inefficient Accretion Flows (RIAF) is semi-analytic model for accretion where the disk is geometrically thin and optically thin. Here the observer’s angle or the inclination angle is changing from 0° to 360°.

Novikon-Thorne Think Accretion Disk

           

Novikov-Thorne Accretion disk which is geometrically thin and optically thin accretion disk model. Here the observer’s angle or the inclination angle is changing from 0° to 360°.

M87 model image and VLBI reconstructed image

            

A RIAF based model (left side) for the supermassive Black hole at the center of M87 galaxy and the reconstructed image of the same model using EHT VLBI 2017 configuration of telescopes.