Image of Kerr-Melvin black hole with thin accretion disk

TL;DR

This paper models the observational appearance of Kerr-Melvin black holes with thin accretion disks, analyzing how magnetic fields and black hole spins influence their images and shadows.

Contribution

It introduces a numerical backward ray-tracing method to simulate black hole images considering magnetic fields and accretion disk properties.

Findings

Inner shadow and critical curves can estimate magnetic field strength.

Black hole spin and magnetic field significantly affect image features.

Profiles of red-shift reveal relativistic effects near the black hole.

Abstract

In this present work, we study the observational appearance of Kerr-Melvin black hole (KMBH) illuminated by an accretion disk. The accretion disk is assumed to be located on the equatorial plane and be thin both geometrically and optically. Considering the fact that outside the innermost stable circular orbit (ISCO) the accretion flow moves in prograde or retrograde circular orbit and falls towards the horizon along plunging orbit inside the ISCO, we develop the numerical backward ray-tracing method and obtain the images of KMBH accompanying with the accretion disk for various black hole spins, strengths of magnetic fields and inclination angles of observers. We present the intensity distribution horizontally and longitudinally and show the profiles of the red-shift for the direct and lensed images. Our study suggests that the inner shadow and critical curves can be used to estimate the magnetic field around a black hole without degeneration.