Imprints of Dark Matter on Black Hole Shadows using Spherical Accretions

Understand

We study the possibility of identifying dark matter in the galactic center from the physical properties of the electromagnetic radiation emitted from a optical-thin disk region around a static and spherically symmetric black hole.

• In particular, we consider two specific models for the optical-thin disk region: a gas at rest and a gas in a radial free fall.
• Due to the effect of dark matter on the spacetime geometry, we find that the dark matter can increase or decrease the intensity of the electromagnetic flux radiation depending on the dark matter model.
• To this end, we analyze two simple dark matter models having different mass functions $\mathcal{M}(r)$, with a matter mass $M$, thickness $\Delta r_s$ along with a dark matter core radius surrounding the black hole.