Image of Bonnor black dihole with a thin accretion disk and its polarization information

Abstract

We have studied the image of Bonnor black dihole surrounded by a thin accretion disk where the electromagnetic emission is assumed to be dominated respectively by black body radiation and synchrotron radiation. Our results show that the intensity of Bonnor black dihole image increases with the magnetic parameter and the inclination angle in both radiation models. The image of Bonnor black dihole in the synchrotron radiation model is one order of magnitude brighter than that in the black body radiation model, but its intensity in the former decreases more rapidly with the radial coordinate. Especially, for the synchrotron radiation model, the intensity of the secondary image is stronger than that of the direct image at certain an inclination angle. We also present the polarization patterns for the images of Bonnor black dihole arising from the synchrotron radiation, which depend sharply on the magnetic parameter and inclination angle. Finally, we make a comparison between the polarimetric images of Bonnor black dihole and M87*. Our result further confirms that the image of black hole depends on the black hole’s properties itself, the matter around black hole and the corresponding radiation occurred in the accretion disk.

Geometrically thick equilibrium tori around a dyonic black hole with quasi-topological electromagnetism

“…( 4), we find that there exist only the radial electric field and the radial magnetic field. The corresponding electric intensity E and magnetic induction intensity B in the local orthonormal frame can be expressed as [46]…”

Imaging thick accretion disks and jets surrounding black holes

“…In the field of theoretical research, many previous studies mainly focus on the gravitational lensing effect stemming from spacetime geometry, where the light sources are modeled to be of simple structures and often as geometrically thin disks [15][16][17][18][19][20][21][22][23][24][25][26][27][28][29][30][31][32][33]. However, for a low-luminosity active galactic nuclei (LLAGN) like the M87*, the horizon-scale accretion flow is mostly geometrically thick [2,34].…”