Photon Regions and Shadows of Kerr-Newman-NUT Black Holes with a Cosmological Constant

By A. Grenzebach, V. Perlick, C. Lammerzahl. 2014

313 citations recorded by the source corpus.

We consider the Pleba\ifmmode \acute{n}\else \'{n}\fi{}ski class of electrovacuum solutions to the Einstein equations with a cosmological constant. These space-times, which are also known as the Kerr-Newman-NUT--(anti--)de Sitter space-times, are characterized by a mass $m$, a spin $a$, a parameter $\ensuremath{\beta}$ that comprises electric and magnetic charge, a NUT parameter $\ensuremath{\ell}$ and a cosmological constant $\mathrm{\ensuremath{\Lambda}}$. Based on a detailed discussion of the photon regions in these space-times (i.e., of the regions in which spherical lightlike geodesics exist), we derive an analytical formula for the shadow of a Kerr-Newman-NUT--(anti--)de Sitter black hole for an observer at given Boyer-Lindquist coordinates $({r}_{O},{\ensuremath{\vartheta}}_{O})$ in the domain of outer communication. We visualize the photon regions and the shadows for various values of the parameters.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/11badcc191f6674f3718d1bbaa9930f6fbecbb83

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Rahul Kumar
2. Sushant G. Ghosh
3. O. Tsupko
4. G. Bisnovatyi-Kogan
5. V. Perlick
6. A. Abdujabbarov
7. B. Ahmedov
8. Luciano Rezzolla

In Atomic and Molecular Physics, and Optics

1. O. Tsupko
2. Rahul Kumar
3. Sushant G. Ghosh
4. G. Bisnovatyi-Kogan
5. Luciano Rezzolla
6. V. Perlick

In Nuclear and High Energy Physics

1. Rahul Kumar
2. O. Tsupko
3. Sushant G. Ghosh
4. G. Bisnovatyi-Kogan
5. V. Perlick
6. A. Abdujabbarov
7. B. Ahmedov
8. Luciano Rezzolla

Citations in the corpus

• Black Hole Parameter Estimation from Its Shadow (2018, methodology): “Although rotating black holes generically have two distinct photon regions, inside the Cauchy horizon (r−) and outside the event horizon (r+), for a black hole shadow we will be only focusing on the latter, i.e., for > +r rp (Grenzebach et al. 2014).”
• A coordinate-independent characterization of a black hole shadow (2015, background): “In most cases, the expression of the shadow as a closed polar curve is not known analytically, but for the Plebański-Demiański class of space-times, the shadow has been cast in an analytic form (Grenzebach et al. 2014, 2015).”
• Calculating black hole shadows: Review of analytical studies (2021, methodology): “For pictures of the Kerr photon region see [4], [75] or [40].”
• Black hole shadow in an expanding universe with a cosmological constant (2018, methodology): “More generally, an analytical formula for the shape and the size of the shadow of a black hole of the Plebański-Demiański class, for an observer anywhere in the domain of outer communication, was derived by Grenzebach et al.[3, 4].”
• Rotating black holes in 4D Einstein-Gauss-Bonnet gravity and its shadow (2020, background): “Indeed rotating black holes have two distinct photon regions, one inside the Cauchy horizon and another outside the event horizon [104].”
• Gravitational Lensing in Presence of Plasma: Strong Lens Systems, Black Hole Lensing and Shadow (2017, methodology): “For an illustration see Figure 7 in [85].”