Academia.eduAcademia.edu

Outline

Title
Abstract
Introduction
Conclusion
References
All Topics
Physics
Relativity

Shadow of rotating charged black hole with Weyl corrections

Profile image of sabir alisabir ali

2019, arXiv (Cornell University)

https://doi.org/10.48550/ARXIV.1906.04146
visibility

…

description

9 pages

link

1 file

Abstract

We construct theoretical investigation of the black hole shadow for rotating charged black hole in an asymptotically flat, axisymmetric, and stationary spacetime with Weyl corrections. This spacetime is characterized by mass (M ), charge parameter (q), rotation parameter (a), and Weyl coupling constant (α). We derive photon geodesics around the black hole and compute expressions for impact parameters with the help of photon spherical orbits conditions. We show how the presence of coupling constant α affects the shapes of black hole shadow from the usual Kerr-Newman black hole. A comparison with the standard Kerr and Kerr-Newman black hole is also include to observe the potential deviation from them. We find that the radius of black hole shadow decreases and the distortion in the shape of shadow increases with an increase in charge q for both positive and negative values of coupling constant α. We further extend our study by considering the plasma environment around the black hole and find out the essential expressions for the black hole shadow.

Related papers

Rotating black hole shadow in Rastall theory
sabir ali

arXiv: General Relativity and Quantum Cosmology, 2017

Due to gravitational lensing effect, a black hole casts a shadow larger than its horizon over a bright background and the shape and size can be calculated. We discuss rotating black holes surrounded by a perfect fluid, namely rotating Rastall black hole, which is characterized by mass $M$, spin $a$, field structure parameter $N_s$ and the Rastall parameter $\psi$. Based on a detailed discussion of the photon regions in these space-times, we derive an analytical formula for the shadow of a rotating Rastall black hole. We go on to visualize the shadow of black holes for various values of the parameters. For a given value of parameters, the presence of a positive Rastall parameter $\psi$ enlarges the shadow and reduces its deformation with respect to the one in the Kerr spacetime, while for a negative Rastall parameter $\psi$, the effect is opposite. Interestingly, for a given value of parameters $a$ and $N_s$, shadows of the black hole, deformed concentric circles with right border be...

View PDFchevron_right
Shadow of the rotating black hole with quintessential energy in the presence of the plasma
Bobomurat Ahmedov

arXiv (Cornell University), 2015

We study the shadow of the rotating black hole with quintessential energy i) in vacuum and ii) in the presence of plasma with radial power-law density. For vacuum case the quintessential field parameter of the rotating black hole sufficiently changes the shape of the shadow. With the increasing the quintessential field parameter the radius of the shadow also increases. With the increase of the radius of the shadow of the rotating black hole the quintessential field parameter causes decrease of the distortion of the shadow shape: In the presence of the quintessential field parameter the shadow of fast rotating black hole starting to become more close to circle. The shape and size of shadow of quintessential rotating black hole surrounded by plasma depends on i) plasma parameters, ii) black hole spin and iii) quintessential field parameter. With the increase of the plasma refraction index the apparent radius of the shadow increases. However, for the big values of the quintessential field parameter the change of the black hole shadow's shape due to the presence of plasma is not sufficient. In other words: the effect of the quintessential field parameter becomes more dominant with compare to the effect of plasma.

View PDFchevron_right
Optical properties of an axially symmetric black hole in the Rastall gravity
Bobomurat Ahmedov

The European Physical Journal Plus

This work is devoted to the study of the optical properties of the charged-rotating-NUT-Kiselev (CRNK) black hole in the Rastall theory of gravity. By investigating the motion of photons in the CRNK black hole spacetime in the Rastall gravity we show that the deflection angle of photons due to the gravitational lensing is mostly influenced by the NUT charge, parameter of the equation of state for the quintessence and the quintessential intensity. We observe that the effects of the rest of the spacetime parameters are negligible on the deflection angle. We present the shape of the shadow cast by the CRNK black hole in the Rastall gravity for various values of the spacetime parameters. We demonstrate that spin parameter a of the black hole changes the position and size of the shadow of the black hole very little. While changing the values of the rest of the spacetime parameters can alter the shape and the size of the observed shadow of the black hole significantly. We observe that the radius of the black hole shadow and the deflection angle of photon are bigger for the CRNK black hole in the Rastall gravity, as compared with the case of the Kerr black hole. Lastly, we show how the spacetime parameters can change the observables Rs and δs, being the average radius of the shadow and the distortion parameter that measures the deviation of the shape of the shadow from a perfect circle with radius Rs, respectively. Our results show that in most scenarios, for bigger values of Rs we get smaller values of the parameter δs.

View PDFchevron_right
Shadow of a rotating braneworld black hole
Leonardo Amarilla

Physical Review D, 2012

We investigate the shadow cast by a rotating braneworld black hole, in the Randall-Sundrum scenario. In addition to the angular momentum, the tidal charge term deforms the shape of the shadow. For a given value of the rotation parameter, the presence of a negative tidal charge enlarges the shadow and reduces its deformation with respect to Kerr spacetime, while for a positive charge, the opposite effect is obtained. We also analyze the case in which the combination of the rotation parameter and the tidal charge results in a naked singularity. We discuss the observational prospects corresponding to the supermassive black hole at the Galactic center.

View PDFchevron_right
Shadow analysis for rotating black holes in the presence of plasma for an expanding universe
abhishek chowdhuri

We explore the structure of shadow for a Kerr-de Sitter black hole with a non-magnetized, pressureless plasma surrounding it. Specific plasma distributions are considered to separate the Hamilton-Jacobi equation and find the photon regions. An analytic formula describing the boundary curve of the shadow for such a black hole in an expanding universe for an observer at any finite point outside the horizon is derived. We observe deviations which are further explored by calculating the curvature radius at a particular point for such structures in the presence and absence of plasma and calculate the diameter of the shadow.

View PDFchevron_right
Shadow cast and center of mass energy in a charged Gauss-Bonnet-AdS black hole
Saeed Ullah Khan

Chinese Journal of Physics, 2021

This work is devoted to the exploration of shadow cast and center of mass energy in the background of a 4-dimensional charged Gauss-Bonnet AdS black hole. On investigating particle dynamics, we have examined BH's metric function. Whereas, with the help of null geodesics, we pursue to calculate the celestial coordinates and the shadow radius of the black hole. We have made use of the hawking temperature to study the energy emission rate. Moreover, we have explored the center of mass energy and discussed its characteristics under the influence of spacetime parameters. For a better understanding, we graphically represent all of our main findings. The acquired result shows that both charge and AdS radius (l) decrease the shadow radius, while the Gauss-Bonnet coupling parameter α increases the shadow radius in AdS spacetime. On the other hand, both Q and α result in diminishing the shadow radius in asymptotically flat spacetime. Finally, we investigate the energy emission rate and center of mass energy under the influence of Q and α. Keywords Black hole shadow • Geodesics • Particle dynamics • Center of mass energy • AdS black hole

View PDFchevron_right
Shadow cast and deflection angle of Kerr-Newman-Kasuya spacetime
Izzet Sakalli

Journal of Cosmology and Astroparticle Physics, 2018

We study the shadow cast or silhouette generated by a Kerr-Newman-Kasuya (KNK) spacetime (rotating dyon black hole). It is shown that in addition to the angular momentum of the black hole, the dyon charge also affects the shadow image of the KNK black hole. Moreover, we analyze the weak gravitational lensing by the KNK black hole by using the Gauss-Bonnet theorem. Finally, we find that extra dyon charge decreases both the deflection angle and shadow of the KNK black hole.

View PDFchevron_right
Shadow of Kerr-Taub-NUT black hole
Yusuf Küçükakça

Astrophysics and Space Science, 2013

View PDFchevron_right
Geodesics and optical properties of a rotating black hole in Randall–Sundrum brane with a cosmological constant
Saeed Ullah Khan

Chinese Journal of Physics

The presence of tidal charge and a cosmological constant has considerable consequences on the spacetime geometry and its study is much important from the observational point of view. Henceforth, we investigate their effects on particle dynamics and the shadow cast by a Randall-Sundrum braneworld black hole with a cosmological constant. On studying the circular geodesics of timelike particles, we have acquired the expressions of energy, angular momentum and effective potential. We noted that the negative values of tidal charge and cosmological constant decreases the energy of particles. In addition, the negative value of cosmological constant leads us to the stable circular orbits, whereas its positive value destabilizes the circular orbits. Our exploration shows that the cosmological constant diminishes the radius of the black hole shadow. In response to the dragging effect, black hole rotation elongates its shadow toward the rotational axis. Besides, black hole spin and positive charge distort shadow and its distortion become maximum as far as the black hole rotates faster. We also discussed the energy emission rate by considering different cases and compared our result with the standard Kerr black hole.

View PDFchevron_right
Shadow of charged black holes in Gauss–Bonnet gravity
ashis saha, anish das

The European Physical Journal C, 2020

In this paper, we investigate the effect of higher curvature corrections from Gauss–Bonnet gravity on the shadow of charged black holes in both AdS and Minkowski spacetimes. The null geodesic equations are computed in $$d=5$$d=5 spacetime dimensions by using the directions of symmetries and Hamilton–Jacobi equation. With the null geodesics in hand, we then proceed to evaluate the celestial coordinates ($$\alpha , \beta $$α,β) and the radius $$R_s$$Rs of the black hole shadow and represent it graphically. The effects of charge Q of the black hole and the Gauss–Bonnet parameter $$\gamma $$γ on the radius of the shadow $$R_s$$Rs is studied in detail. It is observed that the Gauss–Bonnet parameter $$\gamma $$γ affects the radius of the black hole shadow $$R_s$$Rs differently for the AdS black hole spacetime in comparison to the black hole spacetime which is asymptotically flat. In particular the radius of the black hole shadow increases with increase in the Gauss–Bonnet parameter in cas...

View PDFchevron_right

References (53)

  1. B. P. Abbott et al. [LIGO Scientific and Virgo Collabo- rations], Phys. Rev. Lett. 116, 061102 (2016).
  2. M. Schmidt, Nature 197, 1040 (1963).
  3. M. J. Rees, Ann. Rev. Astron. Astrophys. 22, 471 (1984).
  4. J. Kormendy and D. Richstone, Ann. Rev. Astron. As- trophys. 33, 581 (1995).
  5. A. Eckart and R. Genzel, Nature 383, 415 (1996).
  6. A. E. Broderick, R. Narayan, J. Kormendy, E. S. Perl- man, M. J. Rieke and S. S. Doeleman, Astrophys. J. 805, 179 (2015).
  7. J. M. Bardeen, Black holes, in Proceeding of the Les Houches Summer School, Session 215239, edited by C. De Witt and B.S. De Witt and B.S. De Witt (Gordon and Breach, New York, 1973).
  8. S. Chandrasekhar, The Mathematical Theory of Black Holes (Oxford University Press, New York, 1992).
  9. S. Doeleman et al., Nature 455, 78 (2008)
  10. S. Doeleman, E. Agol, D. Backer et al., Astro2010: The Astronomy and Astrophysics Decadal Survey, Science White Papers, no. 68.
  11. A. E. Broderick, A. Loeb and R. Narayan, Astrophys. J. 701, 1357 (2009).
  12. C. Goddi et al., Int. J. Mod. Phys. D 26, 1730001 (2016).
  13. K. Akiyama et al. [Event Horizon Telescope Collabora- tion], Astrophys. J. 875, L1 (2019).
  14. K. Akiyama et al. [Event Horizon Telescope Collabora- tion], Astrophys. J. 875, L5 (2019).
  15. K. Akiyama et al. [Event Horizon Telescope Collabora- tion], Astrophys. J. 875, L6 (2019).
  16. K. Hioki and K.-i. Maeda, Phys. Rev. D 80, 024042 (2009).
  17. A. A. Abdujabbarov, L. Rezzolla and B. J. Ahmedov, Mon. Not. Roy. Astron. Soc. 454, 2423 (2015).
  18. Z. Younsi, A. Zhidenko, L. Rezzolla, R. Konoplya and Y. Mizuno, Phys. Rev. D 94, 084025 (2016).
  19. R. Takahashi, Publ. Astron. Soc. Jap. 57, 273 (2005).
  20. C. Bambi and K. Freese, Phys. Rev. D 79, 043002 (2009).
  21. S. W. Wei and Y. X. Liu, J. Cosmol. Astropart. Phys. 11 (2013) 063.
  22. C. Bambi and N. Yoshida, Class. Quant. Grav. 27, 205006 (2010).
  23. L. Amarilla, E. F. Eiroa and G. Giribet, Phys. Rev. D 81, 124045 (2010).
  24. L. Amarilla and E. F. Eiroa, Phys. Rev. D 85, 064019 (2012).
  25. A. Yumoto, D. Nitta, T. Chiba and N. Sugiyama, Phys. Rev. D 86, 103001 (2012).
  26. L. Amarilla and E. F. Eiroa, Phys. Rev. D 87, 044057 (2013).
  27. A. Abdujabbarov, F. Atamurotov, Y. Kucukakca, B. Ahmedov, and U. Camci, Astrophys. Space Sci. 344, 429 (2013).
  28. F. Atamurotov, A. Abdujabbarov and B. Ahmedov, Phys. Rev. D 88, 064004 (2013).
  29. A. Grenzebach, V. Perlick and C. Lammerzahl, Phys. Rev. D 89, no. 12, 124004 (2014).
  30. Z. Li and C. Bambi, J. Cosmol. Astropart. Phys. 01 (2014) 041.
  31. P. V. P. Cunha, C. A. R. Herdeiro, E. Radu, and H. F. Runarsson, Phys. Rev. Lett. 115, 211102 (2015).
  32. T. Johannsen, Astrophys. J. 777, 170 (2013).
  33. F. Atamurotov and B. Ahmedov, Phys. Rev. D 92, 084005 (2015).
  34. A. Abdujabbarov, M. Amir, B. Ahmedov, and S. G. Ghosh, Phys. Rev. D 93, 104004 (2016).
  35. M. Amir and S. G. Ghosh, Phys. Rev. D 94, 024054 (2016).
  36. R. Kumar, B. P. Singh, M. S. Ali, and S. G. Ghosh, arXiv:1712.09793.
  37. U. Papnoi, F. Atamurotov, S. G. Ghosh, and B. Ahme- dov, Phys. Rev. D 90, 024073 (2014).
  38. M. Amir, B. P. Singh and S. G. Ghosh, Eur. Phys. J. C 78, 399 (2018).
  39. B. P. Singh and S.G. Ghosh, Annals Phys. 395, 127 (2018).
  40. P. G. Nedkova, V. K. Tinchev, and S. S. Yazadjiev, Phys. Rev. D 88, 124019 (2013).
  41. T. Ohgami and N. Sakai, Phys. Rev. D 91, 124020 (2015).
  42. A. Abdujabbarov, B. Juraev, B. Ahmedov and Z. Stuchlík, Astrophys. Space Sci. 361, 226 (2016).
  43. R. Shaikh, Phys. Rev. D 98, 024044 (2018).
  44. M. Amir, A. Banerjee and S. D. Maharaj, Ann. Phys. 400, 198 (2019).
  45. M. Amir, K. Jusufi, A. Banerjee and S. Hansraj, arXiv:1806.07782.
  46. S. Chen and J. Jing, Phys. Rev. D 89, 104014 (2014).
  47. O. Preuss, M. P. Haugan, S. K. Solanki and S. Jordan, Phys. Rev. D 70, 067101 (2004).
  48. S. K. Solanki et al., Phys. Rev. D 69, 062001 (2004).
  49. A. Ritz and J. Ward, Phys. Rev. D 79, 066003 (2009).
  50. J. P. Wu, Y. Cao, X. M. Kuang and W. J. Li, Phys. Lett. B 697, 153 (2011).
  51. D. Z. Ma, Y. Cao and J. P. Wu, Phys. Lett. B 704, 604 (2011).
  52. D. Roychowdhury, Phys. Rev. D 86, 106009 (2012).
  53. J. L. Synge, Relativity: The General Theory, (North- Holland, Amsterdam, 1960).

Related papers

Ergosphere, Photon Region Structure, and the Shadow of a Rotating Charged Weyl Black Hole
Marco Olivares

Galaxies, 2021

In this paper, we explore the photon region and the shadow of the rotating counterpart of a static charged Weyl black hole, which has been previously discussed according to null and time-like geodesics. The rotating black hole shows strong sensitivity to the electric charge and the spin parameter, and its shadow changes from being oblate to being sharp by increasing in the spin parameter. Comparing the calculated vertical angular diameter of the shadow with that of M87*, we found that the latter may possess about 1036 protons as its source of electric charge, if it is a rotating charged Weyl black hole. A complete derivation of the ergosphere and the static limit is also presented.

View PDFchevron_right
Shadow of a Charged Rotating Black Hole in $f(R)$ Gravity
sara dastan

arXiv: General Relativity and Quantum Cosmology, 2016

We study the shadow of a charged rotating black hole in $f(R)$ gravity. This black hole is characterized by mass, $M$, spin, $a$, electric charge, $Q$ and $R_{0}$ which is proportional to cosmological constant. We analyze the image of the black hole's shadow in four types 1) at $r\rightarrow\infty$, 2) at $r\rightarrow r_{o}$, in vacuum, 3) at $r\rightarrow\infty$, 4) at $r\rightarrow r_{o}$, for an observer at the presence of plasma. Moreover, we investigate the effect of spin, charge and modfication of gravity on the shape of shadow. In addition, we use two observables, the radius $R_{s}$ and the distortion parameter $\delta_{s}$, characterizing the apparent shape. We show that for all cases, the shadow becomes smaller with increasing electric charge. Also, by increasing the rotation parameters, circular symmetry of the image of black hole's shadow will change. Furthermore, in the presence of plasma, plasma parameter also effects on size of the shadow.

View PDFchevron_right
Shadow of rotating regular black holes
Muhammed Amir

Physical Review D, 2016

We study the shadows cast by the different types of rotating regular black holes viz. Ayón-Beato-García (ABG), Hayward, and Bardeen. These black holes have in addition to the total mass (M) and rotation parameter (a), different parameters as electric charge (Q), deviation parameter (g), and magnetic charge (g *), respectively. Interestingly, the size of the shadow is affected by these parameters in addition to the rotation parameter. We found that the radius of the shadow in each case decreases monotonically and the distortion parameter increases when the value of these parameters increase. A comparison with the standard Kerr case is also investigated. We have also studied the influence of the plasma environment around regular black holes to discuss its shadow. The presence of the plasma affects the apparent size of the regular black hole's shadow to be increased due to two effects (i) gravitational redshift of the photons and (ii) radial dependence of plasma density.

View PDFchevron_right
Shadow cast by a rotating charged black hole in quintessential dark energy
Saeed Ullah Khan

2020

The existence of quintessential dark energy around a black hole has considerable consequences on its spacetime geometry. Hence, in this article, we explore its effect on horizons and the silhouette generated by a Kerr–Newman black hole in quintessential dark energy. Moreover, to analyse the deflection angle of light, we utilize the Gauss-Bonnet theorem. The obtained result demonstrates that, due to the dragging effect, the black hole spin elongates its shadow in the direction of the rotational axis, while increases the deflection angle. On the other hand, the black hole charge diminishing its shadow, as well as the angle of light’s deflection. Besides, both spin and charge significantly increase the distortion effect in the black hole’s shadow. The quintessence parameter γ, increases the shadow radius, while decreases the distortion effect at higher values of charge and spin parameters.

View PDFchevron_right
Shadow of the rotating black hole with quintessential energy in the presence of plasma
Bobomurat Ahmedov

International Journal of Modern Physics D, 2016

We study the shadow of the rotating black hole with quintessential energy (i) in vacuum, (ii) in the presence of plasma with radial power-law density. For the vacuum case, the quintessential field parameter of the rotating black hole significantly changes the shape of the shadow. With increasing quintessential field parameter, the radius of the shadow also increases. With the increase of the radius of the shadow of the rotating black hole, the quintessential field parameter causes decrease of the distortion of the shadow shape: in the presence of the quintessential field parameter, the shadow of the fast rotating black hole becomes too close to the circle. We assume the distant observer of the black hole shadow to be located near the so-called static radius where the gravitational attraction of the black hole is just balanced by the cosmic repulsion. The shape and size of the shadow of quintessential rotating black hole surrounded by plasma depends on (i) plasma parameters, (ii) bla...

View PDFchevron_right

Related topics

  • Physics
  • rotating black hole
    • 580 California St., Suite 400
    San Francisco, CA, 94104
    © 2025 Academia. All rights reserved