Polarization effects in Kerr black hole shadow due to the coupling between photon and bumblebee field
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Springer
Received: April 29, Revised: June 8, Accepted: June 15, Published: July 8,
2020 2020 2020 2020
Songbai Chen,a,c,1 Mingzhi Wangb and Jiliang Jinga,c a
Department of Physics, Key Laboratory of Low Dimensional Quantum Structures and Quantum Control of Ministry of Education, Synergetic Innovation Center for Quantum Effects and Applications, Hunan Normal University, Changsha, Hunan 410081, People’s Republic of China b School of Mathematics and Physics, Qingdao University of Science and Technology, Qingdao, Shandong 266061, People’s Republic of China c Center for Gravitation and Cosmology, College of Physical Science and Technology, Yangzhou University, Yangzhou 225009, People’s Republic of China
E-mail: [email protected], [email protected], [email protected] Abstract: We present firstly the equation of motion for the photon coupled to a special bumblebee vector field in a Kerr black hole spacetime and find that the propagation of light depends on its polarization due to the birefringence phenomenon. The dependence of black hole shadow on the light’s polarization is dominated by the rotation of black hole. In the non-rotating case, we find that the black hole shadow is independent of the polarization of light. However, the status is changed in the rotating case, in which the black hole shadow depends on the light’s polarization and the coupling between bumblebee vector field and electromagnetic field. These features of black hole shadow casted by polarized lights could help us to understand the bumblebee vector field with Lorentz symmetry breaking and its interaction with electromagnetic field. Keywords: Black Holes, Classical Theories of Gravity ArXiv ePrint: 2004.08857
1
Corresponding author.
c The Authors. Open Access, Article funded by SCOAP3 .
https://doi.org/10.1007/JHEP07(2020)054
JHEP07(2020)054
Polarization effects in Kerr black hole shadow due to the coupling between photon and bumblebee field
Contents 1 Introduction
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2 Equation of motion for the photons coupled to bumblebee field in a Kerr black hole spacetime 2
4 Summary
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Introduction
One of the most exciting events in observing black holes is that Event Horizon Telescope Collaboration [1, 2] released the first image of the supermassive black hole in the center of M87 galaxy at the last year. The information stored in the image has been applied extensively to study the possibility of constraining black hole parameters and extra dimension size [3, 4], and to probe some fundamental physics issues including dark matter [5–9], the equivalence principle [10], and so on. Black hole shadow, caused by light rays that fall into an event horizon, is one of the most important ingredients in the image. Generally, the black hole shadow in the observer’s sky is determined by black hole, the propagation of light ray and the position of observer. It is shown that black hole shadow depends also on the polarization of light itself if we consider some interactions between electromagnetic and gravitational fields, such as Weyl tensor coupling
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