2017/10/22 by C. -H. Chen, C.-H. Chen, H. T. Cho +5
Physics and Astronomy · #Black Holes and Theoretical Physics #Black hole (networking) #Charge (physics) #Cosmology and Gravitation Theories #Mathematical physics #Noncommutative and Quantum Gravity Theories #Physics #Quantum mechanics #Spacetime #WKB approximation #gr-qc #hep-ph
paper · pdf · doi:10.1103/physrevd.97.024038
published as Phys. Rev. D 97, 024038 (2018) · 33 pages
arxiv created 2017/10/22 · openalex created_date 2017/11/10 · openalex publication_date 2018/01/25 · arxiv updated 2018/01/31 · openalex updated_date 2026/08/05
In this paper we consider spin-3/2 fields in a D-dimensional Reissner-Nordstr"om black hole spacetime. As these spacetimes are not Ricci flat, it is necessary to modify the covariant derivative to the supercovariant derivative, by including terms related to the background electromagnetic fields, so as to maintain the gauge symmetry. Using this supercovariant derivative we arrive at the corresponding Rarita-Schwinger equation in a charged black hole background. As in our previous works, we exploit the spherical symmetry of the spacetime and use the eigenspinor vectors on an N sphere to derive the radial equations for both nontransverse-traceless (non-TT) modes and TT modes. We then determine the quasinormal mode and absorption probabilities of the associated gauge-invariant variables using the WKB approximation and the asymptotic iteration method. We then concentrate on how these quantities change with the charge of the black hole, especially when they reach the extremal limits.