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- W2156565719 abstract "We explicitly derive the proper time $(tau)$ principal Lyapunov exponent ($lambda_{p}$) and coordinate time ($t$) principal Lyapunov exponent ($lambda_{c}$) for Reissner Nordstr{o}m (RN) black hole (BH) . We also compute their ratio. For RN space-time, it is shown that the ratio is $frac{lambda_{p}}{lambda_{c}}=frac{r_{0}}{sqrt{r_{0}^2-3Mr_{0}+2Q^2}}$ for time-like circular geodesics and for Schwarzschild BH the ratio is $frac{lambda_{p}}{lambda_{c}}=frac{sqrt{r_{0}}}{sqrt{r_{0}-3M}}$. We further show that their ratio $frac{lambda_{p}}{lambda_{c}}$ may vary from orbit to orbit. For instance, Schwarzschild BH at innermost stable circular orbit(ISCO), the ratio is being $frac{lambda_{p}}{lambda_{c}}mid_{r_{ISCO}=6M}=sqrt{2}$ and at marginally bound circular orbit (MBCO) the ratio is calculated to be $frac{lambda_{p}}{lambda_{c}}mid_{r_{mb}=4M}=2$. Similarly, for extremal RN BH the ratio is at ISCO: $frac{lambda_{p}}{lambda_{c}}mid_{r_{ISCO}=4M}=frac{2sqrt{2}}{sqrt{3}}$. We also further analyzes the geodesic stability via this exponent. By evaluating the Lyapunov exponent, it is shown that emph{ in the eikonal limit , the real and imaginary parts of the quasinormal modes of RN BH are given by the frequency and instability time scale of the unstable null circular geodesics}." @default.
- W2156565719 created "2016-06-24" @default.
- W2156565719 creator A5026583379 @default.
- W2156565719 date "2012-05-25" @default.
- W2156565719 modified "2023-09-27" @default.
- W2156565719 title "Stability Analysis of the Reissner Nordstr{o}m Circular Orbits" @default.
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