{"paper":{"title":"Stability analysis and quasinormal modes of Reissner Nordstr{\\o}m Space-time via Lyapunov exponent","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"gr-qc","authors_text":"Parthapratim Pradhan","submitted_at":"2012-05-25T10:41:52Z","abstract_excerpt":"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 it 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 "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1205.5656","kind":"arxiv","version":3},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}