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Some Astrophysical Aspects of a Schwarzschild Geometry Equipped with a Minimal Measurable Length
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Some Astrophysical Aspects of a Schwarzschild Geometry Equipped with a Minimal Measurable Length
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By considering a deformation of the Schwarzschild metric in the presence of a minimal measurable length which still respects the equivalence principle, we study corrections to the standard general relativistic predictions for some astrophysical phenomena such as stability of circular orbits of black hole accretion disks, redshift of black hole accretion disks, gravitational tidal forces and the geodetic drift rate. We use the \emph{Gravity Probe B} data to see robustness of our results. Our analysis shows also that the relevant deformation parameter $\varepsilon$ which has a geometric origin, plays the same role as the charge to mass ratio, $\frac{e}{m}$ in the Reissner-Nordstr\"{o}m metric.
Forward citations
Cited by 2 Pith papers
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A winding number analysis of Schwarzschild black hole stability in light of Planck-scale modified kinematics
Cubic entropy corrections from the MDR ηE³/E_P leave Schwarzschild black holes with a single physical branch of winding number W=−1; the would-be stable root is unphysical.
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A winding number analysis of Schwarzschild black hole stability in light of Planck-scale modified kinematics
For the cubic entropy correction S=πr_h²−αr_h³ arising from a Planck-scale modified dispersion relation, all physically allowed Schwarzschild-like branches have winding number w=−1, so no stable phase appears.
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