Taum Wuthicharn | Searcharxiv

arXiv2022

Quasinormal Modes of Near-Extremal Black Holes and Black Strings in Massive Gravity Background

Two numerical methods are used to calculate quasinormal modes (QNMs) of near-extremal black holes/strings in the generalized spherically/cylindrically symmetric background, the Asymptotic Iteration Method (AIM) and the Spectral Method. The numerical results confirm the accuracy of the approximate analytic formula using the Pöschl-Teller potential. Our analytic formula is used to investigate the Strong Cosmic Censorship conjecture of extremal and near-extremal black holes in Ref. \cite{Burikham:2020dfi}.

gr-qc↗

arXiv2016

A new mass scale, implications on black hole evaporation and holography

We consider a new mass scale $M_{T}=(\hbar^{2}\sqrtΛ/G)^{1/3}$ constructed from dimensional analysis by using $G$, $\hbar$ and $Λ$ and discuss its physical interpretation. Based on the Generalized Uncertainty Relation, a black hole with age comparable to the universe would stop radiating when the mass reaches a new mass scale $M'_{T}=c(\hbar/G^{2}\sqrtΛ)^{1/3}$ at which its temperature corresponds to the mass $M_{T}$. Black hole remnants could have masses ranging from a Planck mass to a trillion kilograms. Holography persists even when the uncertainty relation is modified to the Minimum Length Uncertainty Relation~(MLUR). The remnant black hole entropy is proportional to the surface area of the black hole in unit of the Planck area in arbitrary noncompact dimensions.

gr-qc↗