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In the present study, we try to describe the evolution of rotating black holes, which are popularly known as Kerr black holes, by considering the accretion of interacting dark energy in the framework of loop quantum cosmology. Our investigation reveals that the effect of dark energy accretion on the lifetimes of Kerr black holes is insignificant, while the impact of rotation parameter is effective to some extent. Again from our investigation, we have found that the upper bound on rotating parameter ( \(a^*\) ) can’t exceed \(10^{-8} M_i^2\) for any Kerr black hole. Further, our analysis predicts that the maximum mass of a black hole supported by rotation should be \(10^{15}M_{\odot }\) , where \(M_{\odot }\) is the solar mass ( \(10^{33}\) g).

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Effects of Quantum Gravity in the Kerr Black Hole Paradigm

  • 会议论文

  • 发表日期：

    2025年

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  • Suryakanta Swain,
  • Gourishankar Sahoo,
  • Bibekananda Nayak

摘要

In the present study, we try to describe the evolution of rotating black holes, which are popularly known as Kerr black holes, by considering the accretion of interacting dark energy in the framework of loop quantum cosmology. Our investigation reveals that the effect of dark energy accretion on the lifetimes of Kerr black holes is insignificant, while the impact of rotation parameter is effective to some extent. Again from our investigation, we have found that the upper bound on rotating parameter ( \(a^*\) ) can’t exceed \(10^{-8} M_i^2\) for any Kerr black hole. Further, our analysis predicts that the maximum mass of a black hole supported by rotation should be \(10^{15}M_{\odot }\) , where \(M_{\odot }\) is the solar mass ( \(10^{33}\) g).