Shadow, quasinormal modes, greybody bounds, and Hawking sparsity of loop quantum gravity motivated non-rotating black hole

• Published in: The European physical journal. C, Particles and fields Particles and fields, 2023-10, Vol.83 (10), p.952-16, Article 952
• Main Author: Jha, Sohan Kumar
• Format: Article
• Language: English
• Subjects: Analysis; Astronomy; Astrophysics and Cosmology; Black holes; Decay rate; Electromagnetism; Elementary Particles; Gravitational waves; Hadrons; Hawking radiation; Heavy Ions; Mathematical analysis; Measurement Science and Instrumentation; Nuclear Energy; Nuclear Physics; Parameters; Perturbation; Physics; Physics and Astronomy; Quantum Field Theories; Quantum Field Theory; Quantum gravity; Radiation; Regular Article - Theoretical Physics; Shadows; Sparsity; String Theory; Waveforms
• ISSN: 1434-6052; 1434-6044; 1434-6052
• DOI: 10.1140/epjc/s10052-023-12123-4

We consider loop quantum gravity (LQG) motivated 4 D polymerized black hole and study shadow, quasinormal modes, and Hawking radiation. We obtain analytical expressions of photonsphere radius and shadow radius and study their qualitative and quantitative nature of variation with respect to the LQG parameter α . We also show shadows of the black hole for various values of α . Our study reveals that both radii increase with an increase in the parameter value. We, then, study quasinormal modes for scalar and electromagnetic perturbations using the 6th order WKB method. Our study reveals that the LQG parameter impacts quasinormal modes. We observe that the oscillation of gravitational wave (GW) and decay rate decrease as α increases. At the same time, the error associated with the 6th order WKB method increases with an increase in α . The ringdown waveform for electromagnetic and scalar perturbations is shown. We also study greybody bounds, power spectrum, and sparsity of Hawking radiation. Greybody bounds for electromagnetic perturbations do not depend on α . For scalar perturbation, greybody bounds increase as the LQG parameter increases, but the variation with α is very small. The peak of the power spectrum as well as total power emitted decrease as we increase the value of α . Also, the sparsity of Hawking radiation gets significantly impacted by quantum correction. Finally, we obtain the area spectrum of the black hole. It is found to be significantly different than that for the Schwarzschild black hole.