Abstract
We study the potential of gravitational wave astronomy to observe the quantum aspects of black holes with tidal heating. According to Bekenstein's quantization, we find that black hole area discretization can have observable imprints on the gravitational wave signal from an inspiraling binary black hole. We model the absorption lines and compute gravitational wave flux due to tidal heating in such a case. By including the quantization we find the dephasing of the gravitational wave. We discuss the observability of the phenomena in different parameter ranges of the binary. We show that in the inspiral, it leads to vanishing tidal heating for the high spin values. Therefore measuring nonzero tidal heating can rule out area quantization. We also argue that if area quantization is present in nature then our current modeling with reflectivity can probe the Hawking radiation.
| Original language | English |
|---|---|
| Article number | 124062 |
| Pages (from-to) | 1-11 |
| Journal | Physical Review D |
| Volume | 104 |
| Issue number | 12 |
| DOIs | |
| Publication status | Published - 15 Dec 2021 |
Bibliographical note
Funding Information:It is a pleasure to thank Adrián del Rio and Vitor Cardoso for providing us numerical data that has been used to find the analytical expression of the line width. We thank Adrián del Rio and Vitor Cardoso for reading an earlier draft of the paper carefully and giving us valuable suggestions. We thank Yash Bhargava, Bhaskar Biswas, and Soumak Maitra for useful discussions. S. D. would like to thank University Grants Commission (UGC), India, for financial support for a senior research fellowship. K. S. P. acknowledges the support of the Science and Engineering Research Board (SERB), India, and the Netherlands Organisation for Scientific Research (NWO). This work was done with partial support provided by the Tata Trusts. This paper has been assigned LIGO Document Number LIGO-P2000115.
Publisher Copyright:
© 2021 American Physical Society.
Funding
It is a pleasure to thank Adrián del Rio and Vitor Cardoso for providing us numerical data that has been used to find the analytical expression of the line width. We thank Adrián del Rio and Vitor Cardoso for reading an earlier draft of the paper carefully and giving us valuable suggestions. We thank Yash Bhargava, Bhaskar Biswas, and Soumak Maitra for useful discussions. S. D. would like to thank University Grants Commission (UGC), India, for financial support for a senior research fellowship. K. S. P. acknowledges the support of the Science and Engineering Research Board (SERB), India, and the Netherlands Organisation for Scientific Research (NWO). This work was done with partial support provided by the Tata Trusts. This paper has been assigned LIGO Document Number LIGO-P2000115.