- Łukaszyk Patent Attorneys, Katowice, Poland
A black hole represents a quantum state that saturates three bounds of the quantum orthogonalization interval. It is a qubit in an equal superposition of its two energy eigenstates, with a vanishing ground state and a nonvanishing one equal to the black hole’s energy, where the product of the black hole’s entropy and temperature amounts to half of its energy. As two black holes frequently merge into one, it is natural to ask what happens with the qubits they carry. I consider a binary black hole as a quantum system of two independent qubits evolving independently under a common Hamiltonian to show that their merger can be considered in terms of two orthogonal projections of this Hamiltonian onto a two-dimensional Hilbert subspace, which correspond to the Bell states of this two-qubit system.
1 Introduction
I have previously (Łukaszyk, 2023) shown that a black hole (BH) can be considered a patternless (Chaitin, 1966) bitstring of
The consideration of qubits and BHs within a single conceptual framework is known from the state of the art (see, for example, Borsten et al., 2009; Lévay, 2010; Duff, 2013; Giddings and Shi, 2013; Verlinde and Verlinde, 2013; Prudêncio et al., 2015; Belhaj et al., 2016; Osuga and Page, 2018; Broda, 2021).
Interferometric data1 on collisions of celestial objects (called “mergers”) indicate that the fraction of BH mergers is much higher than might be expected by chance (Gerosa and Fishbach, 2021; Abbott et al., 2021; Abbott et al., 2023b; Abbott et al., 2023a; Dall’Amico et al., 2024). While gravitational events are real, labeling them as waves may be misleading—normal modulation of the gravitational potential caused by merging objects should not be interpreted as a gravitational wave understood as a carrier of gravity (Szostek et al., 2019). Furthermore, based on the gravitational event GW170817, it was experimentally confirmed that mergers are perfectly spherical (Sneppen et al., 2023). This is also an expected result as no point of impact can be considered unique on a patternless, perfectly spherical BH surface. BHs may be different from their general relativistic counterparts outside Einstein’s relativity (Li et al., 2023).
In this study, I show that a merger of two BHs, as expected, converts a separable two-qubit BH state into a single-qubit BH state.
2 Black hole Hamiltonian
Consider a general
expressed as a linear combination of the Pauli matrices
where the relative phase
are their corresponding normalized eigenstates, which are commonly referred to as “stationary states” (Nielsen and Chuang, 2010). This is because, under the Hamiltonian’s (Equation 1) evolution, they only acquire an overall numerical factor,
and the variance of the Hamiltonian (Equation 1) for the qubit (Equation 2) and its variance of energy is
where the bra-ket terms
According to Levitin and Toffoli (2009), the minimum time needed for any quantum state to evolve into an orthogonal state, known as the “quantum orthogonalization interval”
Furthermore,
I previously found that a BH is the only quantum system having a vanishing ground-state energy, only two possible states, and average energy equal to its standard deviation and half of its total energy (Łukaszyk, 2023; 2024). Thus, a BH’s average energy is its entropic work, which is the scalar product of the BH (Hawking) temperature and (Bekenstein) entropy
where
is the BH energy, and
tend as shown in the Equation 12 to orthogonality with the increasing size of the quantum system as shown in Equation 9. Even toy examples involving just two nonorthogonal states could shed some light on the foundations of quantum theory (Fuchs, 2002).
Expressing the BH energy
With
The stationary eigenstates of the Hamiltonian (Equation 10) are
and the BH qubit (Equation 2) can be expressed as
where, in particular,
which cannot be further reduced to
The unitary evolution operator of the Hamiltonian (Equation 10) is
where
if invoked
3 Merging two qubits into one
If the Hamiltonian (Equation 10) governs the evolution of one BH, then the evolution of two BHs
with
The Hamiltonian (Equation 16) has four eigenvalues (Equation 17)
associated with four eigenstates given by (Equation 18)
Hence, the BHs
and the evolution operator
The BH merger
A merger cannot trace out one qubit from the two-qubit system (Equation 19), as partial trace applies to mixed states and time evolution, not directly to a Hamiltonian. Furthermore, partial trace models a measurement, so that it would be tantamount to asserting that BH
Therefore, the merger must reduce the dimension of the Hamiltonian from
Three distinct projections of the Hamiltonian
for the subspaces spanned by
and for the subspaces spanned by
We must reject the nonorthogonal projection (Equations 21, 22) as they allow the state transitions of one qubit while fixing the state of the other. For example, the projection (Equation 22) of the Hamiltonian (Equation 16) onto a two-dimensional Hilbert subspace spanned by
On the other hand, the orthogonal projection (Equation 23) seems not to preserve the form of the BH Hamiltonian (Equation 10). However, we must not forget that we are crossing the singularity here: we merge two independently evolving, quantum systems
for
Furthermore, the evolution operator of the Hamiltonian (Equation 16) is the anti-diagonal matrix for
4 Conclusion
The qubit (Equation 12) in equal superposition of two energy eigenstates, attaining the bounds for the quantum orthogonalization interval (Mandelstam and Tamm, 1945; Margolus and Levitin, 1998; Levitin and Toffoli, 2009), introduces the Hamiltonian (Equation 10) that completely describes BH dynamics (Nielsen and Chuang, 2010) and is parametrized by one observable parameter (e.g., the BH energy) and the unobservable, relative phase of the qubit.
Considering a binary BH as a quantum system of two independent qubits (Equation 20) evolving independently under a common Hamiltonian (Equation 16), I have shown that their merger can be considered in terms of the orthogonal projection of this Hamiltonian onto a two-dimensional Hilbert subspace spanned by
The relation (Equation 24) shows that BH qubits must be orthogonal to merge. Otherwise, the merger would violate the no-deleting (Kumar Pati and Braunstein, 2000) and no-hiding (Braunstein and Pati, 2007) theorems. On the other hand, the orthogonalization interval (Equation 8) is inversely proportional to the BH’s energy. This may explain why mergers of massive BHs are the most frequently registered gravitational events.
Data availability statement
The original contributions presented in the study are included in the article/supplementary material; further inquiries can be directed to the corresponding author.
Author contributions
SŁ: Writing – review and editing, Writing – original draft.
Funding
The author(s) declare that no financial support was received for the research and/or publication of this article.
Acknowledgments
I thank my partners Wawrzyniec Bieniawski and Piotr Masierak for critical discussion and feedback.
Conflict of interest
Author SŁ was the sole owner of Łukaszyk Patent Attorneys during the conduct of this study.
Generative AI statement
The author(s) declare that no Generative AI was used in the creation of this manuscript.
Any alternative text (alt text) provided alongside figures in this article has been generated by Frontiers with the support of artificial intelligence and reasonable efforts have been made to ensure accuracy, including review by the authors wherever possible. If you identify any issues, please contact us.
Publisher’s note
All claims expressed in this article are solely those of the authors and do not necessarily represent those of their affiliated organizations, or those of the publisher, the editors and the reviewers. Any product that may be evaluated in this article, or claim that may be made by its manufacturer, is not guaranteed or endorsed by the publisher.
Footnotes
1Available online at the Gravitational Wave Open Science Center (GWOSC) portal https://www.gw-openscience.org/eventapi/html/allevents.
References
Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, A., et al. (2021). Population properties of compact objects from the second LIGO–virgo gravitational-wave transient catalog. Astrophysical J. Lett. 913, L7. doi:10.3847/2041-8213/abe949
Abbott, R., Abbott, T., Acernese, F., Ackley, K., Adams, C., Adhikari, N., et al. (2023a). GWTC-3: compact binary coalescences observed by LIGO and virgo during the second part of the third observing run. Phys. Rev. X 13, 041039. doi:10.1103/PhysRevX.13.041039
Abbott, R., Abbott, T., Acernese, F., Ackley, K., Adams, C., Adhikari, N., et al. (2023b). Population of merging compact binaries inferred using gravitational waves through GWTC-3. Phys. Rev. X 13, 011048. doi:10.1103/PhysRevX.13.011048
Bekenstein, J. D. (1973). Black holes and entropy. Phys. Rev. D. 7, 2333–2346. doi:10.1103/PhysRevD.7.2333
Belhaj, A., Benslimane, Z., Sedra, M. B., and Segui, A. (2016). Qubits from black holes in M-theory on K3 surface. Int. J. Geometric Methods Mod. Phys. 13, 1650075. doi:10.1142/S0219887816500754
Borsten, L., Dahanayake, D., Duff, M., Ebrahim, H., and Rubens, W. (2009). Black holes, qubits and octonions. Phys. Rep. 471, 113–219. doi:10.1016/j.physrep.2008.11.002
Braunstein, S. L., and Pati, A. K. (2007). Quantum information cannot be completely hidden in correlations: implications for the black-hole information paradox. Phys. Rev. Lett. 98, 080502. doi:10.1103/PhysRevLett.98.080502
Broda, B. (2021). Causal unitary qubit model of black hole evaporation. Phys. Lett. B 820, 136564. doi:10.1016/j.physletb.2021.136564
Chaitin, G. J. (1966). On the length of programs for computing finite binary sequences. J. ACM 13, 547–569. doi:10.1145/321356.321363
Dall’Amico, M., Mapelli, M., Torniamenti, S., and Arca Sedda, M. (2024). Eccentric black hole mergers via three-body interactions in young, globular, and nuclear star clusters. Astron. Astrophys. 683, A186. doi:10.1051/0004-6361/202348745
Duff, M. J. (2013). “Black holes and qubits,” in What is known and unexpected at LHC (Erice-Sicily, Italy: World Scientific), 57–66. doi:10.1142/9789814522489_0003
Fuchs, C. A. (2002). Just two nonorthogonal quantum states. Boston, MA: Springer US, 11–16. doi:10.1007/0-306-47097-7_2
Gerosa, D., and Fishbach, M. (2021). Hierarchical mergers of stellar-mass black holes and their gravitational-wave signatures. Nat. Astron. 5, 749–760. doi:10.1038/s41550-021-01398-w
Giddings, S. B., and Shi, Y. (2013). Quantum information transfer and models for black hole mechanics. Phys. Rev. D. 87, 064031. doi:10.1103/PhysRevD.87.064031
Kumar Pati, A., and Braunstein, S. L. (2000). Impossibility of deleting an unknown quantum state. Nature 404, 164–165. doi:10.1038/404130b0
Lévay, P. (2010). STU black holes as four-qubit systems. Phys. Rev. D. 82, 026003. doi:10.1103/PhysRevD.82.026003
Levitin, L. B., and Toffoli, T. (2009). Fundamental limit on the rate of quantum dynamics: the unified bound is tight. Phys. Rev. Lett. 103, 160502. doi:10.1103/PhysRevLett.103.160502
Li, D., Wagle, P., Chen, Y., and Yunes, N. (2023). Perturbations of spinning black holes beyond general relativity: modified teukolsky equation. Phys. Rev. X 13, 021029. doi:10.1103/PhysRevX.13.021029
Łukaszyk, S. (2023). Black hole horizons as patternless binary messages and markers of dimensionality. New York, United States: Nova Science Publishers, 317–374. doi:10.52305/RLIT5885
Łukaszyk, S. (2024). Life as the explanation of the measurement problem. J. Phys. Conf. Ser. 2701, 012124. doi:10.1088/1742-6596/2701/1/012124
Mandelstam, L., and Tamm, I. (1945). The uncertainty relation between energy and time in non-relativistic quantum mechanics. J. Phys. (USSR) 9, 249–254. doi:10.1007/978-3-642-74626-0_8
Margolus, N., and Levitin, L. B. (1998). The maximum speed of dynamical evolution. Phys. D. Nonlinear Phenom. 120, 188–195. doi:10.1016/S0167-2789(98)00054-2
Nielsen, M. A., and Chuang, I. L. (2010). Quantum computation and quantum information. Cambridge: Cambridge University Press.
Osuga, K., and Page, D. N. (2018). Qubit transport model for unitary black hole evaporation without firewalls. Phys. Rev. D. 97, 066023. doi:10.1103/PhysRevD.97.066023
Pienaar, J. (2021). A quintet of quandaries: five No-go theorems for relational quantum mechanics. Found. Phys. 51, 97. doi:10.1007/s10701-021-00500-6
Prudêncio, T., Cirilo-Lombardo, D. J., Silva, E. O., and Belich, H. (2015). Black hole qubit correspondence from quantum circuits. Mod. Phys. Lett. A 30, 1550104. doi:10.1142/S0217732315501047
Shannon, C. E. (1948). A mathematical theory of communication. Bell Syst. Tech. J. 27, 379–423. doi:10.1002/j.1538-7305.1948.tb01338.x
Sneppen, A., Watson, D., Bauswein, A., Just, O., Kotak, R., Nakar, E., et al. (2023). Spherical symmetry in the kilonova AT2017gfo/GW170817. Nature 614, 436–439. doi:10.1038/s41586-022-05616-x
Szostek, R., Góralski, P., and Szostek, K. (2019). Gravitational waves in Newton’s gravitation and criticism of gravitational waves resulting from the General Theory of Relativity (LIGO). Bull. Karaganda Univ. “Physics” Ser. 96, 39–56. doi:10.31489/2019Ph4/39-56
Keywords: quantum orthogonalization intervals, quantum foundations and information, black hole merger, black hole information paradox, emergent dimensionality
Citation: Łukaszyk S (2025) Black hole merger as an event converting two qubits into one. Front. Quantum Sci. Technol. 4:1656200. doi: 10.3389/frqst.2025.1656200
Received: 29 June 2025; Accepted: 29 August 2025;
Published: 08 October 2025.
Edited by:
Inyong Park, Philander Smith College, United StatesReviewed by:
Francesco Giovanni Celiberto, University of Alcalá, SpainVarsha Sambhaje, SRM University AP, India
Copyright © 2025 Łukaszyk. This is an open-access article distributed under the terms of the Creative Commons Attribution License (CC BY). The use, distribution or reproduction in other forums is permitted, provided the original author(s) and the copyright owner(s) are credited and that the original publication in this journal is cited, in accordance with accepted academic practice. No use, distribution or reproduction is permitted which does not comply with these terms.
*Correspondence: Szymon Łukaszyk, c3p5bW9uQHBhdGVudC5wbA==