Simulating Black Hole Radiation with Quantum Spin Chains

New research demonstrates a pathway to detect analogue Hawking radiation using a quantum sensor embedded within a chiral spin chain, offering a novel platform for studying quantum gravity effects.
![The study demonstrates that tau pair spin correlations exhibit entanglement-quantified by [latex]\mathcal{C}>0[/latex]-and nonlocality-signaled by [latex]\mathfrak{m}\_{12}>1[/latex]-as functions of center of mass energy and scattering angle, revealing intrinsic quantum properties within particle interactions.](https://arxiv.org/html/2602.03960v1/m12.png)
![Electron-mediated nuclear spin-spin interactions induce a decoherence time [latex]T_2[/latex] that is demonstrably sensitive to the electronic correlation length ξ, with calculations-using parameters including a flip angle of 75° and a dissipation parameter set to zero-showing [latex]T_2 \approx 145\,\rm{s}[/latex] for [latex]\xi = 2.5\rm{a}[/latex], a value corroborated by experimental measurements in YBa2Cu3O7-δ and aligning with prior theoretical work, as evidenced by simulations performed on a 200x200 lattice of 40,000 spins.](https://arxiv.org/html/2602.02732v1/x9.png)
![The study demonstrates consistent convergence on challenging 20-dimensional benchmarks-Ackley, Rastrigin, and Schwefel functions-achieved through an initialization of 10 points, iterative proposal of 10 candidates, and averaging across 10 independent runs, as evidenced by decreasing objective values and minimized feature-space distance to the global optimum-[latex] \min ||x - x^*|| [/latex]-across all tested functions.](https://arxiv.org/html/2602.03319v1/img/math/math_res.png)
![The reflection probability [latex]R(\omega)[/latex] of a charged Bardeen black hole is demonstrably modulated by the parameters α and β, with increasing α suppressing reflection and increasing β enhancing it-a complementary behavior observed across variations of [latex]\alpha = 0.1, 0.2, 0.3[/latex] at fixed [latex]\beta/M = 1[/latex] and [latex]\beta = 1, 1.5, 2[/latex] at fixed [latex]\alpha = 0.2[/latex], given parameters [latex]M = 1[/latex], [latex]Q = 1[/latex], and [latex]q = 0.1[/latex].](https://arxiv.org/html/2602.02586v1/x27.png)
![The Page curve for a non-extremal Kerr [latex]AdS_4[/latex] black hole-shown as a solid line-reveals how the inclusion of an island-represented by a blue line-alters the calculation of entanglement entropy compared to its omission, depicted in red.](https://arxiv.org/html/2602.03366v1/x4.png)

![The metric function [latex]f(r)[/latex] reveals a nuanced relationship between horizon configurations and spacetime geometry in charged Hayward black holes, demonstrating how parameters such as [latex]g/M[/latex], α, and [latex]\beta/M[/latex] dictate transitions from standard Schwarzschild horizons to regular black holes with two horizons, non-extremal cases exhibiting dual horizon crossings, and ultimately, to scenarios involving extremal tangencies or even naked singularities-all while reflecting the non-flat nature of charged de Sitter spacetimes through asymptotic behavior of [latex]f(\in fty) = 1 - \alpha < 1[/latex].](https://arxiv.org/html/2602.02621v1/x1.png)
![The study demonstrates how approximations to the effective potential-ranging from full calculations using [latex]CosmoTransitions[/latex] to those neglecting Daisy contributions-systematically shift the computed bounce action [latex]S\_{3}(T)[/latex], with results benchmarked against a fit from prior work to polynomial potentials, thereby revealing the sensitivity of cosmological phase transitions to the details of potential calculations.](https://arxiv.org/html/2602.02829v1/x6.png)