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| Format: | Preprint |
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2026
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| Online Access: | https://arxiv.org/abs/2606.01296 |
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| _version_ | 1866916071949205504 |
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| author | Keranen, Ville |
| author_facet | Keranen, Ville |
| contents | We develop the Boltzmann--Wasserstein (BW) distance, a temperature-dependent metric on the space of quantum theories defined as the optimal $W_2$ distance between Boltzmann-weighted energy spectra. For semiclassical theories differing by a small entropy shift, the normalised BW distance collapses to a squared horizon-area comparator, $\tilde{\mathcal{W}}^2 \approx (δA/4G)^2/8$, with the two areas evaluated at equal energy. When the Hamiltonians of the theories differ by an operator $V$, then the BW distance equals a time-averaged thermal two-point function of $V$; for primary perturbations where this vanishes by conformal invariance, a four-point representation appears at the next order. Both formulas arise from a similar gravitational picture but capture complementary content. The Schwinger--Keldysh wormhole that determines $C_{\max}$ -- two Euclidean caps sharing a single horizon, joined by a Lorentzian segment that adiabatically interpolates between the two theories -- sees only the rearrangement of the spectrum. The perturbative two-point formula computes the genuinely quantum correction sensitive to the eigenvectors of the perturbation, invisible to the classical gravity saddle. The Lorentzian part of the wormhole is essential for the construction. We work out two examples -- two BTZ black holes with different cosmological constants and a $T\bar{T}$ deformation of BTZ. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2606_01296 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Notes on Wasserstein distance and wormholes Keranen, Ville High Energy Physics - Theory We develop the Boltzmann--Wasserstein (BW) distance, a temperature-dependent metric on the space of quantum theories defined as the optimal $W_2$ distance between Boltzmann-weighted energy spectra. For semiclassical theories differing by a small entropy shift, the normalised BW distance collapses to a squared horizon-area comparator, $\tilde{\mathcal{W}}^2 \approx (δA/4G)^2/8$, with the two areas evaluated at equal energy. When the Hamiltonians of the theories differ by an operator $V$, then the BW distance equals a time-averaged thermal two-point function of $V$; for primary perturbations where this vanishes by conformal invariance, a four-point representation appears at the next order. Both formulas arise from a similar gravitational picture but capture complementary content. The Schwinger--Keldysh wormhole that determines $C_{\max}$ -- two Euclidean caps sharing a single horizon, joined by a Lorentzian segment that adiabatically interpolates between the two theories -- sees only the rearrangement of the spectrum. The perturbative two-point formula computes the genuinely quantum correction sensitive to the eigenvectors of the perturbation, invisible to the classical gravity saddle. The Lorentzian part of the wormhole is essential for the construction. We work out two examples -- two BTZ black holes with different cosmological constants and a $T\bar{T}$ deformation of BTZ. |
| title | Notes on Wasserstein distance and wormholes |
| topic | High Energy Physics - Theory |
| url | https://arxiv.org/abs/2606.01296 |