The Last Equation

WE FOUND IT.

There is nothing underneath.

Z=DgDψ  eiS[g,ψ]/Z = \int \mathcal{D}g\,\mathcal{D}\psi\; e^{\,iS[g,\psi]/\hbar}
(37)

Everything else follows.

biology

chemistry

atoms

particles

fields

geometry

?

17 symbols

Fig. 1. The two descriptions, as of the twentieth century. Each is complete on its own side. Neither survives the other's regime.

Gμν+Λgμν=8πGc4TμνG_{\mu\nu} + \Lambda g_{\mu\nu} = \frac{8\pi G}{c^{4}}\,T_{\mu\nu}
(3)

Einstein, 1915. Gravity.

L=14FμνFμν+iψˉγμDμψ+ψˉiyijψjϕ+h.c.+Dμϕ2V(ϕ)\begin{aligned}\mathcal{L} = {}& -\tfrac{1}{4}F_{\mu\nu}F^{\mu\nu} + i\bar{\psi}\gamma^{\mu}D_{\mu}\psi \\ &+ \bar{\psi}_i\, y_{ij}\, \psi_j\, \phi + \text{h.c.} + |D_\mu\phi|^{2} - V(\phi)\end{aligned}
(11)

sign conventions as in [21]; 19 parameters, all measured, none explained. yet.

The Standard Model, 1970s. Everything else, except gravity.

Gμν+Λgμν=8πGc4Tμν,LSMG_{\mu\nu} + \Lambda g_{\mu\nu} = \frac{8\pi G}{c^{4}}\,T_{\mu\nu}\,,\qquad \mathcal{L}_{\mathrm{SM}}
S[g,ψ]S[g,\psi]

Fig. 2b. Compression. Eqs. (3) and (11) enter as the low-energy limit of the action in Eq. (37). What comes out the other side is shorter.

Fig. 4. The same diagram. The gap is not bridged. It is absent.

Low-energy limit
Newtonian gravityrecovered
general relativity, Eq. (3)recovered
Standard Model, Eq. (11)recovered
Lorentz invariancepreserved
black-hole entropyrecovered
Hawking temperaturerecovered
free parameters0
unexplained residual0

Derivation status: closed.

Nothing special happened.

We expected something beautiful. It wasn't.

We expected symmetry. Not particularly.

We expected the constants to reveal themselves as inevitable. They did.

We expected the universe to become less strange. It became stranger in fewer symbols.

Don't believe us.

Pick something.

An electron.

(iγμμm)ψ=0(i\gamma^{\mu}\partial_{\mu} - m)\psi = 0

Dirac, 1928. Spin ½ and antimatter fall out. The magnetic moment comes out as exactly g = 2.

ae=g22=α2π+a_e = \frac{g-2}{2} = \frac{\alpha}{2\pi} + \cdots

Schwinger, 1948. The first correction. Measured and calculated to twelve digits since. They agree.

from Eq. (37), fermion sector, App. B: me and e are fixed by the spectrum. no input.

ObservedDerived
charge  −e−e
spin  ½ ħ½ ħ
ae  0.001 159 652 1810.001 159 652 181
mass  0.510 998 95 MeV/c² (measured)0.510 998 95 MeV/c² (no input)

residual: 0

A falling apple.

F=GMmr2g=GMR2=9.81 m/s2F = \frac{GMm}{r^{2}}\qquad g = \frac{GM_{\oplus}}{R_{\oplus}^{2}} = 9.81\ \mathrm{m/s^{2}}

Newton, 1687. Good to one part in a billion in an orchard.

d2xμdτ2+Γαβμdxαdτdxβdτ=0g00(1+2Φ/c2)\begin{gathered}\frac{d^{2}x^{\mu}}{d\tau^{2}} + \Gamma^{\mu}_{\alpha\beta}\,\frac{dx^{\alpha}}{d\tau}\,\frac{dx^{\beta}}{d\tau} = 0 \\[.4em] g_{00} \approx -\left(1 + 2\Phi/c^{2}\right)\end{gathered}

Einstein, 1915. The apple is not pulled. It follows the straightest line available. In the weak field, the straightest line is Newton's.

Eq. (37) → Eq. (3) as ħ → 0 (App. A). then v ≪ c. nothing to adjust.

ObservedDerived
acceleration  9.81 m/s²9.81 m/s²
inertial mass = gravitational massexact
clocks run slow near the ground, 1.1 × 10−16 per metre1.1 × 10−16 per metre
the apple's quantum statedecoheres in 10−20 s. as observed.

residual: 0

A black hole.

rs=2GMc2SBH=kBc3A4GTH=c38πGMkBr_s = \frac{2GM}{c^{2}}\qquad S_{\mathrm{BH}} = \frac{k_B c^{3} A}{4G\hbar}\qquad T_H = \frac{\hbar c^{3}}{8\pi G M k_B}

Schwarzschild 1916, Bekenstein 1973, Hawking 1975. A horizon, an entropy that scales with area rather than volume, and a temperature. Three results that did not fit in one theory.

horizonr = 0pastout

Penrose, 1965. Light cones tip over at the horizon. In Eq. (3) the top edge is where the description terminates.

in Eq. (37) the top edge is not there. the geometry is smooth. checked: App. C, three times.

ObservedDerived
entropy ∝ areaentropy ∝ area
temperature  THrecovered
informationconserved
singularityabsent

residual: 0

The early universe.

H2=8πG3ρkc2a2+Λc23H^{2} = \frac{8\pi G}{3}\,\rho - \frac{kc^{2}}{a^{2}} + \frac{\Lambda c^{2}}{3}

Friedmann, 1922. The universe expands. Run it backwards and it gets hot.

TCMB=2.7255 KYp0.245ns0.965T_{\mathrm{CMB}} = 2.7255\ \mathrm{K}\qquad Y_p \approx 0.245\qquad n_s \approx 0.965

Penzias and Wilson 1965; primordial helium; the tilt of the first fluctuations. Three numbers the sky gives you for free.

initial state: the unique regular solution of Eq. (37) (App. D). no tuning. no inflaton put in by hand.

ObservedDerived
helium fraction  0.2450.245
background temperature  2.7255 K2.7255 K
spectral index  0.9650.965
flatness  Ω = 1.001

residual: 0

Empty space.

ρvac(QFT)10113 J/m3ρvac(obs)5×1010 J/m3\rho_{\mathrm{vac}}^{(\mathrm{QFT})} \sim 10^{113}\ \mathrm{J/m^{3}}\qquad \rho_{\mathrm{vac}}^{(\mathrm{obs})} \approx 5\times 10^{-10}\ \mathrm{J/m^{3}}

Weinberg, 1989. The worst prediction in the history of physics: off by about 10122. Empty space should weigh enough to end the universe. It doesn't.

FA=π2c240d4Λ1.1×1052 m2\frac{F}{A} = -\frac{\pi^{2}\hbar c}{240\,d^{4}}\qquad \Lambda \approx 1.1\times 10^{-52}\ \mathrm{m^{-2}}

Casimir, 1948. The vacuum pushes on two plates. It is not nothing. The measured Λ is the small number the vacuum actually weighs.

the 10122 cancels identically. not fine-tuned: forced. App. C, Eq. (C.9).

ObservedDerived
Casimir forcerecovered
Λ  1.1 × 10−52 m−21.1 × 10−52 m−2
vacuum stabilitystable
the 101220

residual: 0

You.

masscompatible
energycompatible
electromagnetic statecompatible
chemical statecompatible
neural activitycompatible
observerincluded

The theory does not require an exception for the person reading it.

Sorry.

References

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  2. M. Planck, Ueber das Gesetz der Energieverteilung im Normalspectrum, Ann. Phys. 4 (1901) 553.
  3. A. Einstein, Zur Elektrodynamik bewegter Körper, Ann. Phys. 17 (1905) 891.
  4. N. Bohr, On the constitution of atoms and molecules, Phil. Mag. 26 (1913) 1.
  5. A. Einstein, Die Feldgleichungen der Gravitation, Sitzungsber. Preuss. Akad. Wiss. (1915) 844.
  6. K. Schwarzschild, Über das Gravitationsfeld eines Massenpunktes nach der Einsteinschen Theorie, Sitzungsber. Preuss. Akad. Wiss. (1916) 189.
  7. E. Noether, Invariante Variationsprobleme, Nachr. Ges. Wiss. Göttingen (1918) 235.
  8. A. Friedmann, Über die Krümmung des Raumes, Z. Phys. 10 (1922) 377.
  9. W. Heisenberg, Über quantentheoretische Umdeutung kinematischer und mechanischer Beziehungen, Z. Phys. 33 (1925) 879.
  10. W. Pauli, Über den Zusammenhang des Abschlusses der Elektronengruppen im Atom mit der Komplexstruktur der Spektren, Z. Phys. 31 (1925) 765.
  11. E. Schrödinger, Quantisierung als Eigenwertproblem, Ann. Phys. 79 (1926) 361.
  12. P. A. M. Dirac, The quantum theory of the electron, Proc. R. Soc. A 117 (1928) 610.
  13. E. Fermi, Versuch einer Theorie der β-Strahlen, Z. Phys. 88 (1934) 161.
  14. H. B. G. Casimir, On the attraction between two perfectly conducting plates, Proc. K. Ned. Akad. Wet. 51 (1948) 793.
  15. J. Schwinger, On quantum-electrodynamics and the magnetic moment of the electron, Phys. Rev. 73 (1948) 416.
  16. R. P. Feynman, Space-time approach to non-relativistic quantum mechanics, Rev. Mod. Phys. 20 (1948) 367.
  17. C. N. Yang, R. L. Mills, Conservation of isotopic spin and isotopic gauge invariance, Phys. Rev. 96 (1954) 191.
  18. S. L. Glashow, Partial-symmetries of weak interactions, Nucl. Phys. 22 (1961) 579.
  19. P. W. Higgs, Broken symmetries and the masses of gauge bosons, Phys. Rev. Lett. 13 (1964) 508.
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  21. M. Gell-Mann, A schematic model of baryons and mesons, Phys. Lett. 8 (1964) 214.
  22. R. Penrose, Gravitational collapse and space-time singularities, Phys. Rev. Lett. 14 (1965) 57.
  23. A. A. Penzias, R. W. Wilson, A measurement of excess antenna temperature at 4080 Mc/s, Astrophys. J. 142 (1965) 419.
  24. S. Weinberg, A model of leptons, Phys. Rev. Lett. 19 (1967) 1264.
  25. B. S. DeWitt, Quantum theory of gravity. I. The canonical theory, Phys. Rev. 160 (1967) 1113.
  26. S. Coleman, J. Mandula, All possible symmetries of the S matrix, Phys. Rev. 159 (1967) 1251.
  27. J. D. Bekenstein, Black holes and entropy, Phys. Rev. D 7 (1973) 2333.
  28. D. J. Gross, F. Wilczek, Ultraviolet behavior of non-abelian gauge theories, Phys. Rev. Lett. 30 (1973) 1343.
  29. H. D. Politzer, Reliable perturbative results for strong interactions?, Phys. Rev. Lett. 30 (1973) 1346.
  30. K. G. Wilson, Confinement of quarks, Phys. Rev. D 10 (1974) 2445.
  31. S. W. Hawking, Particle creation by black holes, Commun. Math. Phys. 43 (1975) 199.
  32. W. G. Unruh, Notes on black-hole evaporation, Phys. Rev. D 14 (1976) 870.
  33. A. H. Guth, Inflationary universe: a possible solution to the horizon and flatness problems, Phys. Rev. D 23 (1981) 347.
  34. M. B. Green, J. H. Schwarz, Anomaly cancellations in supersymmetric D = 10 gauge theory and superstring theory, Phys. Lett. B 149 (1984) 117.
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  37. G. 't Hooft, Dimensional reduction in quantum gravity, arXiv:gr-qc/9310026 (1993).
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  40. J. Maldacena, The large N limit of superconformal field theories and supergravity, Adv. Theor. Math. Phys. 2 (1998) 231.
  41. [41] This work.

Acknowledgments

We thank everyone who spent a lifetime getting us almost here.

We also wanted thelastequation.com. Someone got there first. They can keep it.

We got the equation.

Correspondence: none required.

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Well.

Almost everything.

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Fig. 9. Cancelling a subscription, 2026. Fourteen steps. Not derivable from Eq. (37).

We derived the underlying structure of the universe.
This is apparently still beyond us.

Some futures
are worth building.

Fundamental physics has been handled.
The rest, however, could use you.

Nothing on this page needed to be invented until Eq. (37).
The equations before it are real. The black-hole results are real. The cosmological numbers are real. The references are real.
Eq. (37) is where physics currently stops: the general form is known; the action is not.
That blank is real too.

Keep scrolling. Surely the meaning of everything is just below the footer.

You actually kept scrolling.

We like that about you.

No final answer found down here either. But that curiosity seems good.

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