Ｍ ultiverse and the Naturalness Problem

1. Ｍultiverseand the Naturalness Problem Hikaru KAWAI 2012/ 12/ 4 at Osaka University

2. Contents I will discuss the low energy effective action of quantum gravity and the possibility of solving the naturalness problem by using it. 1. Low energy effective theory of quantum gravity / string theory Wave function of the multiverse 3. Naturalness and Big Fix

3. 1. Low energy effective theoryof quantum gravity / string theory

4. Low energy effective theory of quantum gravity / string theory is obtained by integrating out the short distance physics. Because of the symmetry, it should be Is that all? Usually, action is additive. why not (Sugawara ‘82 )

5. By replacing each factor to its expectation value as is usually done in the mean field approximation, we have An observer finds only a local field theory. The coupling constants are determined by the state or the history of the universe. Actually, in quantum gravity or matrix model, there are some mechanisms that the low energy effective action becomes “multi local action” : local operators

6. Multi local action from wormhole (1)Coleman ‘88 Consider Euclidean path integral which involves the summation over topologies, Then there should be a wormhole-like configuration in which a thin tube connects two points on the universe. Here, the two points may belong to either the same universe or the different universe. If we see such configuration from the side of the large universe(s), it looks like two small punctures. But the effect of a small puncture is equivalent to an insert ion of a local operator.

7. Multi local action from wormhole (2) Therefore, a wormhole contribute to the path integral can be expressed as Summing over the number of wormholes, we have Thus wormholes contribute to the path integral is bifurcated wormholes ⇒ cubic terms, quartic terms, …

8. Multi local action from wormhole (3) The effective action becomes a factorized form By introducing the Laplace transform we can express the path integral as Coupling constants are not merely constant but to be integrated.

9. Multi local action from IIB matrix model (1) Asano , Tsuchiya and HK Various possibilities for the emergence of space-time • Aμ as the space-time coordinates mutually commuting Aμ⇒space-time (2) Aμ as non-commutative space-time non-commutative Aμ ⇒NC space-time (3) Aμ as derivatives

10. Multi local action from IIB matrix model (2) Hanada, HK, Kimura If the covariant derivative on a manifold acts on the regular representation field, its action can be decomposed into D scalars. : regular representation field on D-dim manifold M r : regular representation : the Clebsh-Gordan coefficients embedding in ten matrices

11. Multi local action from IIB matrix model (3) We can calculate the low energy effective action by using the background field method, and we obtain in the Lorentzian space time We consider Lorentzian theory from now on.

12. We have seen the effective action of quantum gravity/string is given by the coupling constants are determined by the state More precisely, the path integral is given by Coupling constants are not merely constant but to be integrated.

13. the question What physics does the multi local action describe? Are some special values of the coupling constants favored? (Naturalness problem) In the following, as an ad hoc assumption, we postulate the probabilistic interpretation for the multiverse wave function.

14. 2. Wave function of the multiverse

15. Each block represents a large universe. the multiverse Okada, HK Multiverse that includes indefinite number of large universes appears naturally in quantum gravity / string theory. ・ ・ matrix model quantum gravity

16. Wave Function of the multiverse The multiverse sate is a superposition of N-verses.

17. Probabilistic interpretation We assume a kind of probabilistic interpretation: represents the probability of finding N universes with size and the coupling constants

18. Probability distribution of is chosen in such a way that is maximized, irrespectively of

19. Wave function of a universe (1) We assume that the universe emerges with a small size ε with probability amplitude .

20. Wave function of a universe (2) is a superposition of the universe with various age, + + +… gives the probability of finding a universe of age .

21. Wave function of a universe (3) infrared cutoff We introduce an infrared cutoff for the size of universes. ∞ finite ceases to exist or bounces back

22. We have seen the coupling constants are chosen in such a way that the lifetime of the universe becomes maximum. the question What values of the coupling constants make the lifetime maximum?

23. 3. Naturalness and Big Fix

24. Cosmological constant What value of Λ maximizes the life time of the universe? For simplicity, we assume the S3 topology. Λ～curvature～energy density The cosmological constant in the far future is predicted to be very small. (extremely small)

25. The other couplings (Big Fix) (1) The exponent is divergent, and regulated by the IR cutoff : assuming all matters decay to radiation BIG FIX are determined in such a way that the entropy of the universe at the late stages is maximized.

26. The other couplings (Big Fix) (2) Quantities like are almost determined by the low energy physics. ⇒ If the low energy physics and the cosmological evolution is understood,we can calculate theoretically, and all of the renormalized couplings are in principle determined by maximizing it. However, some of the couplings can be determined without knowing the detail of the cosmological evolution. case 1. Symmetry example Nielsen, Ninomiya 1. It becomes important only after the QCD phase transition. 2. The effective action at QCD scale is invariant under ⇒　　 is minimum or maximum at at least locally.

27. The other couplings (Big Fix) (3) case 2. End point example Higgs coupling 1. Some couplings are bounded. 2. The entropy of the universe can be monotonic in them. ⇒ The coupling is fixed to the end point. A scenario for . Fixvhto the observed value and vary assuming the leptogenesis ⇒ sphaleron process ⇒ baryon number ⇒ radiation from baryon decay ⇒ Higgs mass is at stability bound, the stability bound. without SUSY

28. The other couplings (Big Fix) (4) non-trivial exampleQCD coupling or proton mass We assume that dark matters decay faster than protons,. If the curvature term balances with matter (protons) before the proton decay, the universe bounce back when the protons decay. The earlier the protons decay, the less Crad remains. Crad is maximized if the curvature term balances with the energy density when the protons decay.

29. The other couplings (Big Fix) (5) (cont’d) The curvature term balances with the energy density when the protons decay. ⇒ ⇒ Cf. in our universe Reasonable? ⇒

30. 4. Summary

31. Summary In the quantum gravity or string theory, the low energy effective action is not a simple local one but the multi-local one. The multiverse naturally appears, and it becomes a superposition of states with various values of the coupling constants. The coupling constants are fixed is such a way that the lifetime of the universe is maximized. For example the cosmological constant in the far future is predicted to be very small: . The Higgs mass is predicted at its lower bound. Future problems Some scenario other than the probabilistic interpretation. Comparison of different dimensional space-time? Generalization to the landscape?

32. Appendix A. Partition function

33. We consider the partition function of the multiverse:

34. the question How to evaluate the partition function for a single universe:

35. The path integral for a universe If the initial and final states are given, the path integral is well defined. Question: Is there a natural choice for them?

36. Initial state For the initial state, we assume that the universe emerges with a small size ε.

37. Final state: case 1 For the final state, we have two possibilities. The universe shrinks back. We assume the final state is finite The partition function

38. Final state: case 2 (1) The universe keeps expanding. It is not clear how to define the path integral for the universe: ∞ If we take , the path integral includes the history of the universe for the corresponding time . Therefore as a trial we take

39. Final state: case 2 (2) Then the partition function becomes If , the result does not depend on except for the phase which should be there in the classical limit: ad hoc assumption

40. Under this ad hoc assumption, we have the partition function for a universe ∞ finite Then the integration for the multiverse partition has an infinite peak at , which again indicates that the cosmological constant at the late stages of the universe vanishes.

41. Big Fix For simplicity we assume the topology of the space and that all matters decay to radiation at the late stages. Then the multiverse partition function is given by BIG FIX are determined in such a way that the entropy at the late stages of the universe is maximized.