Cosmological Relaxation of the Electroweak Scale

Transcription

1 the Relaxion Cosmological Relaxation of the Electroweak Scale with P. Graham and D. E. Kaplan arxiv:

2 The Hierarchy Problem The Higgs mass in the standard model is sensitive to the ultraviolet. Two approaches to explain: New symmetry or new dynamics realized at the electroweak scale. (SUSY, composite Higgs, EOFT) An anthropic explanation for fine tuning of ultraviolet parameters. (Multiverse)

3 We Propose: A Dynamical Solution Higgs mass-squared promoted to a field. The field evolves in time in the early universe. The mass-squared relaxes to a small negative value. The electroweak symmetry breaking stops the time-dependence. The small electroweak scale is fixed until today.

4 Elements of a Dynamical Solution Initial Formation State after millions of years of erosion Time evolution important Dissipation - eroded sand needs to go somewhere Every point along the way is stable - just that the flat surface is much more stable

5 Caveats The solution: is only technically natural. requires large field excursions (larger than the scale that cuts off loops). requires a very long period of inflation. can only push the cutoff up to 108 GeV.

6 Simplest Model Standard Model plus QCD axion L ( M 2 + g ) h 2 + gm 2 + g f Gµ Gµ M cuts off SM loops. Continuous shift symmetry broken completely by g. The axion here is non-compact. (The Abbott model with a coupling to the Higgs & QCD)

7 Simplest Model Standard Model plus QCD axion L ( M 2 + g ) h 2 + gm 2 + g cos f Continuous shift symmetry broken to discrete by nonperturbative effects. Conservative effective field theory regime:. M 2 g g (Assuming expansion of in powers of ) V (g ) M 2

8 Chronology V ( ) Take initial value such that m 2 h > 0. During inflation, slow-rolls, scanning physical Higgs mass. hits value where m 2 h ~ crosses zero. Barriers grow until rolling has stopped. Key: Barriers grow because they depend on the Higgs vev.

9 Higgs vev and the Periodic Potential Barrier height (axion potential) can be approximated in the chiral Lagrangian (2 flavors): V axion Around the normal EW scale: f 4 cos f 4 f 2 m 2 min(mu,m d ) m u + m d m 2 / (y u + y d )hhi Barrier height grows with the Higgs vev.

10 Parameter Requirements φ stops rolling and Higgs vev stops growing when slope turns (gm cos ( /f)) 0 or gm 2 f MeV fixed parameters changes with Higgs vev gm 2 f f 2 µ(y u + y d )hhi

11 Parameter Requirements 1) Vacuum energy density during inflation >M 4 H infl > M 2 M pl 2) Classical rolling dominates: H infl >H infl H 3 infl <gm 2 Plugging in for g, and using 1) and 2): M 6 < 4 M 3 pl f

12 Bound on cutoff GeV 1/6 M<10 7 GeV f However,... gm 2 f 4 QCD ' /2 Prediction: d n ' few e cm

13 Solve Strong CP (1) Usual solutions don t quite work. Dynamical one -- Drop the slope: L ( M 2 + g ) h 2 + apple 2 + gm cos f inflaton - drops at end of inflation gm 2 ' apple 2 gm 2 f 4 H infl > 1 M 2 2 M pl Hinfl 3 < 1 gm 2

14 Bound on cutoff! M 6 < M 3 pl f or M<30 TeV GeV f 1 6

15 Quantum vs. Classical evolution tiny fraction here most patches here slope drop most patches here tiny fraction in AdS If we remove this constraint, upper bound on Hubble comes from requiring barriers to form: H infl <

16 Weaker bound on cutoff! M 2 < 1 2 Mpl or M<1000 TeV

17 Solve Strong CP (2) (Model 2) Use a different strong group and couple to. G 0µ G0 µ The Higgs must change the barrier heights: Add fermions L, N L c,n c SU(3) L m L LL c + m N NN c + yhln c +ỹh L c N Require Higgs vev to be dominant contribution to mn Radiative naturalness => ml < 600 GeV ml > 250 GeV from LHC

18 Bound on cutoff (Model 2) M<( 4 M pl 3 ) 1 7 M f 1 7 or M< GeV f 0 30 GeV 3 7 yỹ GeV m L 1 7 M f 1 7 Bounds from Higgs decays, EWP Constraints weaker due to loops

19 End of Roll V ( ) (a) classical evolution (b) quantum fluctuations (c) tunnelling classical plus quantum fluctuations (d) Need to end up in vacua that lives longer than the age of the universe since reheating

20 Inflation To achieved the relaxed value, inflation has to last long enough: H infl V H 2 infl N gm2 H 2 infl N We require: M 2 & g N & H2 infl g , (Model 1,2 saturated)

21 Inflation Single field: V ( )=m 2 2 N = Z Hdt Z H V d 2 i M 2 pl Classical rolling: H infl <H infl m 2 i M 3 pl < 1 V ( i ) < M 4 pl N N< Mpl M 4 ( ) N & H2 infl g 2 M<10 5, GeV Reheating requires additional dynamics (e.g., hybrid)

22 Observables QCD model: Small parameter space (Rel)axion: May be dark matter, with different abundance prediction from vacuum misalignment. Observable neutron EDM favored. Coupling to the Higgs: (tiny) New force experiments Background oscillations of SM mass scales (if DM) Low-scale inflation (no primordial tensor modes in the CMB) Low energy precision measurements to test this solution to the hierarchy problem!

23 Observables non-qcd model: weak-scale physics (Rel)Axion: Still be dark matter, with different abundance prediction from vacuum misalignment, as well as mass prediction/couplings Fermions with electroweak quantum numbers Coupling to the Higgs: New force experiments Oscillations of SM mass scales, e.g. m e (if DM) Low-scale inflation (no primordial tensor modes in the CMB) Low energy precision measurements to test this solution to the hierarchy problem!

24 Relaxion Conditions L ( M 2 + g ) h 2 + gm 2 + g cos f Self-organized criticality? Dissipation - Dynamical evolution of Higgs mass (field) must stop. Hubble friction. Self-similarity - Cutoff-dependent quantum corrections will choose an arbitrary point where the Higgs mass is cancelled. Periodic axion. Higgs back-reaction - EWSB must stop the evolution at the appropriate value. Yukawa couplings. Long time period - There must be a sufficiently long time period during the early universe for scanning. Inflation.

25 To Do Phenomenology: Dark matter / cosmological predictions Collider predictions New forces New low-energy experimental ideas (CASPEr) UV completion (axion monodromy?) Better Inflation models Better models/higher cutoff