1. 1 Stefan Antusch based on collaborations with: K. Dutta, M. Bastero-Gil, J.P. Baumann, V. Domcke, S.F. King, and P.M. Kostka Particle Physics Models of Inflation in Supergravity: New Developments Max-Planck-Institut für Physik (Werner-Heisenberg-Institut) Talk at COSMO/CosPA 2010, September 30th, Tokyo, Japan

2. Stefan Antusch MPI für Physik (Munich) 2 Inflation = Era of accelerated expansion in the very early universe picture from WMAP website

3. Stefan Antusch MPI für Physik (Munich) Outline ‣ New possible solution to the η-problem in SUGRA inflation: Heisenberg symmetry with stabilised modulus ‣ New class of models, very suitable for applying symmetry solutions to the η-problem: Tribrid Inflation ‣ New possibile connection to particle physics (application of ‘Tribrid Inflation’): Unified Matter Inflation in SUSY GUTs 3

4. Stefan Antusch MPI für Physik (Munich) Inflationary epoch in the early universe ‣ Requirements for “slow roll“ inflation → “Slow roll parameters” small: ε, |η|, ξ << 1, V ~ V 0 dominates “slope of V” “inflaton mass” 4

5. Stefan Antusch MPI für Physik (Munich) The η-problem ‣ Challenge for realising inflation: Flat enough potential, Generic (effective field theory) In supergravity (with K = ϕ * ϕ and V 0 from F-term) 5 V ⊂ E.J Copeland, A.R. Liddle, D.H. Lyth, E.D. Stewart, D. Wands ('94) with

6. Stefan Antusch MPI für Physik (Munich) Approaches to solve the η-problem: 3 strategies ‣ Expansion of K in fields/M P : ‣ 'Shift' symmetry: ‣ Heisenberg symmetry: 6 requires tuning of parameters! (at 1%-level) solves the η-problem for | ϕ | by symmetry! T: 'modulus field’ → has to be stabilised Gaillard, Murayama, Olive ('95), S.A., Bastero-Gil, Dutta, King, Kostka (’08,’09) protects Im[ ϕ ] from obtaining a SUGRA mass by symmetry! (used in many works...)

7. Stefan Antusch MPI für Physik (Munich) Approaches to solve the η-problem: 3 strategies ‣ Expansion of K in fields/M P : ‣ 'Shift' symmetry: ‣ Heisenberg symmetry: 7 Remark: Symmetries have to be broken to allow for slope of V( ϕ )! → approximate symmetries

8. Stefan Antusch MPI für Physik (Munich) Heisenberg symmetry solution to the η-problem ‣ Example for K: → Field X: Provides the vacuum energy V 0 by |F X | 2 during inflation → Consider suitable W with (i) W inf = 0, W ϕ = 0 during inflation and (ii) which yields a tree-level ϕ -flat potential in global SUSY limit → Parameter κ ρ : Couples ρ to V 0 8 K invariant under Heisenberg symmetry S.A., M. Bastero-Gil, K. Dutta, S. F. King, P. M. Kostka ('08) } Example: No-scale form; More general: f(ρ)

9. Stefan Antusch MPI für Physik (Munich) Heisenberg symmetry solution to the η-problem ‣ Calculate L kin and V F : In the the ( ϕ,ρ)-basis: no kinetic mixing between ϕ and ρ The F-term scalar potential depends only on ρ (and not on ϕ ) 9 → η-problem solved!→ ρ can be stabilsed by large V 0

10. Stefan Antusch MPI für Physik (Munich) 10 S.A., M. Bastero-Gil, K. Dutta, S. F. King, P. M. Kostka ('08) Modulus field ρ gets stabilized quickly and allows for >> 60 e-folds of inflation! ϕ ρ, ϕ With V = V tree + V loop

11. Stefan Antusch MPI für Physik (Munich) A new class of inflation models: Tribrid Inflation ‣ Simple example (singlet fields, global SUSY to start with): Three fields, X, H and Φ relevant for the model → “Tribrid Inflation“ 11 Driving superfield Waterfall superfield Inflaton superfield First model of this class in: S.A., Bastero-Gil, King, Shafi (’04) “Tribrid Inflation” in SUGRA: S.A., Dutta, Kostka (’09); S.A., M. Bastero-Gil, K. Dutta, S. F. King, P. M. Kostka ('08)

12. Stefan Antusch MPI für Physik (Munich) A new class of inflation models: Tribrid inflation ‣ Simple example (singlet fields, global SUSY to start with): 12 Driving superfield (its F-term generates the potential for H and provides the vacuum energy V 0 ; During and after inflation: = 0.) V(H,Φ=0) } V0V0 |F X | 2 ⇒

13. Stefan Antusch MPI für Physik (Munich) A new class of inflation models: Tribrid inflation ‣ Simple example (singlet fields, global SUSY to start with): Driving superfield (its F-term generates the potential for H and provides the vacuum energy V 0 ; During and after inflation: = 0.) Waterfall superfield (contains the “waterfall field” (e.g. GUT- or Flavour-Higgs field) that ends inflation by a 2 nd order phase transition and gives mass to ϕ after inflation) V(H,Φ=0) } V0V0 13

14. Stefan Antusch MPI für Physik (Munich) A new class of inflation models: Tribrid inflation ‣ Simple example (singlet fields, global SUSY to start with): 14 Inflaton superfield (contains the inflaton field as scalar component; For > ϕ crit it stabilises H at = 0) V(H,Φ=0) } V0V0

15. Stefan Antusch MPI für Physik (Munich) A new class of inflation models: Tribrid inflation ‣ Simple example (singlet fields, global SUSY to start with): 15 Inflaton superfield (contains the inflaton field as scalar component; For > ϕ crit it stabilises H at = 0) V(H,Φ=0) } V0V0 → Inflaton candidates are e.g.: i) Right-handed Sneutrino (in ‘Tribrid Inflation’-type scenario): S.A., Bastero-Gil, King, Shafi (‘04) ii) Unified Matter Sparticle (16 of SO(10) SUSY GUT) S.A., Bastero-Gil, Baumann, Dutta, King, Kostka (‘10)

16. Stefan Antusch MPI für Physik (Munich) A new class of inflation models: Tribrid inflation ‣ Simple example (singlet fields, global SUSY to start with): 16 During inflation: Inflaton superfield (contains the inflaton field as scalar component; For > ϕ crit it stabilises H at = 0)

17. Stefan Antusch MPI für Physik (Munich) A new class of inflation models: Tribrid inflation ‣ Simple example (singlet fields, global SUSY to start with): 17 End of inflation: Inflaton superfield (contains the inflaton field as scalar component; For > ϕ crit it stabilises H at = 0)

18. Stefan Antusch MPI für Physik (Munich) A new class of inflation models: Tribrid inflation ‣ Simple example (singlet fields, global SUSY to start with): 18 After inflation: Inflaton superfield (contains the inflaton field as scalar component; For > ϕ crit it stabilises H at = 0)

19. Stefan Antusch MPI für Physik (Munich) A new class of inflation models: Tribrid inflation ‣ Simple example (singlet fields, global SUSY to start with): 19 After inflation: Non-thermal leptogenesis after sneutrino inflation: very efficient way of generating the observed baryon asymmetry! Recent study within ‘hybrid-like’ models: ‘Sneutrino Hybrid Inflation and Leptogenesis’ S.A., Baumann, Domcke, Kostka (‘10)

20. Stefan Antusch MPI für Physik (Munich) Tribrid inflation in Supergravity ‣ Example model in SUGRA: → η-problem solved: Flat potential for ϕ at tree-level Slope from V 1-loop 20 K invariant under Heisenberg symmetry breaks the Heisenberg symmetry S.A., M. Bastero-Gil, K. Dutta, S. F. King, P. M. Kostka (‘08)

21. Stefan Antusch MPI für Physik (Munich) 21 spectral index n s r = A T /A S running of the spectral index (α S ) M: scale of the phase transition S.A., K. Dutta, P. M. Kostka ('09) very small (as typical for Hybrid- type models) Example: Predictions in a toy model...

22. Stefan Antusch MPI für Physik (Munich) Can the inflaton be a Gauge Non-Singlet? ‣ Example model of GNS inflation in SUGRA: Many additional challenges for GNS inflation... all resolved! 22 S.A., Bastero-Gil, Baumann, Dutta, King, Kostka (‘10) Example: SO(10) GUTs i = (1,...,4)

23. Stefan Antusch MPI für Physik (Munich) More in Posters... ‣ ‘Unified Matter Inflation in SUSY GUTs‘ Poster by Jochen Baumann ‣ ‘Matter Inflation and Heisenberg Symmetry in Heterotic String Theory‘ Poster by Sebastian Halter 23

24. Stefan Antusch MPI für Physik (Munich) Summary and Conclusions ‣ We discussed three recent developments... Heisenberg symmetry with stabilised modulus: Interesting solution to the η-problem in SUGRA inflation Tribrid Inflation: New class of models, very suitable for applying symmetry solutions to the η-problem Unified Matter Inflation in SUSY/SUGRA GUTs: Inflaton field can be in a GUT matter representation, e.g. in 16 of SO(10) 24