Cosmology in LARGE volume string models

1. 01/29/2013@Osaka U. Cosmology in LARGE volume string models TetsutaroHigaki arXiv: 1208.3563published in JHEP 1211 (2012) 125 with Fuminobu Takahashi at Tohoku U. See also arXiv: 1208.3562 by Cicoli, Conlon and Quevedo

2. Production of a hot dark matter via LARGE extra dimensions.

3. 1. Motivation: Exploring the origin of the Universe. 1. Introduction

4. What is the Universe made of? The present universe consists of Dark matter and dark energy clearly require new physics beyond the Standard Model (SM).

9. Past and now of the Universe In the early Universe • Baryons • Dark matter (Cold DM) • Photons • Neutrinos dominated.

10. Past and now of the Universe In the early Universe • Baryons • Dark matter (Cold DM) • Photons • Neutrinos+ Dark radiation dominated. Sterile 4th neutrino-like (A part of hot dark matter)

11. My motivation Dark radiation Neff ～ 4 || A probe of high energy physics!?

12. Overview of string-theory-models Hidden sectors appear naturally through stringy compactifications! The Standard Model Moduli & Hidden sectors E.g. Gravity Anomaly cancellation condition

13. Supergravity models on a LARGE Swiss-cheese Calabi-Yau (CY) SM

14. Main characters in 4D SUGRA Size of CY32.Higgs 3. Axion (Ex-dim.)(DR) 4. Wino (CDM)

15. Contents • Introduction: Motivations and short summary • Observations and dark Radiation • LARGE volume scenario (LVS) • Dark radiation and dark matter from the modulus decay • Conclusion and open questions

16. 2. Observations of dark radiation (a hot DM)

17. Dark radiation (DR) • 4th neutrino-like component in cosmic νbackground Ultralight mass: MDR≦mν≦ 0.1 eV Almost no interaction: Gravity or… How can we detect the presence indirectly?

18. DR and expansion of the universe In radiation-dominated era with T ≦ 1MeV DR

19. DR and expansion of the universe The expansion rate getsincreasedby ΔNeff. The Friedman equation in rad. era H: Expansion rate (Hubble parameter)

20. Mild DR evidence 4He abundace is sensitive to the expansion rate H at BBN era ～ 1 sec. Cosmic Microwave Background (CMB) is sensitive to H at ～380,000 year.

22. Cyburt, Fields, Olive (2008)

23. HII region (H+, He*,O*,…) Cyburt, Fields, Olive (2008)

24. CMB WMAP 9-year ΔT/T0 map on the sky sphere, where T0 = 2.73K.

25. CMB WMAP 9-year, 1212.5226 Fourier form of ΔT/T0 map on the sky sphere, where T0 = 2.73K.

26. South Pole Telescope (SPT) Wilkinson Microwave Anisotropy Probe (WMAP) Atacama Cosmology Telescope (ACT) in Chili

28. Recent other CMB data • WMAP 9-year, 1212.5226: • Atacama Cosmology Telescope (ACT), 1301.0824:

29. Wrong!!; will be modified. Recent other CMB data • WMAP 9-year, 1212.5226: • Atacama Cosmology Telescope (ACT), 1301.0824: • Fewer # of data • Different frequency in CMB Note: Tension between BAO and H0.

30. Adoption of SPT result So, both 4He abundance and CMB mildly prefer the presence of extra radiation:

31. For confirmation of dark radiation in 4D N=1 supergravity (SUGRA) framework. Needs data from the Planck. WMAP 9-year, 1212.5226

32. 3. LARGE volume scenario (LVS):IIB orientifoldsupergravities in flux vacua

33. Closed string = Gravity Motivation for string theory Unified theory including quantum gravity! Open string between branes = Matter Openstring = Gauge nucleons D-brane

34. Extra dimensions and SUSY • The quantum gravity theory requires extra 6 dimensions and supersymmetry (SUSY). 4 + 6 = 10 M4 ×

35. Phenomenological motivation Hidden sectors appear naturally through stringy compactifications! The Standard Model Moduli & Hidden sectors E.g. Gravity Anomaly cancellation condition

36. Moduliin a Calabi-Yau space SUSY-preserved compactification

37. Moduliin a Calabi-Yau space SUSY-preserved compactification 4-cycle size: T (Kählermoduli) 3-cycle size: U (Complex structure moduli) + String Dilaton: S

38. Why moduli and axions? • Ubiquitous in string vacua. • VEVs = physical constants: • Size of extra dimension; • Gauge/Yukawacouplings, • SUSY-breaking parameters.

39. Moduli ～ gauge couplings (Ex) (4+n) dim. gauge theory on a brane (M4×Σn):

40. Moduli ～ gauge couplings (Ex) (4+n) dim. gauge theory on a brane (M4×Σn): Modulifieldφ : Volume of a cycle

41. Moduli ～ gauge couplings (Ex) (4+n) dim. gauge theory on a brane (M4×Σn): Modulifieldφ : Volume of a cycle An extra 6 dimension space can have many Σn. ↓ Many moduli

42. Axions～ θ-term (Ex) (4+n) dim. gauge theory on a brane (M4×Σn):

43. Axions～ θ-term (Ex) (4+n) dim. gauge theory on a brane (M4×Σn): Axion field a: Integrand of tensor field Cn (NSNS, RR)

44. Axions～ θ-term (Ex) (4+n) dim. gauge theory on a brane (M4×Σn): Axion field a: Integrand of tensor field Cn (NSNS, RR) An extra 6 dimension space can have many Σn. ↓ Many axions

45. What are their masses?What are their VEVs?(= couplings etc.) Moduli/axion stabilization

46. Flux compactificationswith O-planes and D-branes

47. Moduli/axion stabilization • Findinga vacuum of moduliin a string model

48. Example of potential for moduli

49. Ultralightaxion(s) • In a LARGE volume limitof compact space, axion will get ultralightthanks to a residual gauge symmetries onCn in 10D: • The axions originate from gravityCn (NSNS or RR-field).

50. Model:LARGE volume scenario(LVS) V. Balasubramanian, P. Berglund, J. P. Conlon and F. Quevedo.(2005); R. Blumenhagen , J. P. Conlon , S. Krippendorf, S. Moster and F. Quevedo.(2009)