2. Strategies and Hints for a String Phenomenologist Yann Mambrini, DESY Hamburg, in collaboration with P. Binetruy, A. Birkedal, C. Muñoz, B. Nelson and E. Nezri EuroGDR SUSY, Frascatti, november 27 th 2004

3. PLAN II)Constructions of string effective models Perturbative and non-perturbative effect s: Gaugino condensation Lagrangian Construction Phenomenology III)Hints From accelerators to astrophysics Computing Tools I)Philosophy From String to Fields Horizontal versus Vertical sudies IV)Complementarities Experiments vs Theory Theory vs Experiments V)Conclusion and Outlooks

4. PHILOSOPHIES

5. PHILOSOPHIES

6. PHILOSOPHIES

7. PHILOSOPHIES

8. Lagrangian Construction K(S,T) = -Ln(S+S) – 3 Ln(T+T) + (T+T)ⁿC a C a  _ _ _ na na A string  1/a'  ds dt (  s x  x m ) -(y r s  y m ) m m s s Mplanck >> Mw A eff  1/a'  d x  g R / (a') + ¼ Tr F / (a') +... 3 4 2 10 (10) A eff   d x  g R [ ¼ (∂ m S ∂ S) / S + ¾ (∂ m T ∂ T) / T - ¼ S Tr F  m m 2 4 (4) 2 2 Compactification (N=1, dim=4). fa = S = 1/g2 ~ 2 T ~ R 2

9. Gaugino Condensation V 0 L Mplanck Mw. g = _______________ Re(S) + b8 ln(L / M string ) Re(S) + b8 ln(L / M string ) E8 2 8 p 2 L 8 = M string exp (-Re(S)/b 8 ) hidden ~ L 8 hidden ~ L 8_3 L ~ Fs (l l) hidden _ W np ~ M string exp (-3S/b 8 ) 3

10. Gaugino Condensation Wnp(S) = d1 exp(- S/b1) Wnp(S) = d1 exp(-S/b1) + d2 exp (-S/b2) V S W(S) = 0 0 1 2 3 4 I) Racetrack

11. Gaugino Condensation Wnp(S) = d+ exp(- S/b+) Knp(S) = K(S) + k(S) V S W(S) = 0 0 1 2 3 4 II) BGW

12. Gaugino Condensation Wfl(S) = a S + b V S W(S) = 0 0 1 2 3 4 III) Fluxes in Type IIB

13. Lagrangian Construction A string  1/a'  ds dt (  s x  x m ) -(y r s  y m ) m m s s Mplanck >> Mw A eff  1/a'  d x  g R / (a') + ¼ Tr F / (a') +... 3 4 2 10 (10) A eff   d x  g R [ ¼ (∂ m S ∂ S) / S + ¾ (∂ m T ∂ T) / T - ¼ S Tr F  m m 2 4 4 2 2 Compactification W ~ d1 exp(-3S/b1) + d2 exp(-3S/b2) np np W ~ d+ exp(-3S/b+) K = K (S) + K np np K(S,T) = -Ln(S+S) – 3 Ln(T+T) + (T+T)ⁿC a C a  _ _ _ na na

14. Effective Models Landscape SUGRA SUGRA M1 M2 M3 mH1 mH2 mQ mU mD mL mE Au Ad A  μ B Effective String String M3/2 tan b dGS cosq = 0MSUGRA M0 M1/2 A Tanb SignμHet.BGW Knp, 1con d M3/2 Tanb b+ dGS =0Racetrack(Wnp, 2 cond.) Fluxed MSSM (Brane)

15. TOOLS SUSPECT2 SDECAY Br Micromegas1. 3 W b -> sg b -> sg g-2 DarkSusy4 Directe Indirecte e+e- s Suspect2* (Strings, RGE, CCB) Low Energy Spectrum Couplings

16. Results I : Accelerators physics Linear Colider 800 GeV Mh < 113.5 GeV Mx+< 103.5 GeV b -> s g b -> s g 0.1 < W < 0.3 W MAP RACETRACK BGW

17. c c g g Astrophysical Sources

18. Results II : Fluxes

19. Results III : Exclusion? b+ b+ M3/2 M3/2 EWSB condition g-2 b -> s g b -> s g Mchar > 103.5 GeV Mhiggs > 113.5 GeV 0.1 < W < 0.3 0.1 < W < 0.3 Indirect from Sun Indirect from Sun Linear Collider 800 GeV Indirect detection from Galactic Center

20. OUTLOOKS Application to stabilized type IIB fluxes models on D7 branes Positron fluxes (PAMELA, AMS) Reconstruction of String Parameters from LHC/LC analysis Profiles in adiabatic compression models