String Phenomenology. Gary Shiu University of Wisconsin. Symposium
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1 String Phenomenology Gary Shiu University of Wisconsin Symposium
2 YITP s Theory Space QCD/Collider Physics Strings/SUGRA YITP Statistical Mechanics Neutrinos Standard Model & Beyond + a lot more... Cosmology
3 String Phenomenology
4 String Phenomenology
5 String Phenomenology
6 String Phenomenology How do we test these ideas?
7 Cosmic Microwave Background Almost scale invariant, Gaussian primordial spectrum predicted by inflation: good agreement with data. WMAP A tantalizing upper bound on the energy density during inflation: V M 4 GUT (10 16 GeV) 4 i.e., H GeV
8 WMAP & Beyond Can we learn from the CMB (or other cosmological measurements) details of string compactification?
9 LHC & Beyond Can we learn from the LHC (and beyond) details of string compactification?
10 Flux Compactification Σ j Various p!cycles of M n j = Σ j F Analogous to turning on a B-field: In Type IIB: W = Energy cost depends on detailed geometry: M G Ω Energy 1 8π (E 2 + B 2) Gukov, Vafa, Witten V n1,n 2,,n k (φ i ) moduli lifted [Dasgupta, Rajesh, Sethi]; [Greene, Schalm, GS]; [Giddings, Kachru, Polchinski]
11 Warped Throats Fluxes back-react on the metric: e.g., warped deformed conifold Klebanov, Strassler AdS5 IR UV leads to Randall-Sundrum hierarchy Giddings, Kachru, Polchinski
12 Warped Throats Fluxes back-react on the metric: e.g., warped deformed conifold Klebanov, Strassler AdS5 IR UV leads to Randall-Sundrum hierarchy Giddings, Kachru, Polchinski A variety of warped throats with different isometries and IR behavior.
13 Standard-like D-brane Models Marchesano, GS; Verlinde, Wijnholt; Cascales, Garcia del Moral, Quevedo, Uranga; Blumenhagen, Cvetic, GS, Marchesano;...
14 Brane Inflation Dvali and Tye... DD Inflation Reviews: [Quevedo, hep-th/ ];[burgess, hep-th/ ];[tye, hep-th/ ]; [Cline, hep-th/ ];[kallosh,hep-th/ ],...
15 Brane Inflation in Warped Throats D3 D3
16 Brane Inflation in Warped Throats Slow-roll D3 D3
17 Brane Inflation in Warped Throats DBI Silverstein, Tong D3 D3
18 Brane Inflation in Warped Throats DBI Silverstein, Tong D3 S = D3 d 4 x ) g (f(φ) 1 1 f(φ) φ 2 V (φ) f(φ) 1
19 Brane Inflation in Warped Throats DBI Silverstein, Tong D3 D3 S = d 4 x g (f(φ) 1 1 f(φ) φ 2 V (φ) f(φ) 1 ) Speed limit: φ 2 f(φ) 1
20 Brane Inflation in Warped Throats DBI Silverstein, Tong γ = 1 1 f(φ) φ 2 D3 S = D3 d 4 x g (f(φ) 1 1 f(φ) φ 2 V (φ) f(φ) 1 ) Speed limit: φ 2 f(φ) 1
21 Non-Gaussianities Large 3-point correlations that are potentially observable. Moreover, distinctive shape. [Figures from Chen, Huang, Kachru, Shiu] Slow-roll DBI (f NL ɛ) (f NL γ 2 )
22 Non-Gaussianities Large 3-point correlations that are potentially observable. Moreover, distinctive shape. [Figures from Chen, Huang, Kachru, Shiu] 54 < f NL < 114 (WMAP3) f NL 5 (PLANCK) Slow-roll DBI (f NL ɛ) (f NL γ 2 )
23 GS, B. Underwood, PRL Probing the Warped Geometry Spectral index depends on warp factor through: Exact KS AdS Mass Gap Exact KS Mass Gap AdS
24 Probing the Warped Geometry Running of spectral index: Exact KS AdS GS, B. Underwood, PRL
25 Warped throats at the LHC & Beyond
26 Search for Warped KK Gravitons GS, Underwood, Walker, Zurek (to appear) Couplings to KK gravitons only TeV suppressed Much work on LHC signatures of KK gravitons for RS: Davoudiasl, Hewett, Rizzo; Fitzpatrick, Kaplan, Randall, Wang; Agashe, Davoudiasl, Perez, Soni;...
27 Warped KK Spectrum and Couplings GS, Underwood, Walker, Zurek (to appear)
28 Warped KK Spectrum and Couplings GS, Underwood, Walker, Zurek (to appear) In comparison to RS, the KS geometry has:
29 Warped KK Spectrum and Couplings GS, Underwood, Walker, Zurek (to appear) In comparison to RS, the KS geometry has: Smaller KK spacing
30 Warped KK Spectrum and Couplings GS, Underwood, Walker, Zurek (to appear) In comparison to RS, the KS geometry has: Smaller KK spacing Stronger & mode-dependent couplings
31 Warped KK Spectrum and Couplings GS, Underwood, Walker, Zurek (to appear) In comparison to RS, the KS geometry has: Smaller KK spacing Stronger & mode-dependent couplings
32 KK Gravitons: Production and Decay Production: Decay: KK k 2, n k 1, m k2, n µ! (ij), " n k1, m q q µ! (ij), n " A b )(k 2 ) q, l + q, l KK KK A a ((k 1 ) W, Z, γ A b )(k2 ) µ! (ij), " n A a ((k1 ) p W, Z, γ g g KK µ! (ij), " n p µ! (ij), " n p KK g A a ((k1 ) g A b )(k2 )
33 KK Gravitons: Production and Decay Production: Decay: KK k 2, n k 1, m k2, n µ! (ij), " n k1, m q q µ! (ij), n " A b )(k 2 ) q, l + q, l KK KK A a ((k 1 ) W, Z, γ A b )(k2 ) µ! (ij), " n A a ((k1 ) p W, Z, γ g g KK µ! (ij), " n p µ! (ij), " n p KK g A a ((k1 ) g A b )(k2 )
34 KK Graviton Resonances Closer spacing between resonances Higher and broader peaks: σ Λ 4 Γ Λ 2 M KK Relative heights between different KK resonances
35 Happy Birthday, YITP!
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