Theory III: String Theory. presented by Dieter Lüst, MPI and LMU-München

Transcription

1 Theory III: String Theory presented by Dieter Lüst, MPI and LMU-München

2 The string theory group at MPI (started in 2004):

3 The string theory group at MPI (started in 2004): Permanent members: R. Blumenhagen, D. Lüst

4 The string theory group at MPI (started in 2004): Permanent members: R. Blumenhagen, D. Lüst Long term members: J. Erdmenger (MPG outstanding female programme), S. Stieberger, M. Zagermann (Emmy Noether Research Group)

5 The string theory group at MPI (started in 2004): Permanent members: R. Blumenhagen, D. Lüst Long term members: J. Erdmenger (MPG outstanding female programme), S. Stieberger, M. Zagermann (Emmy Noether Research Group) Research fellows: O. Andreev, P. Koerber, D. Tsimpis

6 The string theory group at MPI (started in 2004): Permanent members: R. Blumenhagen, D. Lüst Long term members: J. Erdmenger (MPG outstanding female programme), S. Stieberger, M. Zagermann (Emmy Noether Research Group) Research fellows: O. Andreev, P. Koerber, D. Tsimpis PhD Students: N. Akerblom, C. Caviezel, V. Grass, S. Höhne, M. Kaminski, S. Körs, D. Krefl, R. Meyer, S. Moster, J. Perz E. Plauschinn, F. Rust, R. Schmidt, T. Schmidt, M. Schmidt-Sommerfeld, W. Schulgin

7 The string theory group at MPI (started in 2004): Permanent members: R. Blumenhagen, D. Lüst Long term members: J. Erdmenger (MPG outstanding female programme), S. Stieberger, M. Zagermann (Emmy Noether Research Group) Research fellows: O. Andreev, P. Koerber, D. Tsimpis PhD Students: N. Akerblom, C. Caviezel, V. Grass, S. Höhne, M. Kaminski, S. Körs, D. Krefl, R. Meyer, S. Moster, J. Perz E. Plauschinn, F. Rust, R. Schmidt, T. Schmidt, M. Schmidt-Sommerfeld, W. Schulgin Diploma Students: D. Härtl

8 The string theory group at MPI (started in 2004): Permanent members: R. Blumenhagen, D. Lüst Long term members: J. Erdmenger (MPG outstanding female programme), S. Stieberger, M. Zagermann (Emmy Noether Research Group) Research fellows: O. Andreev, P. Koerber, D. Tsimpis PhD Students: N. Akerblom, C. Caviezel,V. Grass, S. Höhne, M. Kaminski, S. Körs, D. Krefl, R. Meyer, S. Moster, J. Perz E. Plauschinn, F. Rust, R. Schmidt, T. Schmidt, M. Schmidt-Sommerfeld, W. Schulgin Diploma Students: D. Härtl Plus the string theory group at the LMU.

9 Outline:

10 Outline: This talk

11 Outline: String Theory

12 Outline: String Theory Mathematics & Geometry: Calabi-Yau spaces, mirror symmetry, generalized spaces, K-theory,...

13 Outline: String Theory?????? (observable) Mathematics & Geometry: Calabi-Yau spaces, mirror symmetry, generalized spaces, K-theory,... Physics

14 Outline: String Theory?????? (observable) Mathematics & Geometry: Calabi-Yau spaces, mirror symmetry, generalized spaces, K-theory,... Physics A) String Model Building: Getting the Standard Model B) QCD and Strings C) Other activities

15 Physics goals of string theory:

16 Physics goals of string theory: Particle Physics

17 Physics goals of string theory: Particle Physics Unification of all forces, derivation of MSSM: In principle: ; Compute more details, predictions:??

18 Physics goals of string theory: Particle Physics Unification of all forces, derivation of MSSM: In principle: ; Compute more details, predictions:?? (Non-perturbative) informations about QCD: In principle: ; get real, non-supersymmetric QCD:??

19 Physics goals of string theory: Particle Physics Unification of all forces, derivation of MSSM: In principle: ; Compute more details, predictions:?? (Non-perturbative) informations about QCD: In principle: ; get real, non-supersymmetric QCD:?? Quantum gravity and cosmology: Black holes, quantum cosmology: Black hole entropies: ; Non-supersymmetric b.h.:?? Brane inflation: ; Emergence of space-time:??

20 Physics goals of string theory: Particle Physics Unification of all forces, derivation of MSSM: In principle: ; Compute more MPI: details, see predictions: next section?? (Non-perturbative) informations about QCD: In principle: ; get real, non-supersymmetric QCD:?? Quantum gravity and cosmology: Black holes, quantum cosmology: Black hole entropies: ; Non-supersymmetric b.h.:?? Brane inflation: ; Emergence of space-time:??

21 Physics goals of string theory: Particle Physics Unification of all forces, derivation of MSSM: In principle: ; Compute more MPI: details, see predictions: next section?? (Non-perturbative) informations about QCD: In principle: ; get real, non-supersymmetric QCD:?? MPI: see next section Quantum gravity and cosmology: Black holes, quantum cosmology: Black hole entropies: ; Non-supersymmetric b.h.:?? Brane inflation: ; Emergence of space-time:??

22 Physics goals of string theory: Particle Physics Unification of all forces, derivation of MSSM: In principle: ; Compute more MPI: details, see predictions: next section?? (Non-perturbative) informations about QCD: In principle: ; get real, non-supersymmetric QCD:?? MPI: see next section Quantum gravity and cosmology: Black holes, quantum cosmology: Black hole entropies: ; Non-supersymmetric b.h.:?? Black holes:lmu (Cardoso, Perz,...) Brane inflation: ; Emergence of space-time:??

23 A) String Model Building: Intersecting D-branes (Blumenhagen, Gmeiner, Honecker, Krefl, Lüst, Plauschinn, Reffert, Schulgin, Stein, Stieberger, Weigand, Zagermann)

24 ENS- Paris A) String Model Building: Intersecting D-branes CERN (Blumenhagen, Gmeiner, Honecker, Krefl, Lüst, Plauschinn, Reffert, Schulgin, Stein, Stieberger, Weigand, Zagermann) Amsterdam Amsterdam Philadelphia

25 A) String Model Building: Intersecting D-branes (Blumenhagen, Gmeiner, Honecker, Krefl, Lüst, Plauschinn, Reffert, Schulgin, Stein, Stieberger, Weigand, Zagermann) Local D-brane module of the Standard Model by stacks of intersecting D-branes:

26 A) String Model Building: Intersecting D-branes (Blumenhagen, Gmeiner, Honecker, Krefl, Lüst, Plauschinn, Reffert, Schulgin, Stein, Stieberger, Weigand, Zagermann) Local D-brane module of the Standard Model by stacks of intersecting D-branes: D-brane compactifications: Wrapping the D-brane modules around cycles of the compact background space: SM HS

27 A) String Model Building: Intersecting D-branes D-brane compactifications: Wrapping the D-brane modules around cycles of the compact background space: Standard Model module (Blumenhagen, Gmeiner, Honecker, Krefl, Lüst, Plauschinn, Reffert, Schulgin, Stein, Stieberger, Weigand, Zagermann) Local D-brane module of the Standard Model by stacks of intersecting D-branes: G=SU(3)xSU(2) xu(1) SM HS

28 A) String Model Building: Intersecting D-branes (Blumenhagen, Gmeiner, Honecker, Krefl, Lüst, Plauschinn, Reffert, Schulgin, Stein, Stieberger, Weigand, Zagermann) Local D-brane module of the Standard Model by stacks of intersecting D-branes: D-brane compactifications: Wrapping the D-brane modules around cycles of the compact background space: Standard Model module G=SU(3)xSU(2) xu(1) SM HS Hidden sector module Moduli stabilization

29 A) String Model Building: Intersecting D-branes (Blumenhagen, Gmeiner, Honecker, Krefl, Lüst, Plauschinn, Reffert, Schulgin, Stein, Stieberger, Weigand, Zagermann) Local D-brane module of the Standard Model by stacks of intersecting D-branes: D-brane compactifications: Wrapping the D-brane modules around cycles of the compact background space: Standard Model module G=SU(3)xSU(2) xu(1) Soft SUSY breaking (LHC) SM HS Hidden sector module Moduli stabilization (Lüst, Reffert, Stieberger,)

30 IIA Intersecting D-brane landscape: How many D-brane models exist which come close to the (spectrum of the) MSSM? (Blumenhagen, Gmeiner, Honecker, Lüst, Stein, Weigand,)

31 IIA Intersecting D-brane landscape: How many D-brane models exist which come close to the (spectrum of the) MSSM? (Blumenhagen, Gmeiner, Honecker, Lüst, Stein, Weigand,) The number of solutions is finite.

32 IIA Intersecting D-brane landscape: How many D-brane models exist which come close to the (spectrum of the) MSSM? (Blumenhagen, Gmeiner, Honecker, Lüst, Stein, Weigand,) The number of solutions is finite. Example: M 6 = T 6 /(Z 2 Z 2 ) Systematic (complete) computer search: orbifold:

33 IIA Intersecting D-brane landscape: How many D-brane models exist which come close to the (spectrum of the) MSSM? (Blumenhagen, Gmeiner, Honecker, Lüst, Stein, Weigand,) The number of solutions is finite. Example: M 6 = T 6 /(Z 2 Z 2 ) Systematic (complete) computer search: orbifold: There exist about susy D-brane models!

34 IIA Intersecting D-brane landscape: How many D-brane models exist which come close to the (spectrum of the) MSSM? (Blumenhagen, Gmeiner, Honecker, Lüst, Stein, Weigand,) The number of solutions is finite. Example: M 6 = T 6 /(Z 2 Z 2 ) orbifold: Systematic (complete) computer search: There exist about susy D-brane models! Only one in a billion models gives rise to a MSSM like vacuum!

35 IIA Intersecting D-brane landscape: How many D-brane models exist which come close to the (spectrum of the) MSSM? (Blumenhagen, Gmeiner, Honecker, Lüst, Stein, Weigand,) The number of solutions is finite. Example: M 6 = T 6 /(Z 2 Z 2 ) orbifold: Systematic (complete) computer search: There exist about susy D-brane models! Only one in a billion models gives rise to a MSSM like vacuum! Recent other example: M 6 = T 6 /Z susy D-brane models, MSSM like vacua. orbifold:

36 Example: IIA Intersecting D-brane landscape: How many D-brane models exist which come close to the (spectrum of the) MSSM? (Blumenhagen, Gmeiner, Honecker, Lüst, Stein, Weigand,) The number of solutions is finite. M 6 = T 6 /(Z 2 Z 2 ) - Statistics of D- brane models with GUT gauge groups (Gmeiner, Stein) Systematic (complete) computer search: orbifold: There exist about susy D-brane models! Only one in a billion models gives rise to a MSSM like vacuum! Recent other example: M 6 = T 6 /Z susy D-brane models, MSSM like vacua. orbifold:

37 Moduli stabilization problem (flux landscape): Dark energy, string inflation, predictions for SM couplings,.

38 Moduli stabilization problem (flux landscape): Dark energy, string inflation, predictions for SM couplings,. String compactifications contain many massless moduli fields with flat potential.

39 Moduli stabilization problem (flux landscape): Dark energy, string inflation, predictions for SM couplings,. String compactifications contain many massless moduli fields with flat potential. They can be fixed by background fluxes + string instantons! Number of flux vacua: N flux

40 Moduli stabilization problem (flux landscape): Dark energy, string inflation, predictions for SM couplings,. String compactifications contain many massless moduli fields with flat potential. They can be fixed by background fluxes + string instantons! Number of flux vacua: N flux However not for every Calabi-Yau space all moduli can be fixed! We considered IIB orientifolds with D3/D7-branes, compactified on orbifolds or their blown-up versions (smooth Calabi-Yau!) (Lüst, Reffert, Schulgin, Stieberger)

41 Moduli stabilization problem (flux landscape): Dark energy, string inflation, predictions for SM couplings,. String compactifications contain many massless moduli fields with flat potential. They can be fixed by background fluxes + string instantons! Number of flux vacua: N flux However not for every Calabi-Yau space all moduli can be fixed! We considered IIB orientifolds with D3/D7-branes, compactified on orbifolds or their blown-up versions (smooth Calabi-Yau!) (Lüst, Reffert, Schulgin, Stieberger) Conclusion: Moduli stabilization is model dependent!

42 Moduli stabilization problem (flux landscape): Dark energy, string inflation, predictions for SM couplings,. String compactifications contain many massless moduli fields with flat potential. They can be fixed by background fluxes + string instantons! Number of flux vacua: N flux However not for every Calabi-Yau space all moduli can be fixed! We considered IIB orientifolds with D3/D7-branes, compactified on orbifolds or their blown-up versions (smooth Calabi-Yau!) (Lüst, Reffert, Schulgin, Stieberger) Conclusion: Moduli stabilization is model dependent! Incorporate uplift to de Sitter vacuum by D-terms via D7-branes with F-flux. (Haack, Krefl, Lüst, Zagermann)

43 Moduli stabilization problem (flux landscape): Dark energy, string inflation, predictions for SM couplings,. String compactifications contain many massless moduli fields with flat potential. They can be fixed by background fluxes + string instantons! Number of flux vacua: N flux Discussion of flux However compactifications not for every and group Calabi-Yau space all moduli can be fixed! structures (Lüst, Tsimpis) We - Discussion considered of fluxes IIB and orientifolds calibrated D- with D3/D7-branes, compactified branes on (Koerber) orbifolds or their blown-up versions (smooth - Discussion Calabi-Yau!) of Chern-Simons (Lüst, Reffert, Schulgin, Stieberger) couplings in massive supergravity (Zagermann) Conclusion: Moduli stabilization is model dependent! Incorporate uplift to de Sitter vacuum by D-terms via D7-branes with F-flux. (Haack, Krefl, Lüst, Zagermann)

44 Moduli stabilization problem (flux landscape): Dark energy, string inflation, predictions for SM couplings,. String compactifications contain many massless moduli fields with flat potential. They can be fixed by background fluxes + string instantons! Number of flux vacua: N flux Space time instanton effects are However not for every relevant Calabi-Yau for Neutrino space masses all moduli can be fixed! (Blumenhagen, Weigand) We considered - Explicit IIB orientifolds calculation of non-perturbative with D3/D7-branes, ADS compactified superpotential on orbifolds (Akerblom, or their Blumenhagen, blown-up versions Lüst, Plauschinn, Schmidt-Sommerfeld) (smooth Calabi-Yau!) (Lüst, Reffert, Schulgin, Stieberger) Conclusion: Moduli stabilization is model dependent! Incorporate uplift to de Sitter vacuum by D-terms via D7-branes with F-flux. (Haack, Krefl, Lüst, Zagermann)

45 Heterotic string compactifications: (Blumenhagen, Honecker, Moster, Weigand,)

46 Heterotic string compactifications: (Blumenhagen, Honecker, Moster, Weigand,) Alternatively to D-brane models, heterotic string compactications offer good and viable possibilities for obtaining realistic particle physics models.

47 Heterotic string compactifications: (Blumenhagen, Honecker, Moster, Weigand,) Alternatively to D-brane models, heterotic string compactications offer good and viable possibilities for obtaining realistic particle physics models. Problem: in order to obtain models which (directly) lead to the S.M. gauge group (or to other gauge groups with U(1) factor), one needs Abelian gauge bundles over Calabi-Yau spaces.

48 Heterotic string compactifications: (Blumenhagen, Honecker, Moster, Weigand,) Alternatively to D-brane models, heterotic string compactications offer good and viable possibilities for obtaining realistic particle physics models. Problem: in order to obtain models which (directly) lead to the S.M. gauge group (or to other gauge groups with U(1) factor), one needs Abelian gauge bundles over Calabi-Yau spaces. These were first constructed by the MPI string group.

49 Heterotic string compactifications: (Blumenhagen, Honecker, Moster, Weigand,) Alternatively to D-brane models, heterotic string compactications offer good and viable possibilities for obtaining realistic particle physics models. Problem: in order to obtain models which (directly) lead to the S.M. gauge group (or to other gauge groups with U(1) factor), one needs Abelian gauge bundles over Calabi-Yau spaces. These were first constructed by the MPI string group. Interesting by-product: These heterotic models typically contain several massive U(1) gauge symmetries with massive axion fields.

50 B) QCD and Strings (Adding flavor to AdS/CFT): (Apreda, Erdmenger, Grosse, Höhne, Schmidt, Sieg,...)

51 B) QCD and Strings Krakow (Adding flavor to AdS/CFT): (Apreda, Erdmenger, Grosse, Höhne, Schmidt, Sieg,...) Pisa Milano

52 B) QCD and Strings (Adding flavor to AdS/CFT): (Apreda, Erdmenger, Grosse, Höhne, Schmidt, Sieg,...) Features of original AdS/CFT gauge-gravity correspondence: SU(N) gauge theory with N=4 supersymmetry Conformal invariance, no dynamical mass generation Only adjoint fields (gluons), no quarks

53 B) QCD and Strings (Adding flavor to AdS/CFT): (Apreda, Erdmenger, Grosse, Höhne, Schmidt, Sieg,...) Features of original AdS/CFT gauge-gravity correspondence: SU(N) gauge theory with N=4 supersymmetry Conformal invariance, no dynamical mass generation Only adjoint fields (gluons), no quarks How to come more close to real QCD?

54 B) QCD and Strings (Adding flavor to AdS/CFT): (Apreda, Erdmenger, Grosse, Höhne, Schmidt, Sieg,...) Features of original AdS/CFT gauge-gravity correspondence: SU(N) gauge theory with N=4 supersymmetry Conformal invariance, no dynamical mass generation Only adjoint fields (gluons), no quarks How to come more close to real QCD? Break SUSY and conformal invariance by deformed backgrounds (Constable/Myers, AdS-Schwarzschild) Quarks fields as open strings: add D7-branes

55 B) QCD and Strings (Adding flavor to AdS/CFT): (Apreda, Erdmenger, Grosse, Höhne, Schmidt, Sieg,...) Features of original AdS/CFT gauge-gravity correspondence: SU(N) gauge theory with N=4 supersymmetry Conformal invariance, no dynamical mass generation Only adjoint fields (gluons), no quarks How to come more close to real QCD? Break SUSY and conformal invariance by deformed backgrounds (Constable/Myers, AdS-Schwarzschild) Quarks fields as open strings: add D7-branes N D SYM 3!3 conventional open/closed string duality AdS 5 N probe D7 f quarks 3!7 flavour open/open string duality R 4 7!7 AdS 5 Meeting of the Advisory Board, brane March 29th, 2007

56 B) QCD and Strings (Adding flavor to AdS/CFT): (Apreda, Erdmenger, Grosse, Höhne, Schmidt, Sieg,...) Features of original AdS/CFT gauge-gravity correspondence: SU(N) gauge theory with N=4 supersymmetry Conformal invariance, no dynamical mass generation Only adjoint fields (gluons), no quarks How to come more close to real QCD? Break SUSY and conformal invariance by deformed backgrounds (Constable/Myers, AdS-Schwarzschild) Quarks fields as open strings: add D7-branes Result: Obtain gravity dual description of chiral symmetry breaking, Goldstone bosons and meson spectrum.

57 B) QCD and Strings (Adding flavor to AdS/CFT): (Apreda, Erdmenger, Grosse, Höhne, Schmidt, Sieg,...) Features of original AdS/CFT gauge-gravity correspondence: SU(N) gauge theory with N=4 supersymmetry Conformal invariance, no dynamical mass generation Only adjoint fields (gluons), no quarks How to come more close to real QCD? Break SUSY and conformal invariance by deformed backgrounds (Constable/Myers, AdS-Schwarzschild) Quarks fields as open strings: add D7-branes meson mass quark mass

58 B) QCD and Strings (Adding flavor to AdS/CFT): (Apreda, Erdmenger, Grosse, Höhne, Schmidt, Sieg,...) Features of original AdS/CFT gauge-gravity correspondence: SU(N) gauge theory with N=4 supersymmetry Conformal invariance, no dynamical mass generation Only adjoint fields (gluons), no quarks How to come more close to real QCD? Break SUSY and conformal invariance by deformed backgrounds (Constable/Myers, AdS-Schwarzschild) Quarks fields as open strings: add D7-branes AdS/CFT with D7-branes in meson mass 6 5 Polchinski-Strassler background (Apreda, Erdmenger, Lüst, Sieg) quark mass

59 B) QCD and Strings (Adding flavor to AdS/CFT): (Apreda, Erdmenger, Grosse, Höhne, Schmidt, Sieg,...) Features of original AdS/CFT gauge-gravity correspondence: SU(N) gauge theory with N=4 supersymmetry Conformal invariance, no dynamical mass generation Only adjoint fields (gluons), no quarks How to come more close to real QCD? Break SUSY and conformal invariance by deformed backgrounds (Constable/Myers, AdS-Schwarzschild) Quarks fields as open strings: add D7-branes meson mass quark mass

60 B) QCD and Strings (Adding flavor to AdS/CFT): (Apreda, Erdmenger, Grosse, Höhne, Schmidt, Sieg,...) Features of original AdS/CFT gauge-gravity correspondence: SU(N) gauge theory with N=4 supersymmetry Conformal invariance, no dynamical mass generation Only adjoint fields (gluons), no quarks How to come more close to real QCD? Break SUSY and conformal invariance by deformed backgrounds - Discussion (Constable/Myers, of AdS/CFT AdS-Schwarzschild) Quarks fields as open strings: add D7-branes with other D-brane systems: D3- D3,D1-D5, defect CFT, AdS_2/ meson mass 6 CFT_1 (Erdmenger, Meyer, Park, 5 4 Schmidt, Sochichiu) quark mass

61 B) QCD and Strings (Adding flavor to AdS/CFT): (Apreda, Erdmenger, Grosse, Höhne, Schmidt, Sieg,...) Features of original AdS/CFT gauge-gravity correspondence: SU(N) gauge theory with N=4 supersymmetry Conformal invariance, no dynamical mass generation Only adjoint fields (gluons), no quarks How to come more close to real QCD? Break SUSY and conformal invariance by deformed backgrounds (Constable/Myers, AdS-Schwarzschild) Quarks fields as open strings: add D7-branes meson mass Thermal phase transitions, finite chemical potentials (Apreda, Erdmenger, Grosse, Rust, Kaminski) - Gluon condensates, Wilson loops (RHIC) (Andreev, Zakharov) quark mass

62 B) QCD and Strings (Adding flavor to AdS/CFT): (Apreda, Erdmenger, Grosse, Höhne, Schmidt, Sieg,...) Features of original AdS/CFT gauge-gravity correspondence: SU(N) gauge theory with N=4 supersymmetry Conformal invariance, no dynamical mass generation Only adjoint fields (gluons), no quarks How to come more close to real QCD? Break SUSY and conformal invariance by deformed backgrounds (Constable/Myers, AdS-Schwarzschild) Quarks fields as open strings: add D7-branes meson mass quark mass

63 B) QCD and Strings (Adding flavor to AdS/CFT): (Apreda, Erdmenger, Grosse, Höhne, Schmidt, Sieg,...) Features of original AdS/CFT gauge-gravity correspondence: SU(N) gauge theory with N=4 supersymmetry Conformal invariance, no dynamical mass generation Only adjoint fields (gluons), no quarks How to come more close to real QCD? Break SUSY and conformal invariance by deformed backgrounds (Constable/Myers, - Computation of AdS-Schwarzschild) higher Quarks fields as order open MHV strings: amplitudes add D7-branes in meson mass supersymmetric QCD (Oprisa, Stieberger) quark mass

64 C) Other activities:

65 C) Other activities: The MPI string group works closely together with the string group at the LMU!

66 C) Other activities: The MPI string group works closely together with the string group at the LMU! Common research projects,

67 C) Other activities: The MPI string group works closely together with the string group at the LMU! Common research projects, common seminars,...

68 In Jan. 2005, the Arnold-Sommerfeld-Center for theoretical physics was established:

69 In Jan. 2005, the Arnold-Sommerfeld-Center for theoretical physics was established: ASC lecture series (A. Linde, L. Susskind, A. Leggett...)

70 In Jan. 2005, the Arnold-Sommerfeld-Center for theoretical physics was established: ASC lecture series (A. Linde, L. Susskind, A. Leggett...) ASC workshops and conferences: - November 2004: The String Vacuum Workshop - June 2005: Conference String Phenomenology October 2005: Flavor Dynamics - October 2005: Dark Energy - March 2006: Black Holes, Black Rings and Topological Strings - April 2006: Non-commutativity and Physics - July 2006: QCD and Strings - July 2006: Physics and Geometry of String Theory - June 2007: Twistors, Perturbative Gauge Theories, Supergravity and Superstrings

71 Other recent activities (cont.):

72 Other recent activities (cont.): Coordinator of Research Area A in the new Excellence Cluster Origin and Structure of the Universe New W1/W2 position Extra dimensions...

73 Other recent activities (cont.): Coordinator of Research Area A in the new Excellence Cluster Origin and Structure of the Universe New W1/W2 position Extra dimensions... Coordinator of the new Elite Master Study Programme Theoretical and Mathematical Physics New W1/W2 positions

74 Other recent activities (cont.): Coordinator of Research Area A in the new Excellence Cluster Origin and Structure of the Universe New W1/W2 position Extra dimensions... Coordinator of the new Elite Master Study Programme Theoretical and Mathematical Physics New W1/W2 positions Coordinator of the EC network ForcesUniverse

75 Other recent activities (cont.): Coordinator of Research Area A in the new Excellence Cluster Origin and Structure of the Universe New W1/W2 position Extra dimensions... Coordinator of the new Elite Master Study Programme Theoretical and Mathematical Physics New W1/W2 positions Coordinator of the EC network ForcesUniverse Participation (project A3) in the new SFB transregio Dark Universe.

76 Summary:

77 Summary: The string landscape is vast and rich: Flux Vacua M!theory G2 Het: SO(32) CY with U(N) Type IIB! Type IIA! D9 on CY D6 on CY with U(N) Het: E 8x E8 CY with SU(N) HW CY x S 1 Orbifolds?

78 Summary: There are many green spots on this landscape (hopefully the LHC will give new informations also to string theory):

79 Summary: There are many green spots on this landscape (hopefully the LHC will give new informations also to string theory): The Munich string group tries its best to make the landscape flourish and connecting it to physics (LHC, cosmology, QCD,..) Thank you!