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אוניברסיטת בן-גוריון

Ram Brustein. אוניברסיטת בן-גוריון. Inflationary cosmology in the central region of string/M-theory moduli Space. hep-th/0205042 hep-th/02xxxx with S. de Alwis and E. Novak PRL 87 (2001), hep-th/0106174 PRD 64 (2001), hep-th/0002087 with S. de Alwis.

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אוניברסיטת בן-גוריון

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  1. Ram Brustein אוניברסיטת בן-גוריון Inflationary cosmology in the central region of string/M-theory moduli Space hep-th/0205042 hep-th/02xxxx with S. de Alwis and E. Novak PRL 87 (2001), hep-th/0106174 PRD 64 (2001), hep-th/0002087 with S. de Alwis • Outer region of moduli space: problems! • Central region: parametrization with N=1 SUGRA • Scales & shape of central region potential • Inflation: constraints & predictions

  2. String Moduli Space Central region “minimal computability” IIB I IIA HO Outer region perturbative HW MS1 HE • Perturbative theories = cosmological disaster • massless moduli • Gravity = Einstein’s • Inflation blocked • Requirements • D=4 • N=1 SUSY  N=0 • CC<(m 3/2)4 • SM (will not discuss) • Volume/Coupling moduli • T S

  3. Central Region Our proposal: • Parametrization with D=4, N=1 SUGRA • Stabilization by SNP effects @ string scale • Continuously adjustable parameter • SUSY breaking @ lower scale by FT effects • PCCP o.k after SUSY breaking

  4. Scales & Shape of Moduli Potential • The width of the central region In effective 4D theory: moduli kinetic terms multiplied by MS8 V6 (M119 V7 in M-theory). Curvature term multiplied by same factors “Calibrate” using 4D Newton’s constant 8pGN=mp-2 • Typical distances are order one in units of mp

  5. The scale of the potential NO VOLUME FACTORS!!! Banks Numerical examples:

  6. V(f)/MS6mp-2 outer region outer region 2 -1 central region f/mp -4 -2 0 2 4 The shape of the potential zero CC min. & potential vanishes @ infinity  intermediate max.

  7. V(f)/MS6mp-2 outer region outer region 2 -1 central region f/mp -4 -2 0 2 4 Inflation: constraints & predictions • Topological inflation D • – wall thickness in space D/d ~ L4 Inflation dH > 1 D> mp H2~1/3L4/mp2

  8. Slow-roll parameters The “small” parameter Sufficient inflation Number of efolds Sufficient inflation Quantum fluct. not too large

  9. CMB anisotropies and the string scale For consistency need V’’~1/25

  10. For our model  1/3 < 25V’’ < 3  If consistent:

  11. Summary and prospects • Scenario: Stabilization in Central region • Consistent cosmology: • scaling arguments • Curvature of potential needs to be “smallish” • Predictions for CMB • Calculate ? possible to some extent

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