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Problems with the  CDM Model PowerPoint PPT Presentation


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Galaxy formation from the IIB Superstring with Fluxes Tonatiuh Matos http:/www.fis.cinvestav.mx/~tmatos. Problems with the  CDM Model. Dark Energy: Extreme fine tuning for  Coincidence Dark Matter: Cuspy central density profiles Too much substructure Too late galaxy formation

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Problems with the  CDM Model

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Problems with the cdm model

Galaxy formation from the IIB Superstring with FluxesTonatiuh Matoshttp:/www.fis.cinvestav.mx/~tmatos


Problems with the cdm model

Problems with the CDM Model

  • Dark Energy:

  • Extreme fine tuning for 

  • Coincidence

  • Dark Matter:

  • Cuspy central density profiles

  • Too much substructure

  • Too late galaxy formation

  • Too early metalicity formation

  • Etc.


Some alternatives

Some Alternatives

  • Self-Interacting DM

  • Warm DM

  • Super Heavy DM

  • Self-Annihilating DM

  • Repulsive DM

  • Fuzzy DM

  • Decaying DM

  • Scalar Field Dark Matter

  • V = V0 (cosh()-1)


Cosmology from superstrings theory

Cosmology from Superstrings Theory

  • R. Kallosh

  • R. Brandenberger

  • D. Wands, etc.


Cosmology from superstrings theory1

Cosmology from Superstrings Theory

  • R. Kallosh

  • R. Brandenberger


Iib superstrings theory with fluxes phys rev d67 046006 2003

IIB Superstrings theory with FluxesPhys.Rev.D67:046006,2003

  • Type IIB Superstrings With Fluxes


Bose einstein condensate

Bose-Einstein Condensate

 + dV/d = 0

  • V = V0[cosh() – 1]


Bose einstein condensates

Bose-Einstein Condensates

  • Tc TeV

  • m < 10-17 eV

  • Mcrit 0.1 M2Planck /m


Problems with the cdm model

Scalar Field Fluctuation = HaloTonatiuh Matos and F. Siddhartha GuzmanClass. Q. Grav. 17(2000)L9; Tonatiuh Matos, F. Siddhartha Guzman and Dario Nuñez, Phys. Rev. D62(2000)061301(R);Tonatiuh Matos and F. Siddhartha Guzman,Class.Q. Grav. 18(2001)5055

  • M  0.1 M2Planck /m

  • If m  10-23 eV

  • M 1012 Mo


The model t matos r luevano h h garcia compean

The ModelT. Matos, R. Luevano, H. H. Garcia Compean.

  • Inflation

  • hin

  • V = V0[cosh() – 1] +Axion

  •  exp() F2


Problems with the cdm model


Problems with the cdm model

u


Omegas

Omegas


Omegas1

Omegas

exp()zoom


Direct proof of dm chandra

Direct Proof of DM (Chandra)


Density profiles

Density Profiles


Density profiles1

Density Profiles

LSB Galaxies


Density profiles2

Density Profiles

LSB Galaxies


Summarizing

Summarizing

  • The IIB Superstring model:

  • Behaves as CDM after recombination.

  • Reproduces all the successes CDM above galactic scales.

  • Predicts a sharp cut-off in the mass power spectrum

  • The favored values for the two free parameters

  •  20 V0 (310-27 Mpl )4  m 10-23 eV


Conclusions

Conclusions

  • The differences between IIB superstrings and CDM:

  • 1) Recombination

  • 2) Center of the Galaxies


Conclusion

Conclusion

  • The Dilaton could be a good candidate to be the Dark Matter of the Universe


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