Post on 19-Jan-2016
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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• Too early metalicity formation• Etc.
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
• R. Brandenberger
• R. Kallosh
• D. Wands, etc.
Cosmology from Superstrings Theory
• R. Brandenberger
• R. Kallosh
IIB Superstrings theory with FluxesPhys.Rev.D67:046006,2003
• Type IIB Superstrings With Fluxes
Bose-Einstein Condensate
+ dV/d = 0
• V = V0[cosh() – 1]
Bose-Einstein Condensates
• Tc TeV
• m < 10-17 eV
• Mcrit 0.1 M2Planck /m
Scalar Field Fluctuation = HaloTonatiuh Matos and F. Siddhartha Guzman Class. 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 ModelT. Matos, R. Luevano, H. H. Garcia Compean.
• V = V0[cosh() – 1] +Axion
• exp() 2
• Inflation
• hin
u
Omegas
Omegas
exp() zoom
Direct Proof of DM (Chandra)
Density Profiles
Density Profiles
LSB Galaxies
Density Profiles
LSB Galaxies
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 (310-27 Mpl )4 m 10-23 eV
Conclusions
• The differences between IIB superstrings and CDM:
• 1) Recombination
• 2) Center of the Galaxies
Conclusion
• The Dilaton could be a good candidate to be the Dark Matter of
the Universe