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Inflation + CDM Model = Cosmology Galaxies Formation

Bose-Einstein Condesates as Galactic Dark Matter Halos Tonatiuh Matos, F. Siddhartha Guzman, Luis Ureña, Dario Nuñez, Argelia Bernal. http:/www.fis.cinvestav.mx/~tmatos. Inflation + CDM Model = Cosmology Galaxies Formation. Problems with the CDM Model. Dark Energy:

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Inflation + CDM Model = Cosmology Galaxies Formation

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  1. Bose-Einstein Condesates as Galactic Dark Matter HalosTonatiuh Matos, F. Siddhartha Guzman, Luis Ureña, Dario Nuñez, Argelia Bernal.http:/www.fis.cinvestav.mx/~tmatos • Inflation • + • CDM Model • = • Cosmology • Galaxies Formation

  2. 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.

  3. The Model • Examples: • Braneword Scenario • Superstrings  • V  f1exp() + f2exp(-) + … • V = V0[cosh() – 1] • H2 = 8/(3Mpl2)  (1 + /b) •  Inflation  graceful exit •  BBN  Cosmology  • Fix the free constants.

  4. The CosmologyT. Matos and L. Ureña, Class. Q. Grav. 17(2000)L75 • Dark Matter: •  • V0[cosh() –1] • Dark Energy: •   • Baryons, • Neutrinos, etc. •    0.25 •    0.7 • b  0.05

  5. Scalar Field FluctuationsT. Matos and L. Ureña,Phys. Rev. D63(2001)063506

  6. Natural Cut-off

  7. Summarizing • SFDM model is insensitive to initial conditions • Behaves as CDM • 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

  8. 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

  9. 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

  10. 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

  11. Density Profiles

  12. Density Profiles

  13. Density Profiles LSB Galaxies

  14. Conclusion • The scalar field is a good candidate to be the Dark Matter of the Universe

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