inflation + cdm model = cosmology galaxies formation
DESCRIPTION
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: - PowerPoint PPT PresentationTRANSCRIPT
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:• Extreme fine tuning for • Coincidence
• Dark Matter: • Cuspy central density profiles• Too much substructure• Too late galaxy formation• Too early metalicity formation• Etc.
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.
The CosmologyT. Matos and L. Ureña, Class. Q. Grav. 17(2000)L75
• Dark Matter:• • V0[cosh() –1]• Dark Energy:•
• Baryons, • Neutrinos, etc.
0.25 0.7b 0.05
Scalar Field Fluctuations
T. Matos and L. Ureña, Phys. Rev. D63(2001)063506
Natural Cut-off
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 (310-27 Mpl )4 m 10-23 eV
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
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
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
Density Profiles
Density Profiles
Density Profiles
LSB Galaxies
Conclusion
• The scalar field is a good candidate to be the Dark Matter of the
Universe